FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Yoo, J AF Yoo, Jaiyul TI General relativistic description of the observed galaxy power spectrum: Do we understand what we measure? SO PHYSICAL REVIEW D LA English DT Article ID DIGITAL SKY SURVEY; PRIMORDIAL NON-GAUSSIANITY; HALO BIAS; PERTURBATIONS AB We extend the general relativistic description of galaxy clustering developed in Yoo, Fitzpatrick, and Zaldarriaga (2009). For the first time we provide a fully general relativistic description of the observed matter power spectrum and the observed galaxy power spectrum with the linear bias ansatz. It is significantly different from the standard Newtonian description on large scales and especially its measurements on large scales can be misinterpreted as the detection of the primordial non-Gaussianity even in the absence thereof. The key difference in the observed galaxy power spectrum arises from the real-space matter fluctuation defined as the matter fluctuation at the hypersurface of the observed redshift. As opposed to the standard description, the shape of the observed galaxy power spectrum evolves in redshift, providing additional cosmological information. While the systematic errors in the standard Newtonian description are negligible in the current galaxy surveys at low redshift, correct general relativistic description is essential for understanding the galaxy power spectrum measurements on large scales in future surveys with redshift depth z >= 3. We discuss ways to improve the detection significance in the current galaxy surveys and comment on applications of our general relativistic formalism in future surveys. C1 Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Yoo, J (reprint author), Harvard Univ, Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jyoo@cfa.harvard.edu FU Harvard College Observatory FX J. Y. acknowledges useful discussions with Daniel Eisenstein, Eiichiro Komatsu, Uros. Seljak, and Michael Turner. Especially, J. Y. thanks Matias Zaldarriaga for his encouragement and critical comments throughout the completion of this work. J. Y. is supported by the Harvard College Observatory under the Donald H. Menzel fund. NR 32 TC 88 Z9 88 U1 1 U2 1 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1550-7998 J9 PHYS REV D JI Phys. Rev. D PD OCT 7 PY 2010 VL 82 IS 8 AR 083508 DI 10.1103/PhysRevD.82.083508 PG 12 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 660KB UT WOS:000282639300004 ER PT J AU Huang, YM Mathis, WN Wilkerson, RC AF Huang, Yiau-Min Mathis, Wayne N. Wilkerson, Richard C. TI Coetzeemyia, a new subgenus of Aedes, and a redescription of the holotype female of Aedes (Coetzeemyia) fryeri (Theobald) (Diptera: Culicidae) SO ZOOTAXA LA English DT Article DE Coetzeemyia; new subgenus; Aedes fryeri; Ae. dufouri; Ochlerotatus; Levua; Ae. (Levua) geoskusea (=suvae); characteristics; systematics; Culicidae; Aldabra Island ID ALLIED TAXA DIPTERA; LIFE STAGES; MORPHOLOGICAL DATA; AEDINI DIPTERA; CLASSIFICATION; PHYLOGENY; OCHLEROTATUS AB Coetzeemyia, a new subgenus of Aedes Meigen (in the broad traditional sense, pre-Reinert 2000), is characterized and diagnosed. Aedes fryeri (Theobald) is removed from the subgenus Levua Stone and Bohart (genus Levua of Reinert et al. 2004) and placed in the new monotypic subgenus Coetzeemyia as its type species by present designation. Recognition of Coetzeemyia is based in part on a cladistic analysis of 16 species: seven outgroup species (four non-Aedini species and 3 aedine species) and nine within group species, including the three species that had been included in Levua and six other species belonging to three related subgenera in Aedes (Geoskusea Edwards, Rhinoskusea Edwards, and Ochlerotatus-Lynch Arribalzaga). The type female and the male genitalia of Ae. fryeri are redescribed and illustrated. Its affinity to other subgenera of the genus Aedes is discussed. Information on the type data, distribution, bionomics, medical importance, and taxonomy of this species are presented. Some morphological characteristics of adults of the subgenera Ochlerotatus and Levua of Aedes are tabulated. Based on this cladistic analysis, it is evident that Levua is a monotypic lineage represented by a single known species, Ae. geoskusea. Aedes dufouri is transferred back to the subgenus Ochlerotatus and is distinguished from other congeners of this subgenus. C1 [Huang, Yiau-Min; Mathis, Wayne N.] Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA. [Wilkerson, Richard C.] Smithsonian Inst, WRBU, Washington, DC 20013 USA. [Wilkerson, Richard C.] Walter Reed Army Inst Res, Div Entomol, Silver Spring, MD 20910 USA. RP Huang, YM (reprint author), Smithsonian Inst, Dept Entomol, POB 37012,MSC C1109,MRC 534, Washington, DC 20013 USA. EM huangy@si.edu; mathisw@si.edu; wilkersonr@si.edu FU Department of Entomology, Smithsonian Institution; Walter Reed Army Institute of Research and the Smithsonian Institution FX We express our sincere appreciation and gratitude to the Department of Entomology, Smithsonian Institution for providing funding for the publication; to Drs. Leopoldo M. Rueda and Desmond Foley, Walter Reed Biosystematics Unit (WRBU), for critically reviewing this manuscript, and for their valuable comments. We also thank Ms. Karolyn Darrow, Scientific Illustrator, Department of Entomology, Smithsonian Institution, who helped produce the cladogram (Fig. 4).; This research was performed under a Memorandum of Understanding between the Walter Reed Army Institute of Research and the Smithsonian Institution, with institutional support provided by both organizations. The material to be published reflects the views of the authors and should not be construed to represent those of the Department of the Army or the Department of Defense. NR 28 TC 4 Z9 4 U1 0 U2 0 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD OCT 6 PY 2010 IS 2638 BP 1 EP 24 PG 24 WC Zoology SC Zoology GA 660LV UT WOS:000282645300001 ER PT J AU Hohensee, MA Stanwix, PL Tobar, ME Parker, SR Phillips, DF Walsworth, RL AF Hohensee, Michael A. Stanwix, Paul L. Tobar, Michael E. Parker, Stephen R. Phillips, David F. Walsworth, Ronald L. TI Improved constraints on isotropic shift and anisotropies of the speed of light using rotating cryogenic sapphire oscillators SO PHYSICAL REVIEW D LA English DT Article ID ATOMIC CLOCK; TIME AB We demonstrate that Michelson-Morley tests, which detect direction-dependent anisotropies in the speed of light, can also be used to place limits upon isotropic deviations of the vacuum speed of light from c, as described by the photon-sector standard model extension parameter (kappa) over tilde (tr). A shift in the speed of light that is isotropic in one inertial frame implies anisotropic shifts in others. Using observer Lorentz covariance, we derive the time-dependent variations in the relative resonance frequencies of a pair of electromagnetic resonators that would be generated by such a shift in the rest frame of the Sun. A new analysis of a recent experimental test of relativity using this result constrains (kappa) over tilde (tr) with a precision of 7.4 x 10(-9). This represents the first constraint on (kappa) over tilde (tr) by a Michelson-Morley experiment and the first analysis of a single experiment to simultaneously set limits on all nine nonbirefringent terms in the photon sector of the minimal standard model extension. C1 [Hohensee, Michael A.; Walsworth, Ronald L.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Hohensee, Michael A.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Stanwix, Paul L.; Tobar, Michael E.; Parker, Stephen R.] Univ Western Australia, Sch Phys, Nedlands, WA 6009, Australia. [Stanwix, Paul L.; Phillips, David F.; Walsworth, Ronald L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. RP Hohensee, MA (reprint author), Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. EM hohensee@berkeley.edu RI Stanwix, Paul/A-5280-2009; Parker, Stephen/I-4231-2013; Tobar, Michael/C-9763-2009; OI Stanwix, Paul/0000-0002-7069-8569; Parker, Stephen/0000-0003-1914-8833; Tobar, Michael/0000-0002-3139-1994; Hohensee, Michael/0000-0002-8106-4502 FU National Science Foundation; Australian Research Council FX This work was supported by the National Science Foundation and the Australian Research Council. We thank Alan Kostelecky and Ralf Lehnert for encouragement and useful discussions. NR 29 TC 18 Z9 18 U1 0 U2 2 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1550-7998 J9 PHYS REV D JI Phys. Rev. D PD OCT 5 PY 2010 VL 82 IS 7 AR 076001 DI 10.1103/PhysRevD.82.076001 PG 9 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 658SG UT WOS:000282509100006 ER PT J AU Case, AW Spence, HE Golightly, MJ Kasper, JC Blake, JB Mazur, JE Townsend, LW Zeitlin, CJ AF Case, A. W. Spence, H. E. Golightly, M. J. Kasper, J. C. Blake, J. B. Mazur, J. E. Townsend, L. W. Zeitlin, C. J. TI GCR access to the Moon as measured by the CRaTER instrument on LRO SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID ADVANCED COMPOSITION EXPLORER; SOLAR-WIND; MAGNETOPAUSE; PARTICLES AB Recent modeling efforts have yielded varying and conflicting results regarding the possibility that Earth's magnetosphere is able to shield energetic particles of >10 MeV at lunar distances. This population of particles consists of galactic cosmic rays as well as energetic particles that are accelerated by solar flares and coronal mass ejections. The Cosmic Ray Telescope for the Effects of Radiation (CRaTER) onboard the Lunar Reconnaissance Orbiter is in orbit about the Moon and is thus able to directly test these modeling results. Over the course of a month, CRaTER samples the upstream solar wind as well as various regions of Earth's magnetotail. CRaTER data from multiple lunations demonstrate that Earth's magnetosphere at lunar distances produces no measurable influence on energetic particle flux, even at the lowest energies (>14 MeV protons) where any effect should be maximized. For particles with energies of 14-30 MeV, we calculate an upper limit (determined by counting statistics) on the amount of shielding caused by the magnetosphere of 1.7%. The high energy channel (>500 MeV) provides an upper limit of 3.2%. Citation: Case, A. W., H. E. Spence, M. J. Golightly, J. C. Kasper, J. B. Blake, J. E. Mazur, L. W. Townsend, and C. J. Zeitlin (2010), GCR access to the Moon as measured by the CRaTER instrument on LRO, Geophys. Res. Lett., 37, L19101, doi: 10.1029/2010GL045118. C1 [Case, A. W.] Boston Univ, Ctr Space Phys, Boston, MA 02215 USA. [Blake, J. B.] Aerosp Corp, El Segundo, CA 90245 USA. [Spence, H. E.; Golightly, M. J.] Univ New Hampshire, Dept Phys, Durham, NH 03824 USA. [Kasper, J. C.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Mazur, J. E.] Aerosp Corp, Conf Ctr, Chantilly, VA 20151 USA. [Townsend, L. W.] Univ Tennessee, Dept Nucl Engn, Knoxville, TN 37996 USA. [Zeitlin, C. J.] SW Res Inst, Boulder, CO 80302 USA. RP Case, AW (reprint author), Boston Univ, Ctr Space Phys, 725 Commonwealth Ave, Boston, MA 02215 USA. EM tonycase@bu.edu RI Kasper, Justin/D-1152-2010; Spence, Harlan/A-1942-2011 OI Spence, Harlan/0000-0002-2526-2205; Kasper, Justin/0000-0002-7077-930X; FU LRO/CRaTER [NASA NNG05EB92C] FX We would like to thank Chia-Lin Huang for helpful discussions, Dick Mewaldt and the SIS instrument team for providing GCR data from the ACE spacecraft, and the ACE SWEPAM team and the ACE Science Center for providing the ACE solar wind data. This work was supported by the LRO/CRaTER project under contract NASA NNG05EB92C. NR 14 TC 2 Z9 3 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD OCT 2 PY 2010 VL 37 AR L19101 DI 10.1029/2010GL045118 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 657SQ UT WOS:000282433000009 ER PT J AU Harbaugh, DT Oppenheimer, HL Wood, KR Wagner, WL AF Harbaugh, Danica T. Oppenheimer, Hank L. Wood, Kenneth R. Wagner, Warren L. TI Taxonomic Revision of the Endangered Hawaiian Red-flowered Sandalwoods (Santalum) and Discovery of an Ancient Hybrid Species SO SYSTEMATIC BOTANY LA English DT Article DE endangered species; Hawaiian Islands; microsatellites; molecular phylogeny; morphology; taxonomic revision ID SILVERSWORD ALLIANCE COMPOSITAE; SANTALACEAE; PACIFIC; KAUAI; INSULARE; CONSERVATION; ISLANDS; NUCLEAR; GENUS AB The Hawaiian Islands are home to a quarter of the named diversity of sandalwoods in the genus Santa him. There has been considerable confusion on how to best interpret the variation patterns of the red-flowered Hawaiian sandalwoods, S.freycinetianum and S. haleakalae, and particularly of the endangered S. freycinetianum var. lanaiense in an appropriate taxonomy. In this study, nrDNA (ITS, ETS) and cpDNA (3' trnK intron) sequence, microsatellite, and morphological data are integrated to appropriately revise the taxonomy of this group by better understanding the genetic and morphological diversity within and between populations. Results reveal that populations of S. freycinetianum from O'ahu are genetically distinct from populations on Moloka'i, Lana'i, and Maui. Santalum freycinatianum is now considered only to occur on O'ahu. The East Maui endemic S. haleakalae intergrades morphologically and is not genetically distinct from populations of S. freycinetianum var. lanaiense based on the sequence and microsatellite data gathered thus far. We combine them here into a single species, S. haleakalae, with two varieties (var. haleakalae and var. lanaiense, comb nov.). Lastly, examination of populations of S. freycinetianum var. pyrularium suggest it is best treated at specific rank as S. pyrularium. Some populations that are sympatric with S. pyrularium and S. ellipticum in the coastal cliffs and valleys of northern Kaua'i, are morphologically similar to S. pyrularium but are more closely related to the white-flowered S. ellipticum clade according to both nrDNA and cpDNA data. However, at least three synapomorphic sites in the nrDNA data indicate that its origin may have been the result of an ancient hybridization event with the red-flowered clade. The morphological characteristics of this inferred ancient hybrid lineage appear to correspond with the species S. involutum described by H. St. John. C1 [Harbaugh, Danica T.; Wagner, Warren L.] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. [Oppenheimer, Hank L.] Univ Hawaii, Plant Extinct Prevent Program, Pacific Cooperat Studies Unit, Lahaina, HI 96761 USA. [Wood, Kenneth R.] Natl Trop Bot Garden, Kauai, HI 96741 USA. RP Harbaugh, DT (reprint author), Univ Calif Berkeley, 1001 Valley Life Sci Bldg 2465, Berkeley, CA 94720 USA. EM danicah@berkeley.edu FU National Tropical Botanical Garden on Kauai; Department of Botany; National Museum of Natural History; Smithsonian Institution FX The authors thank the associate editor of Systematic Botany, M. Wojciechowski, B. Baldwin, an anonymous reviewer, and D. Lorence for their invaluable comments and suggestions for improvement of the manuscript, as well as the numerous organizations and people who made this research possible by providing herbarium material to examine, permission to collect material in the field, or assistance in collecting it, including: The Bishop Museum (A. Harbottle); The National Tropical Botanical Garden (T. Flynn, D. Lorence, and C. Wichman); The Nature Conservancy, Molokai field office (E. Misaki and K Tachibana); East Molokai Watershed Partnership; Castle & Cooke (B. Plunkett); Maui Land & Pineapple Co. Pu'u Kukui Watershed Preserve (R. Bartlett and M. Webster); West Maui Mountains Watershed Partnership; Makila Land Co.; Leeward Haleakala Watershed Restoration Partnership; Hawai'i Division of Forestry & Wildlife; Kauai State Parks; Haleakala Ranch (S. Meidell), Haleakala National Park (E. Gordon, P. Welton, S. Anderson); Army Natural Resources, O'ahu (S. Ching and K. Welch, N. Maileau, J. Rohrer, M. Keir); The Nature Conservancy, Honouliuli Preserve field office (S. Lu, D. Sailer, D. Forman, L. Williams, M. Walker and J. Chu); The Nature Conservancy Maui office (P. Bily); The Nature Conservancy, Kanepu'u Preserve (R. Hera, R. Sabin, M. Eskaren, A. Amoncio, Ike Aina); Ulupalakua Ranch Auwahi Preserve (A. Medeiros, K. Bustamente, and F. Juan), A. Smith and B. Baldwin (UC Berkeley); R. Hobdy (DOFAW, ret.); U. S. Fish and Wildlife Service; S. Perlman (National Tropical Botanical Garden); and D. Reynaud. The authors also thank B. Baldwin and B. Wessa for assistance with molecular phylogenetic work at the Molecular Phylogenetics Laboratory at the University of California, Berkeley, as well as R. Fleischer and N. Rotzel for their assistance with microsatellite genotyping at the Center for Conservation and Evolutionary Genetics at the Smithsonian National Zoological Park, Washington, DC. Lastly, they thank the National Tropical Botanical Garden on Kauai (McBryde Science Program) and the Department of Botany, National Museum of Natural History, Smithsonian Institution for funding to D. Harbaugh for field and laboratory expenses, while appointed as a McBryde Postdoctoral Research Fellow. NR 48 TC 4 Z9 5 U1 6 U2 15 PU AMER SOC PLANT TAXONOMISTS PI LARAMIE PA UNIV WYOMING, DEPT BOTANY 3165, 1000 E UNIVERSITY AVE, LARAMIE, WY 82071 USA SN 0363-6445 J9 SYST BOT JI Syst. Bot. PD OCT-DEC PY 2010 VL 35 IS 4 BP 827 EP 838 DI 10.1600/036364410X539899 PG 12 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA 693JV UT WOS:000285221300013 ER PT J AU Flacke, G Spiering, P Cooper, D Gunther, MS Robertson, I Palmer, C Warren, K AF Flacke, Gabriella Spiering, Penny Cooper, Dave Gunther, Micaela Szykman Robertson, Ian Palmer, Carlysle Warren, Kristin TI A survey of internal parasites in free-ranging African wild dogs (Lycaon pictus) from KwaZulu-Natal, South Africa SO SOUTH AFRICAN JOURNAL OF WILDLIFE RESEARCH LA English DT Article DE Ancylostoma; Babesia canis; Dipylidium caninum; Ehrlichia canis; internal parasites; Isospora; Sarcocystis; Toxocara canis ID CANIS-MESOMELAS SCHREBER; TRANSMISSION; TEMMINCK AB A study was undertaken between 1 January 2006 and 16 February 2007 to identify haemoparasites and gastrointestinal parasites infecting African wild dogs (Lycaon pictus) in KwaZulu-Natal (KZN) province, South Africa. Blood and faecal samples were opportunistically collected from wild dogs immobilized for collaring or translocation purposes (n = 24). Three common domestic canine gastrointestinal parasites, Toxocara canis, Dipylidium caninum and Ancylostoma spp., and two genera of canid protozoan GI parasites, Sarcocystis and Isospora, were identified in 12 fresh faecal samples. The seroprevalence of Ehrlichia canis from 24 individual serum samples analysed was 83%. However, only 21% of the 14 whole-blood smears evaluated for the presence of E. canis morulae within monocytes were positive. Twelve whole-blood smears were evaluated for the presence of Babesia canistrophozoites within erythrocytes and revealed 0% prevalence. Although there is currently no evidence of direct parasite-related mortality in the KZN population, the presence of internal parasites may be more detrimental to the overall health status of African wild dogs with immunosuppression as a result of other disease conditions, translocation stress, or inbreeding depression. C1 [Flacke, Gabriella; Palmer, Carlysle; Warren, Kristin] Murdoch Univ, Sch Vet & Biomed Sci, Conservat Med Programme, Perth, WA 6150, Australia. [Spiering, Penny; Gunther, Micaela Szykman] Natl Zool Pk, Smithsonian Conservat Biol Inst, Ctr Species Survival, Front Royal, VA 22630 USA. [Spiering, Penny] Univ Pretoria, Ctr Wildlife Management, ZA-0002 Pretoria, South Africa. [Cooper, Dave] Ezemvelo KZN Wildlife, ZA-3202 Pietermaritzburg, South Africa. [Gunther, Micaela Szykman] Humboldt State Univ, Dept Wildlife, Arcata, CA 95521 USA. [Robertson, Ian] Murdoch Univ, Sch Vet & Biomed Sci, Vet Epidemiol Programme, Perth, WA 6150, Australia. RP Flacke, G (reprint author), Murdoch Univ, Sch Vet & Biomed Sci, Conservat Med Programme, Perth, WA 6150, Australia. EM gflacke@hotmail.com FU National Geographic Society Conservation Trust [C91-06]; Murdoch University FX We thank the management of Hluhluwe-iMfolozi Park, the Isimangaliso (Greater St Lucia) Wetland Park Authority, Mkhuze Game Reserve and Thanda Private Game Reserve for permission to conduct this research and for logistical support. We also thank the Ezemvelo-KZN Wildlife Game Capture Unit for use of darting and laboratory equipment. Furthermore, we thank Moritz van Vuuren and the laboratory at the Department of Veterinary Tropical Diseases, Onderstepoort, for conducting the serology for this project, and Darryl Baxter, Heinz Kohrs and Trevor Viljoen, private practice veterinarians who contributed information on disease prevalence in domestic dogs in KZN. Finally, we wish to thank Sboniso Zwane and Thadaigh Baggallay for assistance with field monitoring. This project was supported by the National Geographic Society Conservation Trust (Grant Number C91-06) and the Conservation Medicine Small Research Grants Programme at Murdoch University. NR 19 TC 3 Z9 3 U1 1 U2 10 PU SOUTHERN AFRICAN WILDLIFE MANAGEMENT ASSOC PI BLOUBERGSTRAND PA P O BOX 217, BLOUBERGSTRAND 7437, SOUTH AFRICA SN 0379-4369 J9 S AFR J WILDL RES JI South Afr. J. Wildl. Res. PD OCT PY 2010 VL 40 IS 2 BP 176 EP 180 PG 5 WC Ecology; Zoology SC Environmental Sciences & Ecology; Zoology GA 769KO UT WOS:000291012100010 ER PT J AU D'Apolito, C Pessoa, SM Balestieri, FCDM Balestieri, JBP AF D'Apolito, Carlos Pessoa, Sheila Magalhaes de Lazari Manente Balestieri, Fatima Cristina Perrella Balestieri, Jose Benedito TI Pollen harvest by Apis mellifera L. (Hymenoptera: Apidae) in the Dourados region, Mato Grosso do Sul state (Brazil) SO ACTA BOTANICA BRASILICA LA English DT Article DE bee flora; Brazilian center west ID AFRICANIZED HONEY-BEE; ATLANTIC RAIN-FOREST; STINGLESS BEES; MELIPONA; APOIDEA AB (Pollen harvest by Apis mellifera L. (Hymenoptera: Apidae) in the Dourados region, Mato Grosso do Sul state (Brazil)). We present data on the pollen harvest by Apis mellifera L. at a central-western Brazil site not yet studied. Corbiculae pollen loads were collected during one year in front of the hive, acetolysed and slides mounted for optical microscopy. Identification followed comparisons with a local pollen collection. Forty-two pollen types were utilized by the bee; the most important families were Myrtaceae, Asteraceae, Euphorbiaceae, Brassicaceae and Poaceae. The genus/species level ranking of relative importance showed Eucalyptus (19%), Raphanus raphanistrum (13%), Poaceae type 2 (7.5%), Jatropha cf. gossypiifolia (7%) and Sapium glandulatum (6.5%). Overall, the majority of pollen types (80%) were not abundantly harvested, and a minority (4%) reached values of 10%. Given that the study area has cultivated plants and not natural vegetation, we indicate most of the identified species as manageable and point out that weedy vegetation can be an important food source for bees since it frequently occurred in the pollen spectra even within a totally cultivated area. C1 [D'Apolito, Carlos] Ancon, Smithsonian Trop Res Inst, Panama City, Panama. [Pessoa, Sheila Magalhaes] Fundacao Univ Fed Grande Dourados, Fac Ciencias Agr, Dourados, MS, Brazil. [de Lazari Manente Balestieri, Fatima Cristina; Perrella Balestieri, Jose Benedito] Fundacao Univ Fed Grande Dourados, Fac Ciencias Biol & Ambientais, Lab Abelhas Nativas, Dourados, MS, Brazil. RP D'Apolito, C (reprint author), Ancon, Smithsonian Trop Res Inst, Panama City, Panama. EM carlosdapolito@hotmail.com NR 37 TC 1 Z9 1 U1 1 U2 5 PU SOC BOTANICA BRASIL PI SAO PAULO SP PA CAIXA POSTAL 3005, SAO PAULO SP, 01061-970, BRAZIL SN 0102-3306 EI 1677-941X J9 ACTA BOT BRAS JI Acta Bot. Bras. PD OCT-DEC PY 2010 VL 24 IS 4 BP 898 EP 904 PG 7 WC Plant Sciences SC Plant Sciences GA 728RB UT WOS:000287891100003 ER PT J AU Lee, CF Staines, CL AF Lee, Chi-Feng Staines, Charles L. TI MONOLEPTA ONGI, A NEW SPECIES FROM LANYU ISLAND, WITH REDESCRIPTION OF ITS ALLIED SPECIES MONOLEPTA LONGITARSOIDES CHUJO, 1938 (COLEOPTERA: CHRYSOMELIDAE: GALERUCINAE) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE color variation; Taiwan; taxonomy ID REVISION AB Monolepta ongi, n. sp., is described from Lanyu Island, Taitung county, Taiwan. Its allied species, Monolepta longitarsoides Chujo, 1938, is redescribed for comparison. Their antennae, male aedeagus, female spermatheca and bursa-sclerites are illustrated. The lectotype and paralectotypes are designated for Monolepta longitarsoides from Chujo's type series. C1 [Lee, Chi-Feng] Agr Res Inst Taiwan, Appl Zool Div, Taichung 413, Wufeng, Taiwan. [Staines, Charles L.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, MRC 187, Washington, DC 20013 USA. RP Lee, CF (reprint author), Agr Res Inst Taiwan, Appl Zool Div, 189 Chung Cheng Rd, Taichung 413, Wufeng, Taiwan. EM chifeng@tari.gov.tw; stainesc@si.edu NR 20 TC 0 Z9 0 U1 1 U2 1 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD OCT PY 2010 VL 112 IS 4 BP 530 EP 540 DI 10.4289/0013-8797.112.4.530 PG 11 WC Entomology SC Entomology GA 708IN UT WOS:000286355600007 ER PT J AU Walters, JR Derrickson, SR Fry, DM Haig, SM Marzluff, JM Wunderle, JM AF Walters, Jeffrey R. Derrickson, Scott R. Fry, D. Michael Haig, Susan M. Marzluff, John M. Wunderle, Joseph M., Jr. TI STATUS OF THE CALIFORNIA CONDOR (GYMNOGYPS CALIFORNIANUS) AND EFFORTS TO ACHIEVE ITS RECOVERY SO AUK LA English DT Editorial Material ID ENDANGERED-SPECIES-ACT; ENVIRONMENTAL CONTAMINANTS; LEAD; CONSERVATION; POPULATION; MANAGEMENT; AMMUNITION; VULTURES; REINTRODUCTION; REPRODUCTION C1 [Walters, Jeffrey R.] Virginia Tech Univ, Dept Biol Sci, Blacksburg, VA 24061 USA. [Derrickson, Scott R.] Smithsonian Conservat Res Ctr, Front Royal, VA 22630 USA. [Fry, D. Michael] Amer Bird Conservancy, Washington, DC 20009 USA. [Haig, Susan M.] Oregon State Univ, US Geol Survey, Forest & Rangeland Ecosyst Sci Ctr, Corvallis, OR 97331 USA. [Marzluff, John M.] Univ Washington, Coll Environm, Seattle, WA 98195 USA. [Wunderle, Joseph M., Jr.] Int Inst Trop Forestry, USDA, Forest Serv, Sabana Field Res Stn, Luquillo, PR 00773 USA. RP Walters, JR (reprint author), Virginia Tech Univ, Dept Biol Sci, Blacksburg, VA 24061 USA. EM jrwalt@vt.edu NR 109 TC 41 Z9 43 U1 14 U2 117 PU AMER ORNITHOLOGISTS UNION PI LAWRENCE PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 USA SN 0004-8038 J9 AUK JI AUK PD OCT PY 2010 VL 127 IS 4 BP 969 EP 1001 DI 10.1525/auk.2010.127.4.969 PG 33 WC Ornithology SC Zoology GA 679XZ UT WOS:000284195400027 ER PT J AU da Silva-Caminha, SAF Jaramillo, CA Absy, ML AF da Silva-Caminha, Silane A. F. Jaramillo, Carlos A. Absy, Maria Lucia TI Neogene palynology of the Solimoes Basin, Brazilian Amazonia SO PALAEONTOGRAPHICA ABTEILUNG B-PALAEOPHYTOLOGIE PALAEOBOTANY-PALAEOPHYTOLOGY LA English DT Article DE Palynology; taxonomy; stratigraphy; Neogene; Amazonia ID LATE-MIOCENE; QUANTITATIVE BIOCHRONOLOGY; TERTIARY SEDIMENTS; RECONSTRUCTION; CONSERVATION; COLOMBIA; POLLEN; SPORES; AGE AB The tropics of South America hold the largest plant diversity in the world, yet the origins and processes leading to this high diversity still remain elusive. The Neogene sedimentary and fossil record of Amazonia could contain important clues to understanding the evolution of the Amazonian forest. Here, we study the pollen and spore record of two drill cores of the Neogene Solimoes Formation taken in northwestern Brazil, east of the Iquitos Arch. We studied 41 palynological samples and used several techniques to analyze the results, including Unitary Associations, a quantitative biostratigraphic technique, and Multidimensional Scaling Analysis. We describe 109 species, 51 of which are new, and seven new combinations. The biostratigraphic analysis indicates that the age of the Solimoes Formation in the study area is Late Miocene/Early Pliocene. This age is younger than that of nearby sections located west of the Iquitos arch, suggesting that the Iquitos Arch was active during the accumulation of the Solimoes Formation. The pollen/spore assemblages indicate that the Solimoes accumulated in fluvial deposits. We did not find evidence of either marine/tidal-flat deposits or extensive lakes. C1 [da Silva-Caminha, Silane A. F.; Absy, Maria Lucia] Lab Palinol CPBO INPA, Cordenacao Pos Grad Ecol PGEC, INPA, BR-69011970 Manaus, Amazonas, Brazil. [da Silva-Caminha, Silane A. F.; Jaramillo, Carlos A.] Smithsonian Trop Res Inst, Balboa 084303092, Ancon, Panama. RP da Silva-Caminha, SAF (reprint author), Lab Palinol CPBO INPA, Cordenacao Pos Grad Ecol PGEC, INPA, POB 478, BR-69011970 Manaus, Amazonas, Brazil. FU CAPES; CNPq FX We thank the Smithsonian Tropical Research Institute (STRI) and Instituto Nacional de Pesquisas da Amazonia (INPA) where this research was carried out. We also thank Departamento Nacional de Prospeccao Mineral (DNPM), especially Dr. Fernando Burgos and Gert Woeltje for the sampling permits of the Amazon cores. We thank Instituto Colombiano del Petroleo (ICP) for sample processing. Thanks to Dr. Jean Guex for the biostratigraphical comments; Dr. Jackson Paz, Dr. Fatima Leite, Dr. Edgardo Latrubesse for the geological discussions; Millerlandy Romero, Paula Sucerquia and Jean Caminha for help with the figures; Giovanni Bedoya for the corrections in the Latin names; and especially, Milton Rueda for the palynological morphology discussions. Thanks to Dr. Carmen Schloeder and Dr. Florian Wittmann for the translation of the abstract into German. Thanks to A. Traverse, D. Dilcher, T. Lott and D. Mai for their helpful comments on the manuscript. This study was supported by CAPES and CNPq Brazilian fellowships. NR 114 TC 3 Z9 3 U1 0 U2 5 PU E SCHWEIZERBARTSCHE VERLAGSBUCHHANDLUNG PI STUTTGART PA NAEGELE U OBERMILLER, SCIENCE PUBLISHERS, JOHANNESSTRASSE 3A, D 70176 STUTTGART, GERMANY SN 0375-0299 J9 PALAEONTOGR ABT B JI Palaeontogr. Abt. B-Palaophytol. PD OCT PY 2010 VL 284 IS 1-3 BP 13 EP 79 PG 67 WC Paleontology SC Paleontology GA 679XE UT WOS:000284193300002 ER PT J AU LaFollette, MC AF LaFollette, Marcel Chotkowski TI Keep Watching the Skies! The Story of Operation Moonwatch and the Dawn of the Space Age SO AMERICAN HISTORICAL REVIEW LA English DT Book Review C1 [LaFollette, Marcel Chotkowski] Smithsonian Inst, Washington, DC 20560 USA. RP LaFollette, MC (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0002-8762 J9 AM HIST REV JI Am. Hist. Rev. PD OCT PY 2010 VL 115 IS 4 BP 1177 EP 1177 PG 1 WC History SC History GA 669ZB UT WOS:000283387800089 ER PT J AU Turner, BL AF Turner, Benjamin L. TI Variation in pH Optima of Hydrolytic Enzyme Activities in Tropical Rain Forest Soils SO APPLIED AND ENVIRONMENTAL MICROBIOLOGY LA English DT Article ID MICROBIAL COMMUNITY COMPOSITION; PHOSPHATASE-ACTIVITY; CELLULASE-ACTIVITY; CHITINASE ACTIVITY; BETA-GLUCOSIDASE; ACID-PHOSPHATASE; WETLAND SOILS; PHOSPHODIESTERASE; LITTER; ASSAY AB Extracellular enzymes synthesized by soil microbes play a central role in the biogeochemical cycling of nutrients in the environment. The pH optima of eight hydrolytic enzymes involved in the cycles of carbon, nitrogen, phosphorus, and sulfur, were assessed in a series of tropical forest soils of contrasting pH values from the Republic of Panama. Assays were conducted using 4-methylumbelliferone-linked fluorogenic substrates in modified universal buffer. Optimum pH values differed markedly among enzymes and soils. Enzymes were grouped into three classes based on their pH optima: (i) enzymes with acidic pH optima that were consistent among soils (cellobiohydrolase, beta-xylanase, and arylsulfatase), (ii) enzymes with acidic pH optima that varied systematically with soil pH, with the most acidic pH optima in the most acidic soils (alpha-glucosidase, beta-glucosidase, and N-acetyl-beta-glucosaminidase), and (iii) enzymes with an optimum pH in either the acid range or the alkaline range depending on soil pH (phosphomonoesterase and phosphodiesterase). The optimum pH values of phosphomonoesterase were consistent among soils, being 4 to 5 for acid phosphomonoesterase and 10 to 11 for alkaline phosphomonoesterase. In contrast, the optimum pH for phosphodiesterase activity varied systematically with soil pH, with the most acidic pH optima (3.0) in the most acidic soils and the most alkaline pH optima (pH 10) in near-neutral soils. Arylsulfatase activity had a very acidic optimum pH in all soils (pH <= 3.0) irrespective of soil pH. The differences in pH optima may be linked to the origins of the enzymes and/or the degree of stabilization on solid surfaces. The results have important implications for the interpretation of hydrolytic enzyme assays using fluorogenic substrates. C1 Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Turner, BL (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama. EM TurnerBL@si.edu RI Turner, Benjamin/E-5940-2011 OI Turner, Benjamin/0000-0002-6585-0722 NR 63 TC 49 Z9 54 U1 3 U2 62 PU AMER SOC MICROBIOLOGY PI WASHINGTON PA 1752 N ST NW, WASHINGTON, DC 20036-2904 USA SN 0099-2240 J9 APPL ENVIRON MICROB JI Appl. Environ. Microbiol. PD OCT PY 2010 VL 76 IS 19 BP 6485 EP 6493 DI 10.1128/AEM.00560-10 PG 9 WC Biotechnology & Applied Microbiology; Microbiology SC Biotechnology & Applied Microbiology; Microbiology GA 653ZA UT WOS:000282136700019 PM 20709838 ER PT J AU Baldwin, AH Kettenring, KM Whigham, DF AF Baldwin, Andrew H. Kettenring, Karin M. Whigham, Dennis F. TI Seed banks of Phragmites australis-dominated brackish wetlands: Relationships to seed viability, inundation, and land cover SO AQUATIC BOTANY LA English DT Article DE Seed banks; Phragmites australis; Common reed; Non-native haplotype; Tidal wetlands; Chesapeake Bay; Wave disturbance; Seedling recruitment; Seed viability; Genetic diversity ID SALT-MARSH PLANTS; COMMON REED; CHESAPEAKE BAY; NEW-JERSEY; VEGETATION; EXPANSION; EMERGENCE; SALINITY; DRAWDOWN; FLUCTUATIONS AB In tidal wetlands of the eastern United States, buried seeds of the non-native haplotype of Phragmites australis may be a source of propagules for re-establishment after eradication efforts but factors controlling the development and expression of seed banks in non-native Phragmites stands have not been examined. We sampled surface soil at four Chesapeake Bay brackish tidal wetlands dominated by the non-native (European) haplotype M of Phragmites and used the seedling emergence method to quantity species of seedlings emerging under flooded and non-flooded soil conditions. Within each subestuary, one site was dominated by Phragmites that produced viable seeds (high viability) and the other by Phragmites that did not (low viability). We also described standing vegetation in plots, measured soil salinity, analyzed soil characteristics, and described surrounding land cover. Based on number of emerging seedlings, we found that 284 and 698 Phragmites seeds m(-2) occurred at the two high-viability sites, which was significantly higher than seed densities at the low-viability sites (10 seeds m-2), and greater than densities reported elsewhere. We also found that emergence of Phragmites seedlings from soil samples was prevented by continuous flooding of 3.5 cm of standing water, suggesting that colonization of deep water areas is clue to vegetative clonal expansion from Phragmites in adjacent higher elevations. The density of Phragmites seeds was not related to soil salinity or abundance of other species in the seed bank or vegetation, but instead was positively related to greater wave energy disturbance (much longer fetch and more open water) and lower area of wetlands nearby. The seed bank was more species-rich (15-22 species observed) than standing vegetation (3-15 species) at all sites, meaning that the dominance of Phragmites in vegetation does not prevent the development of a diverse seed bank and implying that a species-rich community may establish rapidly following control efforts. Based on these results and our findings in related studies, we postulate that wave energy disturbance generates repeated opportunities for seedling recruitment by Phragmites, which creates stands of Phragmites with higher genotypic diversity. In turn, genetically diverse stands favor greater cross-pollination and production of viable seed. These findings suggest that, in North America, targeting control efforts on non-native Phragmites patches in areas of higher exposure to wave energy may be more effective in reducing source populations than efforts in more protected locations. (C) 2010 Elsevier B.V. All rights reserved. C1 [Baldwin, Andrew H.] Univ Maryland, Dept Environm Sci & Technol, College Pk, MD 20742 USA. [Kettenring, Karin M.; Whigham, Dennis F.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Baldwin, AH (reprint author), Univ Maryland, Dept Environm Sci & Technol, 1423 Anim Sci Bldg, College Pk, MD 20742 USA. EM baldwin@umd.edu; karin.kettenring@usu.edu; whighamd@si.edu RI Baldwin, Andrew/C-8759-2014; OI Whigham, Dennis/0000-0003-1488-820X FU Smithsonian Institution FX We thank Pete Sharpe for help in the field and Rose Johnson and Jennifer Van Renterghen for assistance in the greenhouse. Heather Baron assisted with the GIS analysis and produced the maps in Fig. 1. K.M. Kettenring was supported by a Smithsonian Institution Post-Doctoral Fellowship. NR 39 TC 21 Z9 22 U1 6 U2 38 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0304-3770 J9 AQUAT BOT JI Aquat. Bot. PD OCT PY 2010 VL 93 IS 3 BP 163 EP 169 DI 10.1016/j.aquabot.2010.06.001 PG 7 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA 650UH UT WOS:000281877600004 ER PT J AU Dickinson, EC David, N Overstreet, LK Steinheimer, FD Jansen, J AF Dickinson, Edward C. David, Normand Overstreet, Leslie K. Steinheimer, Frank D. Jansen, Justin TI Histoire naturelle des pigeons or Les pigeons: Coenraad Jacob Temminck versus Pauline Knip SO ARCHIVES OF NATURAL HISTORY LA English DT Article DE Pauline de Courcelles; fine art; wrappers; deceit; Empress Marie Louise Bonaparte; Napoleon Bonaparte AB Evidence for the dates of the parts of C. J. Temminck's Histoire naturelle des pigeons was planted by the artist who, with the benefit of royal patronage, had earlier made herself the apparent architect of the work as a whole and renamed it Les pigeons. We here reveal the flaws in the planted evidence, available in Philadelphia, and how these flaws show when she committed the deed. Wrappers play a major role, and a set in Berlin reveals the true dates of publication. The consequence is that the work must be seen as two works: one, the combined issue of the last parts where the artist must be allowed her pride of place; the other, the bulk of the work where her evidence crumbles and Temminck is undoubtedly and lead player in the publication not just the author. C1 [Overstreet, Leslie K.] Smithsonian Inst Libraries, Washington, DC 20013 USA. [Steinheimer, Frank D.] Nat Kundliches Univ Museum, D-06108 Halle, Saale, Germany. RP Dickinson, EC (reprint author), Flat 3,19 Bolsover Rd, Eastbourne BN20 7JG, England. EM edward@asiaorn.org NR 25 TC 2 Z9 2 U1 0 U2 0 PU EDINBURGH UNIV PRESS PI EDINBURGH PA 22 GEORGE SQUARE, EDINBURGH EH8 9LF, MIDLOTHIAN, SCOTLAND SN 0260-9541 J9 ARCH NAT HIST JI Arch. Nat. Hist. PD OCT PY 2010 VL 37 IS 2 BP 203 EP 220 DI 10.3366/E0260954110001944 PG 18 WC History & Philosophy Of Science; Multidisciplinary Sciences SC History & Philosophy of Science; Science & Technology - Other Topics GA 846JC UT WOS:000296892200002 ER PT J AU Olson, SL AF Olson, Storrs L. TI James Petiver's "Mary-Land Yellow-Throat" - a bird misidentified through four centuries SO ARCHIVES OF NATURAL HISTORY LA English DT Article DE common yellowthroat; Dendroica dominica; George Edwards; Geothlypis trichas; Hugh Jones; Parulidae; yellow-throated warbler AB The name "Mary-Land Yellow-Throat" coined by James Petiver in 1702 was subsequently applied to the bird now known as the common yellowthroat, Geothlypis trichas, and the term "yellowthroat", ultimately derivable from Petiver, is now used as a generic term for all nine species of the warbler genus Geothlypis (Parulidae). Re-examination of Petiver's illustration shows that his bird cannot have been a Geothlypis warbler and was almost certainly the yellow-throated warbler, Dendroica dominica. C1 Smithsonian Inst, Div Birds, Dept Vertebrate Zool, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Olson, SL (reprint author), Smithsonian Inst, Div Birds, Dept Vertebrate Zool, Natl Museum Nat Hist, POB 37012, Washington, DC 20013 USA. EM olsons@si.edu NR 26 TC 0 Z9 0 U1 1 U2 1 PU EDINBURGH UNIV PRESS PI EDINBURGH PA 22 GEORGE SQUARE, EDINBURGH EH8 9LF, MIDLOTHIAN, SCOTLAND SN 0260-9541 J9 ARCH NAT HIST JI Arch. Nat. Hist. PD OCT PY 2010 VL 37 IS 2 BP 221 EP 226 DI 10.3366/E0260954110001956 PG 6 WC History & Philosophy Of Science; Multidisciplinary Sciences SC History & Philosophy of Science; Science & Technology - Other Topics GA 846JC UT WOS:000296892200003 ER PT J AU Dorr, LJ AF Dorr, L. J. TI "Muy poco se sabe de los resultados": Francis E. Bond's expedition to the Paria Peninsula and delta of the Orinoco, Venezuela (1911) SO ARCHIVES OF NATURAL HISTORY LA English DT Article DE James Bond; Stewardson Brown; Thomas S. Gillin; natural history exploration AB The natural history expedition of the American banker and stock broker Francis E. Bond and companions to the Paria Peninsula and delta of the Orinoco. Venezuela, in early 1911 is described. Biographical details are provided for the three principals; Francis E. Bond, Stewardson Brown and Thomas S. Gillin. The itinerary of their three and a half month expedition is elaborated, and notes are provided on the collections of plants, animals, and artefacts that they gathered in South America and deposited in the Academy of Natural Sciences of Philadelphia on their return. C1 Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Dorr, LJ (reprint author), Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, MRC-166,POB 37012, Washington, DC 20013 USA. EM dorrl@si.edu NR 91 TC 1 Z9 1 U1 0 U2 0 PU EDINBURGH UNIV PRESS PI EDINBURGH PA 22 GEORGE SQUARE, EDINBURGH EH8 9LF, MIDLOTHIAN, SCOTLAND SN 0260-9541 J9 ARCH NAT HIST JI Arch. Nat. Hist. PD OCT PY 2010 VL 37 IS 2 BP 292 EP 308 DI 10.3366/E0260954110002019 PG 17 WC History & Philosophy Of Science; Multidisciplinary Sciences SC History & Philosophy of Science; Science & Technology - Other Topics GA 846JC UT WOS:000296892200009 PM 21137585 ER PT J AU Laycock, S Tang, S Grindlay, J Los, E Simcoe, R Mink, D AF Laycock, S. Tang, S. Grindlay, J. Los, E. Simcoe, R. Mink, D. TI DIGITAL ACCESS TO A SKY CENTURY AT HARVARD: INITIAL PHOTOMETRY AND ASTROMETRY SO ASTRONOMICAL JOURNAL LA English DT Article DE astrometry; stars: variables: general; techniques: photometric ID GUIDE STAR CATALOG; PHOTOGRAPHIC PHOTOMETRY; PLATES AB Digital Access to a Sky Century at Harvard (DASCH) is a project to digitize the collection of similar to 500,000 glass photographic plates held at Harvard College Observatory. The collection spans the time period from 1880 to 1985, during which time every point on the sky was been observed from 500 to 1000 times. In this paper, we describe the DASCH commissioning run, during which we developed the data-reduction pipeline, characterized the plates and fine-tuned the digitizer's performance and operation. This initial run consisted of 500 plates taken from a variety of different plate series, all containing the open cluster Praeseppe (M44). We report that accurate photometry at the 0.1 mag level is possible on the majority of plates, and demonstrate century-long light curves of various types of variable stars in and around M44. DASCH will generate a public online archive of the entire plate collection, including images, source catalogs, and light curves for nearly all astronomical objects brighter than about 17th magnitude. C1 [Laycock, S.] Gemini Observ, Hilo, HI 96720 USA. [Tang, S.; Grindlay, J.; Los, E.; Simcoe, R.; Mink, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Laycock, S (reprint author), Gemini Observ, 670 N AOHoku Pl, Hilo, HI 96720 USA. EM silas@head.cfa.harvard.edu OI Mink, Jessica/0000-0003-3594-1823 FU NSF [AST-0407380] FX We thank our colleagues at Harvard and beyond who have offered advice and expertise in photographic astronomy, digitization, and software development. In particular, we thank A. Doane, G. Champine, and A. Sliski for their inestimable contributions. DASCH has been supported by NSF grant AST-0407380 for which we are grateful. S.L. acknowledges the generous support of Gemini Observatory. NR 24 TC 14 Z9 14 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD OCT PY 2010 VL 140 IS 4 BP 1062 EP 1077 DI 10.1088/0004-6256/140/4/1062 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 648VM UT WOS:000281722500016 ER PT J AU Bacmann, A Caux, E Hily-Blant, P Parise, B Pagani, L Bottinelli, S Maret, S Vastel, C Ceccarelli, C Cernicharo, J Henning, T Castets, A Coutens, A Bergin, EA Blake, GA Crimier, N Demyk, K Dominik, C Gerin, M Hennebelle, P Kahane, C Klotz, A Melnick, G Schilke, P Wakelam, V Walters, A Baudry, A Bell, T Benedettini, M Boogert, A Cabrit, S Caselli, P Codella, C Comito, C Encrenaz, P Falgarone, E Fuente, A Goldsmith, PF Helmich, F Herbst, E Jacq, T Kama, M Langer, W Lefloch, B Lis, D Lord, S Lorenzani, A Neufeld, D Nisini, B Pacheco, S Pearson, J Phillips, T Salez, M Saraceno, P Schuster, K Tielens, X van der Tak, FFS van der Wiel, MHD Viti, S Wyrowski, F Yorke, H Faure, A Benz, A Coeur-Joly, O Cros, A Gusten, R Ravera, L AF Bacmann, A. Caux, E. Hily-Blant, P. Parise, B. Pagani, L. Bottinelli, S. Maret, S. Vastel, C. Ceccarelli, C. Cernicharo, J. Henning, T. Castets, A. Coutens, A. Bergin, E. A. Blake, G. A. Crimier, N. Demyk, K. Dominik, C. Gerin, M. Hennebelle, P. Kahane, C. Klotz, A. Melnick, G. Schilke, P. Wakelam, V. Walters, A. Baudry, A. Bell, T. Benedettini, M. Boogert, A. Cabrit, S. Caselli, P. Codella, C. Comito, C. Encrenaz, P. Falgarone, E. Fuente, A. Goldsmith, P. F. Helmich, F. Herbst, E. Jacq, T. Kama, M. Langer, W. Lefloch, B. Lis, D. Lord, S. Lorenzani, A. Neufeld, D. Nisini, B. Pacheco, S. Pearson, J. Phillips, T. Salez, M. Saraceno, P. Schuster, K. Tielens, X. van der Tak, F. F. S. van der Wiel, M. H. D. Viti, S. Wyrowski, F. Yorke, H. Faure, A. Benz, A. Coeur-Joly, O. Cros, A. Guesten, R. Ravera, L. TI First detection of ND in the solar-mass protostar IRAS16293-2422 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: molecules; stars: formation ID DOUBLY DEUTERATED FORMALDEHYDE; STAR-FORMING REGIONS; DEUTERIUM FRACTIONATION; MOLECULAR-SPECTROSCOPY; COLOGNE DATABASE; CORES; TRANSITION; METHANOL; AMMONIA; CDMS AB Context. In the past decade, much progress has been made in characterising the processes leading to the enhanced deuterium fractionation observed in the ISM and in particular in the cold, dense parts of star forming regions such as protostellar envelopes. Very high molecular D/H ratios have been found for saturated molecules and ions. However, little is known about the deuterium fractionation in radicals, even though simple radicals often represent an intermediate stage in the formation of more complex, saturated molecules. The imidogen radical NH is such an intermediate species for the ammonia synthesis in the gas phase. Many of these light molecules however have their fundamental transitions in the submillimetre domain and their detection is hampered by the opacity of the atmosphere at these wavelengths. Herschel/HIFI represents a unique opportunity to study the deuteration and formation mechanisms of species not observable from the ground. Aims. We searched here for the deuterated radical ND in order to determine the deuterium fractionation of imidogen and constrain the deuteration mechanism of this species. Methods. We observed the solar-mass Class 0 protostar IRAS16293-2422 with the heterodyne instrument HIFI in Bands 1a (480-560 GHz), 3b (858-961 GHz), and 4a (949-1061 GHz) as part of the Herschel key programme CHESS (Chemical HErschel Survey of Star forming regions). Results. The deuterated form of the imidogen radical ND was detected and securely identified with 2 hyperfine component groups of its fundamental transition (N = 0-1) at 522.1 and 546.2 GHz, in absorption against the continuum background emitted from the nascent protostar. The 3 groups of hyperfine components of its hydrogenated counterpart NH were also detected in absorption. The absorption arises from the cold envelope, where many deuterated species have been shown to be abundant. The estimated column densities are similar to 2 x 10(14) cm(-2) for NH and similar to 1.3 x 10(14) cm(-2) for ND. We derive a very high deuterium fractionation with an [ND]/[NH] ratio of between 30 and 100%. Conclusions. The deuterium fractionation of imidogen is of the same order of magnitude as that in other molecules, which suggests that an efficient deuterium fractionation mechanism is at play. We discuss two possible formation pathways for ND, by means of either the reaction of N+ with HD, or deuteron/proton exchange with NH. C1 [Bacmann, A.; Hily-Blant, P.; Maret, S.; Ceccarelli, C.; Castets, A.; Crimier, N.; Kahane, C.; Lefloch, B.; Pacheco, S.; Faure, A.] Univ Grenoble 1, CNRS, UMR 5571, Lab Astrophys Grenoble, Grenoble, France. [Bacmann, A.; Ceccarelli, C.; Wakelam, V.; Baudry, A.] Univ Bordeaux, Lab Astrophys Bordeaux, Floirac, France. [Boogert, A.; Lord, S.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91109 USA. [Benedettini, M.; Saraceno, P.] INAF Ist Fis Spazio Interplanetario, Rome, Italy. [Caux, E.; Bottinelli, S.; Vastel, C.; Coutens, A.; Demyk, K.; Klotz, A.; Walters, A.; Coeur-Joly, O.; Cros, A.; Ravera, L.] Univ Toulouse 3, Ctr Etud Spatiale Rayonnements, F-31062 Toulouse, France. [Caselli, P.] Univ Leeds, Sch Phys & Astron, Leeds, W Yorkshire, England. [Pagani, L.; Cabrit, S.; Encrenaz, P.; Salez, M.] Observ Paris, LERMA, F-75014 Paris, France. [Pagani, L.; Cabrit, S.; Encrenaz, P.; Salez, M.] Observ Paris, CNRS, UMR 8112, F-75014 Paris, France. [Cernicharo, J.; Crimier, N.] CSIC INTA, Ctr Astrobiol, Madrid, Spain. [Parise, B.; Schilke, P.; Comito, C.; Wyrowski, F.; Guesten, R.] Max Planck Inst Radioastron, D-5300 Bonn, Germany. [Codella, C.; Lorenzani, A.] INAF Osservatorio Astrofis Arcetri, Florence, Italy. [Dominik, C.; Kama, M.] Univ Amsterdam, Astron Inst Anton Pannekoek, Amsterdam, Netherlands. [Dominik, C.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6525 ED Nijmegen, Netherlands. [Fuente, A.] IGN Observ Astron Nacl, Alcala De Henares, Spain. [Goldsmith, P. F.; Langer, W.; Pearson, J.; Yorke, H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Helmich, F.; van der Tak, F. F. S.; van der Wiel, M. H. D.] SRON Netherlands Inst Space Res, Groningen, Netherlands. [Herbst, E.] Ohio State Univ, Columbus, OH 43210 USA. [Melnick, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Neufeld, D.] Johns Hopkins Univ, Baltimore, MD USA. [Schilke, P.] Univ Cologne, Inst Phys, Cologne, Germany. [Schuster, K.] Inst Radio Astron Millimetr, Grenoble, France. [Tielens, X.] Leiden Univ, Leiden Observ, Leiden, Netherlands. [Viti, S.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Nisini, B.] INAF Osservatorio Astron Roma, Monte Porzio Catone, Italy. [Bergin, E. A.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Henning, T.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [van der Tak, F. F. S.; van der Wiel, M. H. D.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AB Groningen, Netherlands. [Gerin, M.; Hennebelle, P.; Falgarone, E.; Salez, M.] UCP, UPMC, ENS,UMR CNRS INSU 8112, OP,Lab Etud Rayonnement & Matiere Astrophys, Paris, France. [Caux, E.; Bottinelli, S.; Vastel, C.; Coutens, A.; Demyk, K.; Klotz, A.; Walters, A.; Coeur-Joly, O.; Cros, A.; Ravera, L.] CNRS INSU, UMR 5187, Toulouse, France. [Bacmann, A.; Ceccarelli, C.; Wakelam, V.; Baudry, A.; Jacq, T.] CNRS INSU, UMR 5804, Floirac, France. [Benz, A.] ETH, Inst Astron, CH-8092 Zurich, Switzerland. RP Bacmann, A (reprint author), Univ Grenoble 1, CNRS, UMR 5571, Lab Astrophys Grenoble, Grenoble, France. EM aurore.bacmann@obs.ujf-grenoble.fr RI van der Wiel, Matthijs/M-4531-2014; Coutens, Audrey/M-4533-2014; Fuente, Asuncion/G-1468-2016; Goldsmith, Paul/H-3159-2016; OI van der Wiel, Matthijs/0000-0002-4325-3011; Coutens, Audrey/0000-0003-1805-3920; Fuente, Asuncion/0000-0001-6317-6343; Lorenzani, Andrea/0000-0002-4685-3434; Wakelam, Valentine/0000-0001-9676-2605; Kama, Mihkel/0000-0003-0065-7267; Codella, Claudio/0000-0003-1514-3074; , Brunella Nisini/0000-0002-9190-0113; Maret, Sebastien/0000-0003-1104-4554 NR 32 TC 26 Z9 26 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 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR L42 DI 10.1051/0004-6361/201015102 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900042 ER PT J AU Benz, AO Bruderer, S van Dishoeck, EF Stauber, P Wampfler, SF Melchior, M Dedes, C Wyrowski, F Doty, SD van der Tak, F Bachtold, W Csillaghy, A Megej, A Monstein, C Soldati, M Bachiller, R Baudry, A Benedettini, M Bergin, E Bjerkeli, P Blake, GA Bontemps, S Braine, J Caselli, P Cernicharo, J Codella, C Daniel, F di Giorgio, AM Dieleman, P Dominik, C Encrenaz, P Fich, M Fuente, A Giannini, T Goicoechea, JR de Graauw, T Helmich, F Herczeg, GJ Herpin, F Hogerheijde, MR Jacq, T Jellema, W Johnstone, D Jorgensen, JK Kristensen, LE Larsson, B Lis, D Liseau, R Marseille, M McCoey, C Melnick, G Neufeld, D Nisini, B Olberg, M Ossenkopf, V Parise, B Pearson, JC Plume, R Risacher, C Santiago-Garcia, J Saraceno, P Schieder, R Shipman, R Stutzki, J Tafalla, M Tielens, AGGM van Kempen, TA Visser, R Yildiz, UA AF Benz, A. O. Bruderer, S. van Dishoeck, E. F. Staeuber, P. Wampfler, S. F. Melchior, M. Dedes, C. Wyrowski, F. Doty, S. D. van der Tak, F. Baechtold, W. Csillaghy, A. Megej, A. Monstein, C. Soldati, M. Bachiller, R. Baudry, A. Benedettini, M. Bergin, E. Bjerkeli, P. Blake, G. A. Bontemps, S. Braine, J. Caselli, P. Cernicharo, J. Codella, C. Daniel, F. di Giorgio, A. M. Dieleman, P. Dominik, C. Encrenaz, P. Fich, M. Fuente, A. Giannini, T. Goicoechea, J. R. de Graauw, Th. Helmich, F. Herczeg, G. J. Herpin, F. Hogerheijde, M. R. Jacq, T. Jellema, W. Johnstone, D. Jorgensen, J. K. Kristensen, L. E. Larsson, B. Lis, D. Liseau, R. Marseille, M. McCoey, C. Melnick, G. Neufeld, D. Nisini, B. Olberg, M. Ossenkopf, V. Parise, B. Pearson, J. C. Plume, R. Risacher, C. Santiago-Garcia, J. Saraceno, P. Schieder, R. Shipman, R. Stutzki, J. Tafalla, M. Tielens, A. G. G. M. van Kempen, T. A. Visser, R. Yildiz, U. A. TI Hydrides in young stellar objects: Radiation tracers in a protostar-disk-outflow system SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE astrochemistry; line: identification; stars: formation; stars: massive; photon-dominated region; submillimeter: ISM ID H2O+; SPECTROSCOPY; CHEMISTRY; REGIONS; W3IRS5; DR21; H3O+ AB Context. Hydrides of the most abundant heavier elements are fundamental molecules in cosmic chemistry. Some of them trace gas irradiated by UV or X-rays. Aims. We explore the abundances of major hydrides in W3 IRS5, a prototypical region of high-mass star formation. Methods. W3 IRS5 was observed by HIFI on the Herschel Space Observatory with deep integration (similar or equal to 2500 s) in 8 spectral regions. Results. The target lines including CH, NH, H3O+, and the new molecules SH+, H2O+, and OH+ are detected. The H2O+ and OH+ J = 1-0 lines are found mostly in absorption, but also appear to exhibit weak emission (P-Cyg-like). Emission requires high density, thus originates most likely near the protostar. This is corroborated by the absence of line shifts relative to the young stellar object (YSO). In addition, H2O+ and OH+ also contain strong absorption components at a velocity shifted relative to W3 IRS5, which are attributed to foreground clouds. Conclusions. The molecular column densities derived from observations correlate well with the predictions of a model that assumes the main emission region is in outflow walls, heated and irradiated by protostellar UV radiation. C1 [Benz, A. O.; Bruderer, S.; Staeuber, P.; Wampfler, S. F.; Melchior, M.; Dedes, C.; Monstein, C.] ETH, Inst Astron, CH-8093 Zurich, Switzerland. [van Dishoeck, E. F.; Hogerheijde, M. R.; Kristensen, L. E.; Tielens, A. G. G. M.; Visser, R.; Yildiz, U. A.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [van Dishoeck, E. F.; Herczeg, G. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Caselli, P.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Caselli, P.; Codella, C.; Jacq, T.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Baudry, A.; Bontemps, S.; Braine, J.; Herpin, F.] Univ Bordeaux, Lab Astrophys Bordeaux, Bordeaux, France. [Baudry, A.; Bontemps, S.; Braine, J.; Herpin, F.] CNRS INSU, UMR 5804, Floirac, France. [Johnstone, D.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Johnstone, D.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 1A1, Canada. [Bjerkeli, P.; Liseau, R.; Olberg, M.] Chalmers, Onsala Space Observ, Dept Radio & Space Sci, S-43992 Onsala, Sweden. [van der Tak, F.; Dieleman, P.; de Graauw, Th.; Helmich, F.; Jellema, W.; Marseille, M.; Risacher, C.; Shipman, R.] SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [van der Tak, F.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Bachiller, R.; Tafalla, M.] Observ Astron Nacl IGN, Madrid 28014, Spain. [Benedettini, M.; di Giorgio, A. M.; Saraceno, P.] INAF Ist Fis Spazio Interplanetario, Area Ric Tor Vergata, I-00133 Rome, Italy. [Bergin, E.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Cernicharo, J.; Daniel, F.; Goicoechea, J. R.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Dominik, C.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. [Dominik, C.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands. [Doty, S. D.] Denison Univ, Dept Phys & Astron, Granville, OH 43023 USA. [Encrenaz, P.] Observ Paris, LERMA, F-75014 Paris, France. [Encrenaz, P.] Observ Paris, CNRS, UMR 8112, F-75014 Paris, France. [Fich, M.; McCoey, C.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [Fuente, A.] Observ Astron Nacl, Alcala De Henares 28803, Spain. [Giannini, T.; Nisini, B.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy. [Jorgensen, J. K.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark. [Larsson, B.] Stockholm Univ, Dept Astron, S-10691 Stockholm, Sweden. [Lis, D.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [McCoey, C.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [Melnick, G.; van Kempen, T. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Neufeld, D.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Wyrowski, F.; Parise, B.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Pearson, J. C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Plume, R.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Santiago-Garcia, J.] Inst Radio Astron Millimetr, Granada 18012, Spain. [Ossenkopf, V.; Schieder, R.; Stutzki, J.] Univ Cologne, Inst Phys 1, KOSMA, D-50937 Cologne, Germany. [Melchior, M.; Csillaghy, A.; Soldati, M.] Univ Appl Sci NW, Inst Technol 4D, CH-5210 Windisch, Switzerland. [Baechtold, W.; Megej, A.] ETH, Lab Electromagnet Fields & Microwave Elect, CH-8092 Zurich, Switzerland. RP Benz, AO (reprint author), ETH, Inst Astron, CH-8093 Zurich, Switzerland. EM benz@astro.phys.ethz.ch RI Yildiz, Umut/C-5257-2011; Kristensen, Lars/F-4774-2011; Visser, Ruud/J-8574-2012; Jorgensen, Jes Kristian/L-7936-2014; Wampfler, Susanne/D-2270-2015; Fuente, Asuncion/G-1468-2016; OI Giannini, Teresa/0000-0002-0224-096X; Yildiz, Umut/0000-0001-6197-2864; Kristensen, Lars/0000-0003-1159-3721; Jorgensen, Jes Kristian/0000-0001-9133-8047; Wampfler, Susanne/0000-0002-3151-7657; Fuente, Asuncion/0000-0001-6317-6343; Bjerkeli, Per/0000-0002-7993-4118; Codella, Claudio/0000-0003-1514-3074; , Brunella Nisini/0000-0002-9190-0113 FU Swiss National Science Foundation [200020-113556] FX We thank Michael Kaufman and Serena Viti for helpful comments on an early draft. This program is made possible thanks to the Swiss Herschel guaranteed time program. HIFI has been designed and built by a consortium of institutes and university departments from across Europe, Canada and the United States under the leadership of SRON Netherlands Institute for Space Research Groningen, The Netherlands and with major contributions from Germany, France, and the US. Consortium members are: Canada:CSA, U. Waterloo; France: CESR, LAB, LERMA, IRAM; Germany: KOSMA, MPIfR, MPS; Ireland: NUI Maynooth; Italy: ASI, IFSI-INAF, Osservatorio Astrofisico di Arcetri-INAF; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astronomico Nacional (IGN), Centro de Astrobiologia (CSIC-INT); Sweden: Chalmers University of Technology, Onsala Space Observatory, Swedish National Space Board, Stockholm University; Switzerland: ETH Zurich, FHNW; USA: Caltech, JPL, NHSC. The work on star formation at ETH Zurich is partially funded by the Swiss National Science Foundation (grant no. 200020-113556). NR 27 TC 44 Z9 44 U1 1 U2 5 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR L35 DI 10.1051/0004-6361/201015111 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900035 ER PT J AU Bergin, EA Phillips, TG Comito, C Crockett, NR Lis, DC Schilke, P Wang, S Bell, TA Blake, GA Bumble, B Caux, E Cabrit, S Ceccarelli, C Cernicharo, J Daniel, F de Graauw, T Dubernet, ML Emprechtinger, M Encrenaz, P Falgarone, E Gerin, M Giesen, TF Goicoechea, JR Goldsmith, PF Gupta, H Hartogh, P Helmich, FP Herbst, E Joblin, C Johnstone, D Kawamura, JH Langer, WD Latter, WB Lord, SD Maret, S Martin, PG Melnick, GJ Menten, KM Morris, P Muller, HSP Murphy, JA Neufeld, DA Ossenkopf, V Pagani, L Pearson, JC Perault, M Plume, R Roelfsema, P Qin, SL Salez, M Schlemmer, S Stutzki, J Tielens, AGGM Trappe, N van der Tak, FFS Vastel, C Yorke, HW Yu, S Zmuidzinas, J AF Bergin, E. A. Phillips, T. G. Comito, C. Crockett, N. R. Lis, D. C. Schilke, P. Wang, S. Bell, T. A. Blake, G. A. Bumble, B. Caux, E. Cabrit, S. Ceccarelli, C. Cernicharo, J. Daniel, F. de Graauw, Th. Dubernet, M. -L. Emprechtinger, M. Encrenaz, P. Falgarone, E. Gerin, M. Giesen, T. F. Goicoechea, J. R. Goldsmith, P. F. Gupta, H. Hartogh, P. Helmich, F. P. Herbst, E. Joblin, C. Johnstone, D. Kawamura, J. H. Langer, W. D. Latter, W. B. Lord, S. D. Maret, S. Martin, P. G. Melnick, G. J. Menten, K. M. Morris, P. Mueller, H. S. P. Murphy, J. A. Neufeld, D. A. Ossenkopf, V. Pagani, L. Pearson, J. C. Perault, M. Plume, R. Roelfsema, P. Qin, S. -L. Salez, M. Schlemmer, S. Stutzki, J. Tielens, A. G. G. M. Trappe, N. van der Tak, F. F. S. Vastel, C. Yorke, H. W. Yu, S. Zmuidzinas, J. TI Herschel observations of EXtra-Ordinary Sources (HEXOS): The present and future of spectral surveys with Herschel/ HIFI SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: abundances; ISM: molecules; submillimeter: ISM ID LINE SURVEY; ORION KL; MOLECULAR-SPECTROSCOPY; COLOGNE DATABASE; HOT CORES; WATER; SUBMILLIMETER; GHZ; CLOUDS; BAND AB We present initial results from the Herschel GT key program: Herschel observations of EXtra-Ordinary Sources (HEXOS) and outline the promise and potential of spectral surveys with Herschel/HIFI. The HIFI instrument offers unprecedented sensitivity, as well as continuous spectral coverage across the gaps imposed by the atmosphere, opening up a largely unexplored wavelength regime to high-resolution spectroscopy. We show the spectrum of Orion KL between 480 and 560 GHz and from 1.06 to 1.115 THz. From these data, we confirm that HIFI separately measures the dust continuum and spectrally resolves emission lines in Orion KL. Based on this capability we demonstrate that the line contribution to the broad-band continuum in this molecule-rich source is similar to 20-40% below 1 THz and declines to a few percent at higher frequencies. We also tentatively identify multiple transitions of (HDO)-O-18 in the spectra. The first detection of this rare isotopologue in the interstellar medium suggests that HDO emission is optically thick in the Orion hot core with HDO/H2O similar to 0.02. We discuss the implications of this detection for the water D/H ratio in hot cores. C1 [Bergin, E. A.; Crockett, N. R.; Wang, S.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Phillips, T. G.; Lis, D. C.; Bell, T. A.; Emprechtinger, M.; Zmuidzinas, J.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Comito, C.; Schilke, P.; Menten, K. M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Schilke, P.; Giesen, T. F.; Mueller, H. S. P.; Ossenkopf, V.; Qin, S. -L.; Schlemmer, S.; Stutzki, J.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Blake, G. A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Bumble, B.; Goldsmith, P. F.; Gupta, H.; Kawamura, J. H.; Langer, W. D.; Pearson, J. C.; Yorke, H. W.; Yu, S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Caux, E.; Joblin, C.; Vastel, C.] Univ Toulouse UPS, Ctr Etud Spatiale Rayonnements, F-31062 Toulouse 9, France. [Caux, E.; Joblin, C.; Vastel, C.] CNRS INSU, UMR 5187, F-31028 Toulouse 4, France. [Cabrit, S.; Pagani, L.; Salez, M.] LERMA, F-75014 Paris, France. [Ceccarelli, C.; Maret, S.] Lab Astrophys Observ Grenoble, F-38041 Grenoble 9, France. [Cernicharo, J.; Daniel, F.; Goicoechea, J. R.] Ctr Astrobiol CSIC INTA, Lab Astrofis Mol, Madrid 28850, Spain. [Cabrit, S.; Pagani, L.; Salez, M.] Observ Paris, CNRS, UMR8112, F-75014 Paris, France. [Daniel, F.; Encrenaz, P.; Falgarone, E.; Gerin, M.; Perault, M.] Observ Paris, UMR8112, CNRS, LERMA, F-75231 Paris 05, France. [Daniel, F.; Encrenaz, P.; Falgarone, E.; Gerin, M.; Perault, M.] Ecole Normale Super, F-75231 Paris 05, France. [de Graauw, Th.; Helmich, F. P.; Ossenkopf, V.; Roelfsema, P.; van der Tak, F. F. S.] Univ Groningen, SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [Dubernet, M. -L.] Univ Paris 06, LPMAA, UMR7092, Paris, France. [Dubernet, M. -L.] Observ Paris, LUTH, UMR8102, Meudon, France. [Hartogh, P.] MPI Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. [Herbst, E.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Herbst, E.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Herbst, E.] Ohio State Univ, Dept Chem, Columbus, OH 43210 USA. [Johnstone, D.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Latter, W. B.; Lord, S. D.; Morris, P.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Martin, P. G.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Melnick, G. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Murphy, J. A.; Trappe, N.] Natl Univ Ireland Maynooth, Maynooth, Kildare, Ireland. [Neufeld, D. A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Plume, R.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Tielens, A. G. G. M.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. RP Bergin, EA (reprint author), Univ Michigan, Dept Astron, 500 Church St, Ann Arbor, MI 48109 USA. EM ebergin@umich.edu RI Giesen, Thomas /B-9476-2015; Schlemmer, Stephan/E-2903-2015; Trappe, Neil/C-9014-2016; Yu, Shanshan/D-8733-2016; Goldsmith, Paul/H-3159-2016; OI Maret, Sebastien/0000-0003-1104-4554; Giesen, Thomas /0000-0002-2401-0049; Schlemmer, Stephan/0000-0002-1421-7281; Trappe, Neil/0000-0003-2527-9821; Mueller, Holger/0000-0002-0183-8927 FU NASA 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; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio AstronU mico Nacional (IGN), Centro de AstrobiologSa (CSIC-INTA). Sweden: Chalmers University of Technology -MC2, RSS & GARD; Onsala Space Observatory; Swedish National Space Board, Stockholm University -Stockholm Observatory; Switzerland: ETH Zurich, FHNW; USA: Caltech, JPL, NHSC. The HEXOS team also is grateful to the HIFI instrument team for building a fantastic instrument. Support for this work was provided by NASA through an award issued by JPL/Caltech. NR 29 TC 73 Z9 73 U1 0 U2 5 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR L20 DI 10.1051/0004-6361/201015071 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900020 ER PT J AU Bergin, EA Hogerheijde, MR Brinch, C Fogel, J Yildiz, UA Kristensen, LE van Dishoeck, EF Bell, TA Blake, GA Cernicharo, J Dominik, C Lis, D Melnick, G Neufeld, D Panic, O Pearson, JC Bachiller, R Baudry, A Benedettini, M Benz, AO Bjerkeli, P Bontemps, S Braine, J Bruderer, S Caselli, P Codella, C Daniel, F di Giorgio, AM Doty, SD Encrenaz, P Fich, M Fuente, A Giannini, T Goicoechea, JR de Graauw, T Helmich, F Herczeg, GJ Herpin, F Jacq, T Johnstone, D Jorgensen, JK Larsson, B Liseau, R Marseille, M Mc Coey, C Nisini, B Olberg, M Parise, B Plume, R Risacher, C Santiago-Garcia, J Saraceno, P Shipman, R Tafalla, M van Kempen, TA Visser, R Wampfler, SF Wyrowski, F van der Tak, F Jellema, W Tielens, AGGM Hartogh, P Stutzki, J Szczerba, R AF Bergin, E. A. Hogerheijde, M. R. Brinch, C. Fogel, J. Yildiz, U. A. Kristensen, L. E. van Dishoeck, E. F. Bell, T. A. Blake, G. A. Cernicharo, J. Dominik, C. Lis, D. Melnick, G. Neufeld, D. Panic, O. Pearson, J. C. Bachiller, R. Baudry, A. Benedettini, M. Benz, A. O. Bjerkeli, P. Bontemps, S. Braine, J. Bruderer, S. Caselli, P. Codella, C. Daniel, F. di Giorgio, A. M. Doty, S. D. Encrenaz, P. Fich, M. Fuente, A. Giannini, T. Goicoechea, J. R. de Graauw, Th Helmich, F. Herczeg, G. J. Herpin, F. Jacq, T. Johnstone, D. Jorgensen, J. K. Larsson, B. Liseau, R. Marseille, M. Mc Coey, C. Nisini, B. Olberg, M. Parise, B. Plume, R. Risacher, C. Santiago-Garcia, J. Saraceno, P. Shipman, R. Tafalla, M. van Kempen, T. A. Visser, R. Wampfler, S. F. Wyrowski, F. van der Tak, F. Jellema, W. Tielens, A. G. G. M. Hartogh, P. Stuetzki, J. Szczerba, R. TI Sensitive limits on the abundance of cold water vapor in the DM Tauri protoplanetary disk SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: abundances; ISM: molecules; protoplanetary disks ID PLANET-FORMING REGION; CIRCUMSTELLAR DISKS; H2O; STARS; DUST; MOLECULES; SPECTRA; GAS; DESORPTION; EVOLUTION AB We performed a sensitive search for the ground-state emission lines of ortho-and para-water vapor in the DM Tau protoplanetary disk using the Herschel/HIFI instrument. No strong lines are detected down to 3 sigma levels in 0.5 km s(-1) channels of 4.2 mK for the 1(10)-1(01) line and 12.6 mK for the 1(11)-0(00) line. We report a very tentative detection, however, of the 1(10)-1(01) line in the wide band spectrometer, with a strength of T-mb = 2.7 mK, a width of 5.6 km s(-1) and an integrated intensity of 16.0 mK km s(-1). The latter constitutes a 6 sigma detection. Regardless of the reality of this tentative detection, model calculations indicate that our sensitive limits on the line strengths preclude efficient desorption of water in the UV illuminated regions of the disk. We hypothesize that more than 95-99% of the water ice is locked up in coagulated grains that have settled to the midplane. C1 [Bergin, E. A.; Fogel, J.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Hogerheijde, M. R.; Brinch, C.; Yildiz, U. A.; Kristensen, L. E.; van Dishoeck, E. F.; Visser, R.; Tielens, A. G. G. M.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [van Dishoeck, E. F.; Herczeg, G. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Blake, G. A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Cernicharo, J.; Daniel, F.; Goicoechea, J. R.] CSIC INTA, Ctr Astrobiol, Dept Astrofis, Madrid 28850, Spain. [Dominik, C.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. [Dominik, C.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands. [Bell, T. A.; Lis, D.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Melnick, G.; van Kempen, T. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Neufeld, D.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Panic, O.] European So Observ, D-85748 Garching, Germany. [Pearson, J. C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bachiller, R.; Tafalla, M.] Observ Astron Nacl IGN, Madrid 28014, Spain. [Baudry, A.; di Giorgio, A. M.; Herpin, F.; Nisini, B.; Saraceno, P.] INAF Ist Fis Spazio Interplanetario, Area Ric Tor Vergata, I-00133 Rome, Italy. [Benedettini, M.; Caselli, P.; Codella, C.; Jacq, T.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Benz, A. O.; Bruderer, S.; Wampfler, S. F.] ETH, Inst Astron, CH-8093 Zurich, Switzerland. [Bjerkeli, P.; Liseau, R.; Olberg, M.] Chalmers, Onsala Space Observ, Dept Radio & Space Sci, S-43992 Onsala, Sweden. [Bontemps, S.] Univ Bordeaux, Lab Astrophys Bordeaux, Bordeaux, France. [Bontemps, S.] CNRS INSU, UMR 5804, Floirac, France. [Braine, J.; Caselli, P.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Doty, S. D.] Denison Univ, Dept Phys & Astron, Granville, OH 43023 USA. [Encrenaz, P.] Observ Paris, LERMA, F-75014 Paris, France. [Fich, M.; Mc Coey, C.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [Fuente, A.] Observ Astron Nacl, Alcala De Henares 28803, Spain. [Giannini, T.] INAF Osservatorio Astronom Roma, I-00040 Monte Porzio Catone, Italy. [de Graauw, Th; Helmich, F.; Marseille, M.; Risacher, C.; Shipman, R.; van der Tak, F.; Jellema, W.] SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [Johnstone, D.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Johnstone, D.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 1A1, Canada. [Jorgensen, J. K.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen K, Denmark. [Larsson, B.] Stockholm Univ, Dept Astron, S-10691 Stockholm, Sweden. [Mc Coey, C.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [Parise, B.; Wyrowski, F.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Plume, R.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Santiago-Garcia, J.] Inst Radio Astron Millimetr, Granada 18012, Spain. [van der Tak, F.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Hartogh, P.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. [Stuetzki, J.] Univ Cologne, Inst Phys 1, KOSMA, D-50937 Cologne, Germany. [Szczerba, R.] Nicholas Copernicus Astron Ctr, PL-87100 Torun, Poland. RP Bergin, EA (reprint author), Univ Michigan, Dept Astron, 500 Church St, Ann Arbor, MI 48109 USA. EM ebergin@umich.edu RI Yildiz, Umut/C-5257-2011; Kristensen, Lars/F-4774-2011; Visser, Ruud/J-8574-2012; Wampfler, Susanne/D-2270-2015; Brinch, Christian/G-5157-2015; Fuente, Asuncion/G-1468-2016; OI Yildiz, Umut/0000-0001-6197-2864; Kristensen, Lars/0000-0003-1159-3721; Wampfler, Susanne/0000-0002-3151-7657; Brinch, Christian/0000-0002-5074-7183; Fuente, Asuncion/0000-0001-6317-6343; Bjerkeli, Per/0000-0002-7993-4118; Codella, Claudio/0000-0003-1514-3074; Giannini, Teresa/0000-0002-0224-096X; , Brunella Nisini/0000-0002-9190-0113 FU NASA through JPL/Caltech; NSF [0707777]; NWO [639.042.404] 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; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astronomico Nacional (IGN), Centro de Astrobiologia (CSIC-INTA). Sweden: Chalmers University of Technology - MC2, RSS & GARD; Onsala Space Observatory; Swedish National Space Board, Stockholm University - Stockholm Observatory; Switzerland: ETH Zurich, FHNW; USA: Caltech, JPL, NHSC. Support for this work was provided by NASA through an award issued by JPL/Caltech. E.A.B. acknowledges support by NSF Grant 0707777, M.R.H. by NWO grant 639.042.404. NR 37 TC 42 Z9 42 U1 1 U2 4 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR L33 DI 10.1051/0004-6361/201015104 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900033 ER PT J AU Bruderer, S Benz, AO van Dishoeck, EF Melchior, M Doty, SD van der Tak, F Stauber, P Wampfler, SF Dedes, C Yildiz, UA Pagani, L Giannini, T de Graauw, T Whyborn, N Teyssier, D Jellema, W Shipman, R Schieder, R Honingh, N Caux, E Bachtold, W Csillaghy, A Monstein, C Bachiller, R Baudry, A Benedettini, M Bergin, E Bjerkeli, P Blake, GA Bontemps, S Braine, J Caselli, P Cernicharo, J Codella, C Daniel, F di Giorgio, AM Dominik, C Encrenaz, P Fich, M Fuente, A Goicoechea, JR Helmich, F Herczeg, GJ Herpin, F Hogerheijde, MR Jacq, T Johnstone, D Jorgensen, JK Kristensen, LE Larsson, B Lis, D Liseau, R Marseille, M McCoey, C Melnick, G Neufeld, D Nisini, B Olberg, M Parise, B Pearson, JC Plume, R Risacher, C Santiago-Garcia, J Saraceno, P Shipman, R Tafalla, M van Kempen, TA Visser, R Wyrowski, F AF Bruderer, S. Benz, A. O. van Dishoeck, E. F. Melchior, M. Doty, S. D. van der Tak, F. Staeuber, P. Wampfler, S. F. Dedes, C. Yildiz, U. A. Pagani, L. Giannini, T. de Graauw, Th. Whyborn, N. Teyssier, D. Jellema, W. Shipman, R. Schieder, R. Honingh, N. Caux, E. Baechtold, W. Csillaghy, A. Monstein, C. Bachiller, R. Baudry, A. Benedettini, M. Bergin, E. Bjerkeli, P. Blake, G. A. Bontemps, S. Braine, J. Caselli, P. Cernicharo, J. Codella, C. Daniel, F. di Giorgio, A. M. Dominik, C. Encrenaz, P. Fich, M. Fuente, A. Goicoechea, J. R. Helmich, F. Herczeg, G. J. Herpin, F. Hogerheijde, M. R. Jacq, T. Johnstone, D. Jorgensen, J. K. Kristensen, L. E. Larsson, B. Lis, D. Liseau, R. Marseille, M. McCoey, C. Melnick, G. Neufeld, D. Nisini, B. Olberg, M. Parise, B. Pearson, J. C. Plume, R. Risacher, C. Santiago-Garcia, J. Saraceno, P. Shipman, R. Tafalla, M. van Kempen, T. A. Visser, R. Wyrowski, F. TI Herschel/HIFI detections of hydrides towards AFGL 2591 Envelope emission versus tenuous cloud absorption SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: molecules; stars: formation; astrochemistry; ISM: individual objects: AFGL 2591 ID STAR-FORMING REGIONS; INTERSTELLAR-MEDIUM; OUTFLOW; CHEMISTRY; SPECTROSCOPY; GL-2591; H2O+; EXCITATION; ABUNDANCE AB The Heterodyne Instrument for the Far Infrared (HIFI) onboard the Herschel Space Observatory allows the first observations of light diatomic molecules at high spectral resolution and in multiple transitions. Here, we report deep integrations using HIFI in different lines of hydrides towards the high-mass star forming region AFGL 2591. Detected are CH, CH+, NH, OH+, H2O+, while NH+ and SH+ have not been detected. All molecules except for CH and CH+ are seen in absorption with low excitation temperatures and at velocities different from the systemic velocity of the protostellar envelope. Surprisingly, the CH(J(F,P) = 3/2(2),(-) - 1/2(1,+)) and CH+(J = 1-0, J = 2-1) lines are detected in emission at the systemic velocity. We can assign the absorption features to a foreground cloud and an outflow lobe, while the CH and CH+ emission stems from the envelope. The observed abundance and excitation of CH and CH+ can be explained in the scenario of FUV irradiated outflow walls, where a cavity etched out by the outflow allows protostellar FUV photons to irradiate and heat the envelope at larger distances driving the chemical reactions that produce these molecules. C1 [Bruderer, S.; Benz, A. O.; Staeuber, P.; Wampfler, S. F.; Dedes, C.; Monstein, C.] ETH, Inst Astron, CH-8093 Zurich, Switzerland. [van Dishoeck, E. F.; Yildiz, U. A.; Hogerheijde, M. R.; Kristensen, L. E.; Visser, R.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [van Dishoeck, E. F.; Herczeg, G. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Melchior, M.; Csillaghy, A.] FHNW, Inst Technol 4D, CH-5210 Windisch, Switzerland. [Doty, S. D.] Denison Univ, Dept Phys & Astron, Granville, OH 43023 USA. [van der Tak, F.; Jellema, W.; Shipman, R.; Helmich, F.; Marseille, M.; Risacher, C.; Shipman, R.] SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [van der Tak, F.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Pagani, L.] Observ Paris, LERMA, F-75014 Paris, France. [Giannini, T.; Nisini, B.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy. [Pagani, L.] Observ Paris, CNRS, UMR 8112, F-75014 Paris, France. [de Graauw, Th.; Whyborn, N.] Joint ALMA Off, Santiago, Chile. [Teyssier, D.] ESA, European Space Astron Ctr, Madrid 28691, Spain. [Schieder, R.; Honingh, N.] Univ Cologne, Inst Phys 1, KOSMA, D-50937 Cologne, Germany. [Caux, E.] Univ Toulouse UPS, Ctr Etud Spatiale Rayonnements, F-31062 Toulouse 9, France. [Caux, E.] CNRS INSU, UMR 5187, F-31028 Toulouse 4, France. [Baechtold, W.] ETH, Lab Electromagnet Fields Ad Microwave Elect, CH-8092 Zurich, Switzerland. [Bachiller, R.; Tafalla, M.] Observ Astron Nacl IGN, Madrid 28014, Spain. [Baudry, A.; Bontemps, S.; Braine, J.; Herpin, F.] Univ Bordeaux, Lab Astrophys Bordeaux, Bordeaux, France. [Baudry, A.; Bontemps, S.; Braine, J.; Herpin, F.] CNRS INSU, UMR 5804, Floirac, France. [Benedettini, M.; di Giorgio, A. M.; Saraceno, P.] INAF Ist Fis Spazio Interplanetario, Area Ric Tor Vergata, I-00133 Rome, Italy. [Bergin, E.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Bjerkeli, P.; Liseau, R.; Olberg, M.] Chalmers, Onsala Space Observ, Dept Radio & Space Sci, S-43992 Onsala, Sweden. [Blake, G. A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Caselli, P.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Caselli, P.; Codella, C.; Jacq, T.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Cernicharo, J.; Daniel, F.; Goicoechea, J. R.] CSIC INTA, Ctr Astrobiol, Dept Astrofis, Madrid 28850, Spain. [Dominik, C.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. [Dominik, C.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands. [Fich, M.; McCoey, C.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [Fuente, A.] Observ Astron Nacl, Alcala De Henares 28803, Spain. [Johnstone, D.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Johnstone, D.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 1A1, Canada. [Jorgensen, J. K.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen K, Denmark. [Larsson, B.] Stockholm Univ, Dept Astron, S-10691 Stockholm, Sweden. [Lis, D.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [McCoey, C.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [Melnick, G.; van Kempen, T. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Neufeld, D.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Parise, B.; Wyrowski, F.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Pearson, J. C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Plume, R.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Santiago-Garcia, J.] IRAM, E-18012 Granada, Spain. RP Bruderer, S (reprint author), ETH, Inst Astron, CH-8093 Zurich, Switzerland. EM simonbr@astro.phys.ethz.ch RI Yildiz, Umut/C-5257-2011; Kristensen, Lars/F-4774-2011; Visser, Ruud/J-8574-2012; Jorgensen, Jes Kristian/L-7936-2014; Wampfler, Susanne/D-2270-2015; Fuente, Asuncion/G-1468-2016; OI Yildiz, Umut/0000-0001-6197-2864; Kristensen, Lars/0000-0003-1159-3721; Jorgensen, Jes Kristian/0000-0001-9133-8047; Wampfler, Susanne/0000-0002-3151-7657; Fuente, Asuncion/0000-0001-6317-6343; Bjerkeli, Per/0000-0002-7993-4118; Codella, Claudio/0000-0003-1514-3074; Giannini, Teresa/0000-0002-0224-096X; , Brunella Nisini/0000-0002-9190-0113 FU Swiss National Science Foundation [200020-113556] FX We thank the anonymous referee for useful comments. The work on star formation at ETH Zurich is partially funded by the Swiss National Science Foundation grant 200020-113556. This program is made possible thanks to the Swiss HIFI guaranteed time program. HIFI has been designed and built by a consortium of institutes and university departments from acrossEurope, Canada and the United States under the leadership of SRON Netherlands Institute for Space Research, Groningen, The Netherlands and with major contributions from Germany, France and the US. Consortium members are: Canada: CSA, U. Waterloo; France: CESR, LAB, LERMA, IRAM; Germany: KOSMA, MPIfR, MPS; Ireland, NUI Maynooth; Italy: ASI, IFSI-INAF, Osservatorio Astrofisico di Arcetri-INAF; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astronomico Nacional (IGN), Centro de 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, JPL, NHSC. HIPE is a joint development by the Herschel Science Ground Segment Consortium, consisting of ESA, the NASA Herschel Science Center, and the HIFI, PACS and SPIRE consortia. NR 27 TC 31 Z9 31 U1 1 U2 6 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 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR L44 DI 10.1051/0004-6361/201015098 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900044 ER PT J AU Bujarrabal, V Alcolea, J Soria-Ruiz, R Planesas, P Teyssier, D Marston, AP Cernicharo, J Decin, L Dominik, C Justtanont, K de Koter, A Melnick, G Menten, KM Neufeld, DA Olofsson, H Schmidt, M Schoier, FL Szczerba, R Waters, LBFM Quintana-Lacaci, G Gusten, R Gallego, JD Diez-Gonzalez, MC Barcia, A Lopez-Fernandez, I Wildeman, K Tielens, AGGM Jacobs, K AF Bujarrabal, V. Alcolea, J. Soria-Ruiz, R. Planesas, P. Teyssier, D. Marston, A. P. Cernicharo, J. Decin, L. Dominik, C. Justtanont, K. de Koter, A. Melnick, G. Menten, K. M. Neufeld, D. A. Olofsson, H. Schmidt, M. Schoier, F. L. Szczerba, R. Waters, L. B. F. M. Quintana-Lacaci, G. Guesten, R. Gallego, J. D. Diez-Gonzalez, M. C. Barcia, A. Lopez-Fernandez, I. Wildeman, K. Tielens, A. G. G. M. Jacobs, K. TI Herschel/HIFI observations of high-J CO transitions in the protoplanetary nebula CRL 618 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: AGB and post-AGB; circumstellar matter; stars: mass-loss; planetary nebulae: general; planetary nebulae: individual: CRL 618 ID HETERODYNE INSTRUMENT; MOLECULAR ENVELOPE; CRL-618; DYNAMICS; FACILITY; APEX AB Aims. We aim to study the physical conditions, particularly the excitation state, of the intermediate-temperature gas components in the protoplanetary nebula CRL 618. These components are particularly important for understanding the evolution of the nebula. Methods. We performed Herschel/HIFI observations of several CO lines in the far-infrared/sub-mm in the protoplanetary nebula CRL 618. The high spectral resolution provided by HIFI allows measurement of the line profiles. Since the dynamics and structure of the nebula is well known from mm-wave interferometric maps, it is possible to identify the contributions of the different nebular components (fast bipolar outflows, double shells, compact slow shell) to the line profiles. The observation of these relatively high-energy transitions allows an accurate study of the excitation conditions in these components, particularly in the warm ones, which cannot be properly studied from the low-energy lines. Results. The (CO)-C-12 J = 16-15, 10-9, and 6-5 lines are easily detected in this source. Both (CO)-C-13 J = 10-9 and 6-5 are also detected. Wide profiles showing spectacular line wings have been found, particularly in (CO)-C-12 J = 16-15. Other lines observed simultaneously with CO are also shown. Our analysis of the CO high-J transitions, when compared with the existing models, confirms the very low expansion velocity of the central, dense component, which probably indicates that the shells ejected during the last AGB phases were driven by radiation pressure under a regime of maximum transfer of momentum. No contribution of the diffuse halo found from mm-wave data is identified in our spectra, because of its low temperature. We find that the fast bipolar outflow is quite hot, much hotter than previously estimated; for instance, gas flowing at 100 km s(-1) must have a temperature higher than similar to 200 K. Probably, this very fast outflow, with a kinematic age < 100 yr, has been accelerated by a shock and has not yet cooled down. The double empty shell found from mm-wave mapping must also be relatively hot, in agreement with the previous estimate. C1 [Bujarrabal, V.; Planesas, P.] Observ Astron Nacl IGN, Alcala De Henares 28803, Spain. [Alcolea, J.; Soria-Ruiz, R.] Observ Astron Nacl IGN, Madrid 28014, Spain. [Cernicharo, J.] CSIC, INTA, CAB, Madrid 28850, Spain. [Decin, L.; Waters, L. B. F. M.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Heverlee, Belgium. [Decin, L.; Dominik, C.; de Koter, A.; Waters, L. B. F. M.] Univ Amsterdam, Sterrenkundig Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. [Justtanont, K.; Olofsson, H.; Schoier, F. L.] Chalmers, Dept Radio & Space Sci, Onsala Space Observ, S-43992 Onsala, Sweden. [Teyssier, D.; Marston, A. P.] ESA, European Space Astron Ctr, Madrid, Spain. [Melnick, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Menten, K. M.; Guesten, R.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Neufeld, D. A.] Johns Hopkins Univ, Baltimore, MD 21218 USA. [Olofsson, H.] Stockholm Univ, Dept Astron, AlbaNova Univ Ctr, S-10691 Stockholm, Sweden. [Planesas, P.] Joint ALMA Observ, Santiago, Chile. [Schmidt, M.; Szczerba, R.] Nicholas Copernicus Astron Ctr, PL-87100 Torun, Poland. [Dominik, C.] Radboud Univ Nijmegen, Dept Astrophys, IMAPP, NL-6525 ED Nijmegen, Netherlands. [de Koter, A.] Univ Utrecht, Astron Inst, NL-3584 CC Utrecht, Netherlands. [Quintana-Lacaci, G.] IRAM, E-18012 Granada, Spain. [Gallego, J. D.; Diez-Gonzalez, M. C.; Barcia, A.; Lopez-Fernandez, I.] Ctr Astron Yebes, Observ Astron Nacl IGN, E-19080 Guadalajara, Spain. [Wildeman, K.] Univ Groningen, SRON Netherlands Inst Space Res, NL-9747 AD Groningen, Netherlands. [Tielens, A. G. G. M.] Leiden Univ, NL-2300 RA Leiden, Netherlands. [Jacobs, K.] Univ Cologne, KOSMA, Inst Phys 1, D-50937 Cologne, Germany. RP Bujarrabal, V (reprint author), Observ Astron Nacl IGN, Ap 112, Alcala De Henares 28803, Spain. EM v.bujarrabal@oan.es RI Planesas, Pere/G-7950-2015; OI Planesas, Pere/0000-0002-7808-3040; /0000-0003-1689-9201; Quintana-Lacaci, Guillermo/0000-0002-5417-1943 FU Spanish MICINN [CSD2009-00038]; Polish MNiSW [N 203 393334]; SNSB; MICINN [AYA2009-07304]; National Aeronautics and Space Administration 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; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astronomico Nacional (IGN), Centro de Astrobiologia (CSIC-INTA). Sweden: Chalmers University of Technology - MC2, RSS & GARD; Onsala Space Observatory; Swedish National Space Board, Stockholm University - Stockholm Observatory; Switzerland: ETH Zurich, FHNW; USA: Caltech, J.P.L., NHSC. HCSS / HSpot / HIPE is a joint development (are joint developments) by the Herschel Science Ground Segment Consortium, consisting of ESA, the NASA Herschel Science Center, and the HIFI, PACS, and SPIRE consortia. This work has been partially supported by the Spanish MICINN, program CONSOLIDER INGENIO 2010, grant "ASTROMOL" (CSD2009-00038). R.Sz. and M.Sch. acknowledge support from grant N 203 393334 from the Polish MNiSW. K.J. acknowledges the funding from SNSB. J.C. acknowledges funding from MICINN, grant AYA2009-07304. This research was performed, in part, through a JPL contract funded by the National Aeronautics and Space Administration. NR 16 TC 21 Z9 21 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR L3 DI 10.1051/0004-6361/201015068 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900003 ER PT J AU Caselli, P Keto, E Pagani, L Aikawa, Y Yildiz, UA van der Tak, FFS Tafalla, M Bergin, EA Nisini, B Codella, C van Dishoeck, EF Bachiller, R Baudry, A Benedettini, M Benz, AO Bjerkeli, P Blake, GA Bontemps, S Braine, J Bruderer, S Cernicharo, J Daniel, F di Giorgio, AM Dominik, C Doty, SD Encrenaz, P Fich, M Fuente, A Gaier, T Giannini, T Goicoechea, JR de Graauw, T Helmich, F Herczeg, GJ Herpin, F Hogerheijde, MR Jackson, B Jacq, T Javadi, H Johnstone, D Jorgensen, JK Kester, D Kristensen, LE Laauwen, W Larsson, B Lis, D Liseau, R Luinge, W Marseille, M McCoey, C Megej, A Melnick, G Neufeld, D Olberg, M Parise, B Pearson, JC Plume, R Risacher, C Santiago-Garcia, J Saraceno, P Shipman, R Siegel, P van Kempen, TA Visser, R Wampfler, SF Wyrowski, F AF Caselli, P. Keto, E. Pagani, L. Aikawa, Y. Yildiz, U. A. van der Tak, F. F. S. Tafalla, M. Bergin, E. A. Nisini, B. Codella, C. van Dishoeck, E. F. Bachiller, R. Baudry, A. Benedettini, M. Benz, A. O. Bjerkeli, P. Blake, G. A. Bontemps, S. Braine, J. Bruderer, S. Cernicharo, J. Daniel, F. di Giorgio, A. M. Dominik, C. Doty, S. D. Encrenaz, P. Fich, M. Fuente, A. Gaier, T. Giannini, T. Goicoechea, J. R. de Graauw, Th. Helmich, F. Herczeg, G. J. Herpin, F. Hogerheijde, M. R. Jackson, B. Jacq, T. Javadi, H. Johnstone, D. Jorgensen, J. K. Kester, D. Kristensen, L. E. Laauwen, W. Larsson, B. Lis, D. Liseau, R. Luinge, W. Marseille, M. McCoey, C. Megej, A. Melnick, G. Neufeld, D. Olberg, M. Parise, B. Pearson, J. C. Plume, R. Risacher, C. Santiago-Garcia, J. Saraceno, P. Shipman, R. Siegel, P. van Kempen, T. A. Visser, R. Wampfler, S. F. Wyrowski, F. TI Water vapor toward starless cores: The Herschel view SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE astrochemistry; line: formation; molecular processes; radiative transfer; stars: formation; ISM: clouds ID DENSE INTERSTELLAR CLOUDS; PRE-STELLAR CORES; MOLECULAR-IONS; INITIAL CONDITIONS; PRESTELLAR CORES; ABUNDANCE; L1544; TEMPERATURE; DEPLETION; OXYGEN AB Aims. Previous studies by the satellites SWAS and Odin provided stringent upper limits on the gas phase water abundance of dark clouds (x(H2O) < 7 x 10(-9)). We investigate the chemistry of water vapor in starless cores beyond the previous upper limits using the highly improved angular resolution and sensitivity of Herschel and measure the abundance of water vapor during evolutionary stages just preceding star formation. Methods. High spectral resolution observations of the fundamental ortho water (o-H2O) transition (557 GHz) were carried out with the Heterodyne Instrument for the Far Infrared onboard Herschel toward two starless cores: Barnard 68 (hereafter B68), a Bok globule, and LDN 1544 (L1544), a prestellar core embedded in the Taurus molecular cloud complex. Detailed radiative transfer and chemical codes were used to analyze the data. Results. The RMS in the brightness temperature measured for the B68 and L1544 spectra is 2.0 and 2.2 mK, respectively, in a velocity bin of 0.59 km s(-1). The continuum level is 3.5 +/- 0.2 mK in B68 and 11.4 +/- 0.4 mK in L1544. No significant feature is detected in B68 and the 3 sigma upper limit is consistent with a column density of o-H2O N(o-H2O) < 2.5 x 10(13) cm(-2), or a fractional abundance x(o-H2O) < 1.3 x 10(-9), more than an order of magnitude lower than the SWAS upper limit on this source. The L1544 spectrum shows an absorption feature at a 5 sigma level from which we obtain the first value of the o-H2O column density ever measured in dark clouds: N(o-H2O) = (8 +/- 4) x 10(12) cm(-2). The corresponding fractional abundance is x(o-H2O) similar or equal to 5 x 10(-9) at radii > 7000 AU and similar or equal to 2 x 10(-10) toward the center. The radiative transfer analysis shows that this is consistent with a x(o-H2O) profile peaking at similar or equal to 10(-8), 0.1 pc away from the core center, where both freeze-out and photodissociation are negligible. Conclusions. Herschel has provided the first measurement of water vapor in dark regions. Column densities of o-H2O are low, but prestellar cores such as L1544 (with their high central densities, strong continuum, and large envelopes) appear to be very promising tools to finally shed light on the solid/vapor balance of water in molecular clouds and oxygen chemistry in the earliest stages of star formation. C1 [Caselli, P.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Caselli, P.; Codella, C.; Jacq, T.] Ist Nazl Fis Nucl, Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Keto, E.; Melnick, G.; van Kempen, T. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Pagani, L.; Encrenaz, P.] Observ Paris, LERMA, F-75014 Paris, France. [Pagani, L.; Encrenaz, P.] Observ Paris, CNRS, UMR 8112, F-75014 Paris, France. [Aikawa, Y.] Kobe Univ, Dept Earth & Planetary Sci, Nada Ku, Kobe, Hyogo 6578501, Japan. [Yildiz, U. A.; van Dishoeck, E. F.; Hogerheijde, M. R.; Kristensen, L. E.; Visser, R.] Leiden Univ, Leiden Observ, Leiden, Netherlands. [van der Tak, F. F. S.; de Graauw, Th.; Helmich, F.; Jackson, B.; Kester, D.; Laauwen, W.; Luinge, W.; Marseille, M.; Risacher, C.; Shipman, R.] SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [van der Tak, F. F. S.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Tafalla, M.; Bachiller, R.] Observ Astron Nacl IGN, Madrid 28014, Spain. [Bergin, E. A.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Nisini, B.; Giannini, T.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy. [van Dishoeck, E. F.; Herczeg, G. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Benz, A. O.; Bruderer, S.; Wampfler, S. F.] ETH, Inst Astron, CH-8093 Zurich, Switzerland. [Baudry, A.; Bontemps, S.; Braine, J.; Herpin, F.] Univ Bordeaux, Lab Astrophys Bordeaux, Bordeaux, France. [Baudry, A.; Bontemps, S.; Braine, J.; Herpin, F.] CNRS INSU, UMR 5804, F-33271 Floirac, France. [Johnstone, D.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Johnstone, D.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 1A1, Canada. [Bjerkeli, P.; Liseau, R.; Olberg, M.] Chalmers, Dept Radio & Space Sci, Onsala Space Observ, S-43992 Onsala, Sweden. [Benedettini, M.; di Giorgio, A. M.; Saraceno, P.] INAF Ist Fis Spazio Interplanetario, Area Ric Tor Vergata, I-00133 Rome, Italy. [Blake, G. A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Cernicharo, J.; Daniel, F.; Goicoechea, J. R.] CSIC INTA, Ctr Astrobiol, Dept Astrofis, Madrid 28850, Spain. [Dominik, C.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. [Dominik, C.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands. [Doty, S. D.] Denison Univ, Dept Phys & Astron, Granville, OH 43023 USA. [Fich, M.; McCoey, C.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [Fuente, A.] Observ Astron Nacl, Alcala De Henares 28803, Spain. [Gaier, T.; Javadi, H.; Pearson, J. C.; Siegel, P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Jorgensen, J. K.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen K, Denmark. [Larsson, B.] Stockholm Univ, Dept Astron, S-10691 Stockholm, Sweden. [Lis, D.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [McCoey, C.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [Neufeld, D.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Parise, B.; Wyrowski, F.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Plume, R.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Santiago-Garcia, J.] Inst Radioastron Milimetr IRAM, Granada 18012, Spain. [Megej, A.] ETH, Microwave Lab, CH-8092 Zurich, Switzerland. RP Caselli, P (reprint author), Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. EM p.caselli@leeds.ac.uk RI Yildiz, Umut/C-5257-2011; Kristensen, Lars/F-4774-2011; Visser, Ruud/J-8574-2012; Jorgensen, Jes Kristian/L-7936-2014; Wampfler, Susanne/D-2270-2015; Fuente, Asuncion/G-1468-2016; OI Giannini, Teresa/0000-0002-0224-096X; Yildiz, Umut/0000-0001-6197-2864; Kristensen, Lars/0000-0003-1159-3721; Jorgensen, Jes Kristian/0000-0001-9133-8047; Wampfler, Susanne/0000-0002-3151-7657; Fuente, Asuncion/0000-0001-6317-6343; Bjerkeli, Per/0000-0002-7993-4118; Codella, Claudio/0000-0003-1514-3074; , Brunella Nisini/0000-0002-9190-0113 NR 39 TC 28 Z9 28 U1 1 U2 7 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR L29 DI 10.1051/0004-6361/201015097 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900029 ER PT J AU Ceccarelli, C Bacmann, A Boogert, A Caux, E Dominik, C Lefloch, B Lis, D Schilke, P van der Tak, F Caselli, P Cernicharo, J Codella, C Comito, C Fuente, A Baudry, A Bell, T Benedettini, M Bergin, EA Blake, GA Bottinelli, S Cabrit, S Castets, A Coutens, A Crimier, N Demyk, K Encrenaz, P Falgarone, E Gerin, M Goldsmith, PF Helmich, F Hennebelle, P Henning, T Herbst, E Hily-Blant, P Jacq, T Kahane, C Kama, M Klotz, A Langer, W Lord, S Lorenzani, A Maret, S Melnick, G Neufeld, D Nisini, B Pacheco, S Pagani, L Parise, B Pearson, J Phillips, T Salez, M Saraceno, P Schuster, K Tielens, X van der Wiel, MHD Vastel, C Viti, S Wakelam, V Walters, A Wyrowski, F Yorke, H Liseau, R Olberg, M Szczerba, R Benz, AO Melchior, M AF Ceccarelli, C. Bacmann, A. Boogert, A. Caux, E. Dominik, C. Lefloch, B. Lis, D. Schilke, P. van der Tak, F. Caselli, P. Cernicharo, J. Codella, C. Comito, C. Fuente, A. Baudry, A. Bell, T. Benedettini, M. Bergin, E. A. Blake, G. A. Bottinelli, S. Cabrit, S. Castets, A. Coutens, A. Crimier, N. Demyk, K. Encrenaz, P. Falgarone, E. Gerin, M. Goldsmith, P. F. Helmich, F. Hennebelle, P. Henning, T. Herbst, E. Hily-Blant, P. Jacq, T. Kahane, C. Kama, M. Klotz, A. Langer, W. Lord, S. Lorenzani, A. Maret, S. Melnick, G. Neufeld, D. Nisini, B. Pacheco, S. Pagani, L. Parise, B. Pearson, J. Phillips, T. Salez, M. Saraceno, P. Schuster, K. Tielens, X. van der Wiel, M. H. D. Vastel, C. Viti, S. Wakelam, V. Walters, A. Wyrowski, F. Yorke, H. Liseau, R. Olberg, M. Szczerba, R. Benz, A. O. Melchior, M. TI Herschel spectral surveys of star- forming regions Overview of the 555-636 GHz range SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE astrochemistry; stars: formation ID NGC 6334 I; PROTOSTELLAR SHOCK L1157-B1; MASSIVE YOUNG STARS; DEUTERATED FORMALDEHYDE; HOT CORE; SUBMILLIMETER; MILLIMETER; PROTOSTARS; WATER; I(N) AB High resolution line spectra of star-forming regions are mines of information: they provide unique clues to reconstruct the chemical, dynamical, and physical structure of the observed source. We present the first results from the Herschel key project " Chemical HErschel Surveys of Star forming regions", CHESS. We report and discuss observations towards five CHESS targets, one outflow shock spot and four protostars with luminosities bewteen 20 and 2 x 105 L similar to : L1157-B1, IRAS 16293-2422, OMC2-FIR4, AFGL 2591, and NGC 6334I. The observations were obtained with the heterodyne spectrometer HIFI on board Herschel, with a spectral resolution of 1 MHz. They cover the frequency range 555-636 GHz, a range largely unexplored before the launch of the Herschel satellite. A comparison of the five spectra highlights spectacular differences in the five sources, for example in the density of methanol lines, or the presence./absence of lines from S-bearing molecules or deuterated species. We discuss how these differences can be attributed to the different star-forming mass or evolutionary status. C1 [Ceccarelli, C.; Bacmann, A.; Lefloch, B.; Castets, A.; Crimier, N.; Hily-Blant, P.; Kahane, C.; Maret, S.; Pacheco, S.] Univ Grenoble 1, CNRS, UMR 5571, Lab Astrophys Grenoble, Grenoble, France. [Ceccarelli, C.; Bacmann, A.; Baudry, A.; Castets, A.; Jacq, T.; Wakelam, V.] Univ Bordeaux, Lab Astrophys Bordeaux, Floirac, France. [Ceccarelli, C.; Bacmann, A.; Baudry, A.; Castets, A.; Jacq, T.; Wakelam, V.] CNRS INSU, UMR 5804, Floirac, France. [Boogert, A.; Lord, S.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Caux, E.; Bottinelli, S.; Coutens, A.; Demyk, K.; Klotz, A.; Vastel, C.; Walters, A.] Univ Toulouse 3, Ctr Etud Spatiale Rayonnements, F-31062 Toulouse, France. [Caux, E.; Bottinelli, S.; Coutens, A.; Demyk, K.; Klotz, A.; Vastel, C.; Walters, A.] CNRS INSU, UMR 5187, Toulouse, France. [Dominik, C.; Kama, M.] Univ Amsterdam, Astron Inst Anton Pannekoek, Amsterdam, Netherlands. [Dominik, C.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6525 ED Nijmegen, Netherlands. [Schilke, P.; Comito, C.; Parise, B.; Wyrowski, F.] Max Planck Inst Radioastron, D-5300 Bonn, Germany. [Schilke, P.] Univ Cologne, Inst Phys 1, D-5000 Cologne, Germany. [van der Tak, F.; Helmich, F.; van der Wiel, M. H. D.; Olberg, M.] SRON Netherlands Inst Space Res, Groningen, Netherlands. [van der Tak, F.; van der Wiel, M. H. D.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AB Groningen, Netherlands. [Caselli, P.; Benedettini, M.; Saraceno, P.] INAF Ist Fis Spazio Interplanetario, Rome, Italy. [Caselli, P.] Univ Leeds, Sch Phys & Astron, Leeds, W Yorkshire, England. [Cernicharo, J.; Crimier, N.] CSIC INTA, Ctr Astrobiol, Madrid, Spain. [Codella, C.; Lorenzani, A.] INAF Osservatorio Astrofis Arcetri, Florence, Italy. [Fuente, A.] IGN Observ Astron Nacl, Alcala De Henares, Spain. [Bergin, E. A.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Cabrit, S.; Encrenaz, P.; Falgarone, E.; Gerin, M.; Hennebelle, P.; Pagani, L.; Salez, M.] UCP, UPMC, Lab Etud Rayonnement & Mat Astrophys, UMR 8112,CNRS INSU,OP,ENS, Paris, France. [Goldsmith, P. F.; Langer, W.; Pearson, J.; Yorke, H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Henning, T.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Herbst, E.] Ohio State Univ, Columbus, OH 43210 USA. [Melnick, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Neufeld, D.] Johns Hopkins Univ, Baltimore, MD USA. [Nisini, B.] INAF Osservatorio Astronom Roma, Monte Porzio Catone, Italy. [Schuster, K.] Inst RadioAstron Millimetr, Grenoble, France. [Tielens, X.] Leiden Univ, Leiden Observ, Leiden, Netherlands. [Viti, S.] UCL, Dept Phys & Astron, London, England. [Liseau, R.; Olberg, M.] Stockholm Univ, Dept Astron, Chalmers Univ Technol, S-10691 Stockholm, Sweden. [Szczerba, R.] Nicholas Copernicus Astron Ctr, Torun, Poland. [Benz, A. O.] ETH, Inst Astron, CH-8093 Zurich, Switzerland. RP Ceccarelli, C (reprint author), Univ Grenoble 1, CNRS, UMR 5571, Lab Astrophys Grenoble, Grenoble, France. EM cecilia.ceccarelli@obs.ujf-grenoble.fr RI van der Wiel, Matthijs/M-4531-2014; Coutens, Audrey/M-4533-2014; Fuente, Asuncion/G-1468-2016; Goldsmith, Paul/H-3159-2016; OI Maret, Sebastien/0000-0003-1104-4554; van der Wiel, Matthijs/0000-0002-4325-3011; Coutens, Audrey/0000-0003-1805-3920; Fuente, Asuncion/0000-0001-6317-6343; Lorenzani, Andrea/0000-0002-4685-3434; Wakelam, Valentine/0000-0001-9676-2605; Kama, Mihkel/0000-0003-0065-7267; Codella, Claudio/0000-0003-1514-3074; , Brunella Nisini/0000-0002-9190-0113 FU Swedish National Space Board, Stockholm University -Stockholm Observatory 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 abd the US. Consortium members are: Canada: CSA, U. Waterloo; France: CESR, LAB, LERMA, IRAM; Germany: KOSMA, MPIfR, MPS; Ireland, NUI Maynooth; Italy: ASI, IFSI-INAF, Osservatorio Astrofisico di Arcetri-INAF; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astronomico Nacional (IGN), Centro de Astrobiolog a (CSIC-INTA). Sweden: Chalmers University of Technology -MC2, RSS & GARD; Onsala Space Observatory; Swedish National Space Board, Stockholm University -Stockholm Observatory; Switzerland: ETH Zurich, FHNW; USA: Caltech, JPL, NHSC. We thank many funding agencies for financial NR 34 TC 63 Z9 63 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 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR L22 DI 10.1051/0004-6361/201015081 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900022 ER PT J AU Chavarria, L Herpin, F Jacq, T Braine, J Bontemps, S Baudry, A Marseille, M van der Tak, F Pietropaoli, B Wyrowski, F Shipman, R Frieswijk, W van Dishoeck, EF Cernicharo, J Bachiller, R Benedettini, M Benz, AO Bergin, E Bjerkeli, P Blake, GA Bruderer, S Caselli, P Codella, C Daniel, F di Giorgio, AM Dominik, C Doty, SD Encrenaz, P Fich, M Fuente, A Giannini, T Goicoechea, JR de Graauw, T Hartogh, P Helmich, F Herczeg, GJ Hogerheijde, MR Johnstone, D Jorgensen, JK Kristensen, LE Larsson, B Lis, D Liseau, R McCoey, C Melnick, G Nisini, B Olberg, M Parise, B Pearson, JC Plume, R Risacher, C Santiago-Garcia, J Saraceno, P Stutzki, J Szczerba, R Tafalla, M Tielens, A van Kempen, TA Visser, R Wampfler, SF Willem, J Yildiz, UA AF Chavarria, L. Herpin, F. Jacq, T. Braine, J. Bontemps, S. Baudry, A. Marseille, M. van der Tak, F. Pietropaoli, B. Wyrowski, F. Shipman, R. Frieswijk, W. van Dishoeck, E. F. Cernicharo, J. Bachiller, R. Benedettini, M. Benz, A. O. Bergin, E. Bjerkeli, P. Blake, G. A. Bruderer, S. Caselli, P. Codella, C. Daniel, F. di Giorgio, A. M. Dominik, C. Doty, S. D. Encrenaz, P. Fich, M. Fuente, A. Giannini, T. Goicoechea, J. R. de Graauw, Th. Hartogh, P. Helmich, F. Herczeg, G. J. Hogerheijde, M. R. Johnstone, D. Jorgensen, J. K. Kristensen, L. E. Larsson, B. Lis, D. Liseau, R. McCoey, C. Melnick, G. Nisini, B. Olberg, M. Parise, B. Pearson, J. C. Plume, R. Risacher, C. Santiago-Garcia, J. Saraceno, P. Stutzki, J. Szczerba, R. Tafalla, M. Tielens, A. van Kempen, T. A. Visser, R. Wampfler, S. F. Willem, J. Yildiz, U. A. TI Water in massive star-forming regions: HIFI observations of W3 IRS5 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: formation; stars: massive; ISM: molecules; ISM: abundances; dust, extinction; radio lines: ISM ID RADIATIVE-TRANSFER; ABUNDANCES; ENVELOPES; RATIOS; SPECTROSCOPY; PROTOSTARS; TRAPEZIUM; CONTINUUM; TRACERS; MODELS AB We present Herschel observations of the water molecule in the massive star-forming region W3 IRS5. The o-(H2O)-O-17 1(10)-1(01), p-(H2O)-O-18 1(11)-0(00), p-H2O 2(02)-1(11), p-H2O 1(11)-0(00), o-H2O 2(21)-2(12), and o-H2O 2(12)-1(01) lines, covering a frequency range from 552 up to 1669 GHz, have been detected at high spectral resolution with HIFI. The water lines in W3 IRS5 show well-defined high-velocity wings that indicate a clear contribution by outflows. Moreover, the systematically blue-shifted absorption in the H2O lines suggests expansion, presumably driven by the outflow. No infall signatures are detected. The p-H2O 1(11)-0(00) and o-H2O 2(12)-1(01) lines show absorption from the cold material (T similar to 10 K) in which the high-mass protostellar envelope is embedded. One-dimensional radiative transfer models are used to estimate water abundances and to further study the kinematics of the region. We show that the emission in the rare isotopologues comes directly from the inner parts of the envelope (T greater than or similar to 100 K) where water ices in the dust mantles evaporate and the gas-phase abundance increases. The resulting jump in the water abundance (with a constant inner abundance of 10(-4)) is needed to reproduce the o-(H2O)-O-17 1(10)-1(01) and p-(H2O)-O-18 1(11)-0(00) spectra in our models. We estimate water abundances of 10(-8) to 10(-9) in the outer parts of the envelope (T less than or similar to 100 K). The possibility of two protostellar objects contributing to the emission is discussed. C1 [Chavarria, L.; Herpin, F.; Jacq, T.; Braine, J.; Bontemps, S.; Baudry, A.; Pietropaoli, B.] Univ Bordeaux, Lab Astrophys Bordeaux, Bordeaux, France. [Chavarria, L.; Herpin, F.; Jacq, T.; Braine, J.; Bontemps, S.; Baudry, A.; Pietropaoli, B.] CNRS INSU, UMR 5804, Floirac, France. [Marseille, M.; van der Tak, F.; Shipman, R.; Frieswijk, W.; de Graauw, Th.; Helmich, F.; Willem, J.] SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [van der Tak, F.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Pietropaoli, B.] Ecole Mines, F-44300 Nantes, France. [Wyrowski, F.; Parise, B.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [van Dishoeck, E. F.; Hogerheijde, M. R.; Kristensen, L. E.; Tielens, A.; Visser, R.; Yildiz, U. A.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [van Dishoeck, E. F.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Cernicharo, J.; Daniel, F.; Goicoechea, J. R.] CSIC INTA, Dept Astrofis, Ctr Astrobiol, Madrid 28850, Spain. [Bachiller, R.; Tafalla, M.] Observ Astron Nacl IGN, Madrid 28014, Spain. [Benedettini, M.; di Giorgio, A. M.; Saraceno, P.] INAF Ist Fis Spazio Interplanetario, Area Ric Tor Vergata, I-00133 Rome, Italy. [Benz, A. O.; Bruderer, S.; Wampfler, S. F.] ETH, Inst Astron, CH-8093 Zurich, Switzerland. [Bergin, E.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Bjerkeli, P.; Liseau, R.; Olberg, M.] Chalmers, Onsala Space Observ, Dept Radio & Space Sci, S-43992 Onsala, Sweden. [Blake, G. A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Caselli, P.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Caselli, P.; Codella, C.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Dominik, C.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. [Dominik, C.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands. [Doty, S. D.] Denison Univ, Dept Phys & Astron, Granville, OH 43023 USA. [Encrenaz, P.] Observ Paris, LERMA, F-75014 Paris, France. [Encrenaz, P.] Observ Paris, CNRS, UMR 8112, F-75014 Paris, France. [Fich, M.; McCoey, C.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [Fuente, A.] Observ Astron Nacl, Alcala De Henares 28803, Spain. [Giannini, T.; Nisini, B.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy. [Hartogh, P.] MPI Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. [Johnstone, D.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Johnstone, D.] Univ Victoria, Dept Phys & Astron, Victoria, BC V9E 2E7, Canada. [Jorgensen, J. K.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen K, Denmark. [Larsson, B.] Stockholm Univ, Dept Astron, S-10691 Stockholm, Sweden. [Lis, D.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [McCoey, C.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [Melnick, G.; van Kempen, T. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Pearson, J. C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Plume, R.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Santiago-Garcia, J.] IRAM, E-18012 Granada, Spain. [Stutzki, J.] Univ Cologne, Inst Phys 1, KOSMA, D-50937 Cologne, Germany. [Szczerba, R.] Nicholas Copernicus Astron Ctr, PL-87100 Torun, Poland. RP Chavarria, L (reprint author), Univ Bordeaux, Lab Astrophys Bordeaux, Bordeaux, France. EM luisagustinchavarria@gmail.com RI Yildiz, Umut/C-5257-2011; Kristensen, Lars/F-4774-2011; Visser, Ruud/J-8574-2012; Wampfler, Susanne/D-2270-2015; Fuente, Asuncion/G-1468-2016; OI Yildiz, Umut/0000-0001-6197-2864; Kristensen, Lars/0000-0003-1159-3721; Wampfler, Susanne/0000-0002-3151-7657; Fuente, Asuncion/0000-0001-6317-6343; Bjerkeli, Per/0000-0002-7993-4118; Codella, Claudio/0000-0003-1514-3074; Giannini, Teresa/0000-0002-0224-096X; , Brunella Nisini/0000-0002-9190-0113 FU French Space Agency CNES 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; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astronomico Nacional (IGN), Centro de Astrobiologia (CSIC-INTA). Sweden: Chalmers University of Technology - MC2, RSS & GARD; Onsala Space Observatory; Swedish National Space Board, Stockholm University - Stockholm Observatory; Switzerland: ETH Zurich, FHNW; USA: Caltech, JPL, NHSC. HIPE is a joint development by the Herschel Science Ground Segment Consortium, consisting of ESA, the NASA Herschel Science Center, and the HIFI, PACS and SPIRE consortia. We also thank the French Space Agency CNES for financial support. NR 31 TC 36 Z9 36 U1 1 U2 4 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR L37 DI 10.1051/0004-6361/201015113 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900037 ER PT J AU Comito, C Schilke, P Rolffs, R Lis, DC Belloche, A Bergin, EA Phillips, TG Bell, TA Crockett, NR Wang, S Blake, GA Caux, E Ceccarelli, C Cernicharo, J Daniel, F Dubernet, ML Emprechtinger, M Encrenaz, P Gerin, M Giesen, TF Goicoechea, JR Goldsmith, PF Gupta, H Herbst, E Joblin, C Johnstone, D Langer, WD Latter, WD Lord, SD Maret, S Martin, PG Melnick, GJ Menten, KM Morris, P Muller, HSP Murphy, JA Neufeld, DA Ossenkopf, V Pearson, JC Perault, M Plume, R Qin, SL Schlemmer, S Stutzki, J Trappe, N van der Tak, FFS Vastel, C Yorke, HW Yu, S Olberg, M Szczerba, R Larsson, B Liseau, R Lin, RH Samoska, LA Schlecht, E AF Comito, C. Schilke, P. Rolffs, R. Lis, D. C. Belloche, A. Bergin, E. A. Phillips, T. G. Bell, T. A. Crockett, N. R. Wang, S. Blake, G. A. Caux, E. Ceccarelli, C. Cernicharo, J. Daniel, F. Dubernet, M. -L. Emprechtinger, M. Encrenaz, P. Gerin, M. Giesen, T. F. Goicoechea, J. R. Goldsmith, P. F. Gupta, H. Herbst, E. Joblin, C. Johnstone, D. Langer, W. D. Latter, W. D. Lord, S. D. Maret, S. Martin, P. G. Melnick, G. J. Menten, K. M. Morris, P. Mueller, H. S. P. Murphy, J. A. Neufeld, D. A. Ossenkopf, V. Pearson, J. C. Perault, M. Plume, R. Qin, S. -L. Schlemmer, S. Stutzki, J. Trappe, N. van der Tak, F. F. S. Vastel, C. Yorke, H. W. Yu, S. Olberg, M. Szczerba, R. Larsson, B. Liseau, R. Lin, R. H. Samoska, L. A. Schlecht, E. TI Herschel observations of deuterated water towards Sgr B2(M) SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: molecules; molecular processes; line: formation ID LINE OBSERVATIONS; HOT CORES; SAGITTARIUS-B2; SUBMILLIMETER; EXCITATION; ASTRONOMY; VAPOR; BAND AB Observations of HDO are an important complement for studies of water, because they give strong constraints on the formation processes - grain surfaces versus energetic process in the gas phase, e. g. in shocks. The HIFI observations of multiple transitions of HDO in Sgr B2(M) presented here allow the determination of the HDO abundance throughout the envelope, which has not been possible before with ground-based observations only. The abundance structure has been modeled with the spherical Monte Carlo radiative transfer code RATRAN, which also takes radiative pumping by continuum emission from dust into account. The modeling reveals that the abundance of HDO rises steeply with temperature from a low abundance (2.5 x 10(-11)) in the outer envelope at temperatures below 100 K through a medium abundance (1.5 x 10(-9)) in the inner envelope/outer core at temperatures between 100 and 200 K, and finally a high abundance (3.5 x 10(-9)) at temperatures above 200 K in the hot core. C1 [Comito, C.; Schilke, P.; Rolffs, R.; Belloche, A.; Menten, K. M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Schilke, P.; Rolffs, R.; Giesen, T. F.; Mueller, H. S. P.; Ossenkopf, V.; Qin, S. -L.; Schlemmer, S.; Stutzki, J.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Lis, D. C.; Phillips, T. G.; Bell, T. A.; Blake, G. A.; Emprechtinger, M.] CALTECH, Cahill Ctr Astron & Astrophys 301 17, Pasadena, CA 91125 USA. [Bergin, E. A.; Crockett, N. R.; Wang, S.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Caux, E.; Joblin, C.; Vastel, C.] Univ Toulouse UPS, Ctr Etud Spatiale Rayonnements, F-31062 Toulouse 9, France. [Caux, E.; Joblin, C.; Vastel, C.] CNRS INSU, UMR 5187, F-31028 Toulouse 4, France. [Ceccarelli, C.; Maret, S.] Observ Grenoble, Astrophys Lab, F-38041 Grenoble 9, France. [Cernicharo, J.; Daniel, F.; Goicoechea, J. R.] Ctr Astrobiol CSIC INTA, Lab Astrofis Mol, Madrid, Spain. [Daniel, F.; Encrenaz, P.; Gerin, M.; Perault, M.] Observ Paris, LERMA, CNRS UMR8112, F-75231 Paris 05, France. [Daniel, F.; Encrenaz, P.; Gerin, M.; Perault, M.] Ecole Normale Super, F-75231 Paris 05, France. [Dubernet, M. -L.] Univ Paris 06, LPMAA, UMR7092, Paris, France. [Dubernet, M. -L.] Observ Paris, LUTH, UMR8102, Meudon, France. [Goldsmith, P. F.; Gupta, H.; Langer, W. D.; Pearson, J. C.; Yorke, H. W.; Yu, S.; Lin, R. H.; Samoska, L. A.; Schlecht, E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Herbst, E.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Herbst, E.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Herbst, E.] Ohio State Univ, Dept Chem, Columbus, OH 43210 USA. [Johnstone, D.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Latter, W. D.; Lord, S. D.; Morris, P.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Martin, P. G.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Melnick, G. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Murphy, J. A.; Trappe, N.] Natl Univ Ireland Maynooth, Maynooth, Kildare, Ireland. [Neufeld, D. A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Ossenkopf, V.; van der Tak, F. F. S.] Univ Groningen, SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [Plume, R.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Olberg, M.; Liseau, R.] Chalmers, S-41296 Gothenburg, Sweden. [Szczerba, R.] Nicholas Copernicus Astron Ctr, PL-87100 Torun, Poland. [Larsson, B.] Stockholm Univ, Dept Astron, S-10691 Stockholm, Sweden. RP Comito, C (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. EM ccomito@mpifr.de RI Giesen, Thomas /B-9476-2015; Schlemmer, Stephan/E-2903-2015; Trappe, Neil/C-9014-2016; Yu, Shanshan/D-8733-2016; Goldsmith, Paul/H-3159-2016 OI Mueller, Holger/0000-0002-0183-8927; Maret, Sebastien/0000-0003-1104-4554; Giesen, Thomas /0000-0002-2401-0049; Schlemmer, Stephan/0000-0002-1421-7281; Trappe, Neil/0000-0003-2527-9821; FU NASA through JPL/Caltech; NSF [AST-0540882] 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; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astronifimico Nacional (IGN), Centro de Astrobiologia (CSIC-INTA). Sweden: Chalmers University of Technology - MC2, RSS & GARD; Onsala Space Observatory; Swedish National Space Board, Stockholm University - Stockholm Observatory; Switzerland: ETH Zurich, FHNW; USA: Caltech, JPL, NHSC. Support for this work was provided by NASA through an award issued by JPL/Caltech. CSO is supported by the NSF, award AST-0540882. NR 24 TC 7 Z9 7 U1 0 U2 4 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR L38 DI 10.1051/0004-6361/201015121 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900038 ER PT J AU Covino, S Campana, S Conciatore, ML D'Elia, V Palazzi, E Thone, CC Vergani, SD Wiersema, K Brusasca, M Cucchiara, A Cobb, BE Fernandez-Soto, A Kann, DA Malesani, D Tanvir, NR Antonelli, LA Bremer, M Castro-Tirado, AJ Postigo, AD Molinari, E Nicastro, L Stefanon, M Testa, V Tosti, G Vitali, F Amati, L Chapman, R Conconi, P Cutispoto, G Fynbo, JPU Goldoni, P Henriksen, C Horne, KD Malaspina, G Meurs, EJA Pian, E Stella, L Tagliaferri, G Ward, P Zerbi, FM AF Covino, S. Campana, S. Conciatore, M. L. D'Elia, V. Palazzi, E. Thoene, C. C. Vergani, S. D. Wiersema, K. Brusasca, M. Cucchiara, A. Cobb, B. E. Fernandez-Soto, A. Kann, D. A. Malesani, D. Tanvir, N. R. Antonelli, L. A. Bremer, M. Castro-Tirado, A. J. Postigo, A. de Ugarte Molinari, E. Nicastro, L. Stefanon, M. Testa, V. Tosti, G. Vitali, F. Amati, L. Chapman, R. Conconi, P. Cutispoto, G. Fynbo, J. P. U. Goldoni, P. Henriksen, C. Horne, K. D. Malaspina, G. Meurs, E. J. A. Pian, E. Stella, L. Tagliaferri, G. Ward, P. Zerbi, F. M. TI Challenging gamma-ray burst models through the broadband dataset of GRB060908 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE gamma-ray burst: individual: GRB 060908; gamma-ray burst: general; radiation mechanisms: non-thermal ID SWIFT XRT DATA; AFTERGLOW LIGHT CURVES; EARLY OPTICAL AFTERGLOWS; REVERSE SHOCK EMISSION; X-RAY; COMPREHENSIVE ANALYSIS; MULTIWAVELENGTH ANALYSIS; PARTICLE-ACCELERATION; RELATIVISTIC JETS; CANNONBALL MODEL AB Context. Multiwavelength observations of gamma-ray burst prompt and afterglow emission are a key tool to separate the various possible emission processes and scenarios proposed to interpret the complex gamma-ray burst phenomenology. Aims. We collected a large dataset on GRB060908 in order to carry out a comprehensive analysis of the prompt emission as well as the early and late afterglow. Methods. Data from Swift-BAT, -XRT and -UVOT together with data from a number of different ground-based optical/near-infrared and millimeter telescopes allowed us to follow the afterglow evolution after about a minute from the high-energy event down to the host galaxy limit. We discuss the physical parameters required to model these emissions. Results. The prompt emission of GRB060908 was characterised by two main periods of activity, spaced by a few seconds of low intensity, with a tight correlation between activity and spectral hardness. Observations of the afterglow began less than one minute after the high-energy event, when it was already in a decaying phase, and it was characterised by a rather flat optical/near-infrared spectrum which can be interpreted as due to a hard energy-distribution of the emitting electrons. On the other hand, the X-ray spectrum of the afterglow could be fit by a rather soft electron distribution. Conclusions. GRB060908 is a good example of a gamma-ray burst with a rich multi-wavelength set of observations. The availability of this dataset, built thanks to the joint efforts of many different teams, allowed us to carry out stringent tests for various interpretative scenarios, showing that a satisfactorily modelling of this event is challenging. In the future, similar efforts will enable us to obtain optical/near-infrared coverage comparable in quality and quantity to the X-ray data for more events, therefore opening new avenues to progress gamma-ray burst research. C1 [Covino, S.; Campana, S.; Thoene, C. C.; Brusasca, M.; Postigo, A. de Ugarte; Conconi, P.; Malaspina, G.; Tagliaferri, G.; Zerbi, F. M.] Osserv Astron Brera, INAF, I-23807 Merate, LC, Italy. [Campana, S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [D'Elia, V.; Antonelli, L. A.; Testa, V.; Vitali, F.; Stella, L.] Osserv Astron Roma, INAF, I-00040 Rome, Italy. [Palazzi, E.; Nicastro, L.; Amati, L.] Ist Astrofis Spaziale & Fis Cosm Bologna, INAF, I-40129 Bologna, Italy. [Vergani, S. D.; Goldoni, P.] APC, Lab Astroparticule & Cosmol, UMR 7164, F-75231 Paris 05, France. [Vergani, S. D.; Goldoni, P.] CEA Saclay, DSM, Serv Astrophys, DAPNIA, F-91191 Gif Sur Yvette, France. [Wiersema, K.; Tanvir, N. R.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Cucchiara, A.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Cobb, B. E.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Fernandez-Soto, A.] CSIC UC, Inst Fis Cantabria, Santander 39005, Spain. [Kann, D. A.] Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany. [Malesani, D.; Fynbo, J. P. U.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. [Bremer, M.] Inst Radio Astron Millimetr, F-38406 St Martin Dheres, France. [Castro-Tirado, A. J.] Inst Astrofis Andalucia, E-18080 Granada, Spain. [Molinari, E.] INAF TNG Fdn Galileo Galilei, Brena Baja 38712, TF, Spain. [Stefanon, M.] Univ Valencia, Astron Observ, Valencia 46980, Spain. [Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [Tosti, G.] Univ Perugia, Osservatorio Astron, I-06123 Perugia, Italy. [Chapman, R.] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Chapman, R.] Univ Iceland, Inst Sci, Ctr Astrophys & Cosmol, IS-107 Reykjavik, Iceland. [Cutispoto, G.] Catania Astrophys Observ, INAF, I-95123 Catania, Italy. [Horne, K. D.] Univ St Andrews, SUPA Phys & Astron, St Andrews KY 9SS, Fife, Scotland. [Meurs, E. J. A.; Ward, P.] Dunsink Observ, DIAS, Dublin 15, Ireland. [Pian, E.] Osserv Astron Trieste, INAF, I-34143 Trieste, Italy. [Pian, E.] Scuola Normale Super Pisa, I-56126 Pisa, Italy. RP Covino, S (reprint author), Osserv Astron Brera, INAF, Via Emilio Bianchi 46, I-23807 Merate, LC, Italy. EM stefano.covino@brera.inaf.it RI Tosti, Gino/E-9976-2013; Fynbo, Johan/L-8496-2014; Nicastro, Luciano/F-5866-2015; Palazzi, Eliana/N-4746-2015; Amati, Lorenzo/N-5586-2015; Stefanon, Mauro/F-8708-2016; Fernandez-Soto, Alberto/A-2443-2009; OI Zerbi, Filippo Maria/0000-0002-9996-973X; Campana, Sergio/0000-0001-6278-1576; Fynbo, Johan/0000-0002-8149-8298; Nicastro, Luciano/0000-0001-8534-6788; Amati, Lorenzo/0000-0001-5355-7388; Stefanon, Mauro/0000-0001-7768-5309; Fernandez-Soto, Alberto/0000-0002-5732-3121; Palazzi, Eliana/0000-0002-8691-7666; Molinari, Emilio/0000-0002-1742-7735; Testa, Vincenzo/0000-0003-1033-1340; Pian, Elena/0000-0001-8646-4858; Vitali, Fabrizio/0000-0001-8332-4227; D'Elia, Valerio/0000-0002-7320-5862; Castro-Tirado, A. J./0000-0003-2999-3563; Thone, Christina/0000-0002-7978-7648; de Ugarte Postigo, Antonio/0000-0001-7717-5085; Covino, Stefano/0000-0001-9078-5507; Tagliaferri, Gianpiero/0000-0003-0121-0723 FU NSF [AST 0707627]; Spanish MICINN [AYA2006-14056]; Generalitat Valenciana [2008/132] FX The SMARTS project is supported by NSF-AST 0707627. S.C. thanks Paolo D'Avanzo, Arnon Dar, Yizhong Fan, Dino Fugazza, Gabriele Ghisellini, Cristiano Guidorzi, Ruben Salvaterra and Zhiping Zin for many useful discussions. A.F.S. acknowledges support from the Spanish MICINN projects AYA2006-14056, Consolider-Ingenio 2007-32022, and from the Generalitat Valenciana project Prometeo 2008/132. We also acknowledge the use of data obtained with the Danish 1.5 m telescope as part of a program led by Jens Hjorth. NR 122 TC 17 Z9 18 U1 0 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR A53 DI 10.1051/0004-6361/201014994 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900114 ER PT J AU Crockett, NR Bergin, EA Wang, S Lis, DC Bell, TA Blake, GA Boogert, A Bumble, B Cabrit, S Caux, E Ceccarelli, C Cernicharo, J Daniel, F Daniel, F Dubernet, ML Emprechtinger, M Encrenaz, P Falgarone, E Gerin, M Giesen, TF Goicoechea, JR Goldsmith, PF Gupta, H Gusten, R Hartogh, P Helmich, F Herbst, E Honingh, N Joblin, C Johnstone, D Karpov, A Kawamura, JH Kooi, J Krieg, JM Langer, WD Latter, WD Lord, SD Maret, S Martin, PG Melnick, GJ Menten, KM Morris, P Muller, HSP Murphy, JA Neufeld, DA Ossenkopf, V Pearson, JC Perault, M Phillips, TG Plume, R Qin, SL Roelfsema, P Schieder, R Schilke, P Schlemmer, S Stutzki, J van der Tak, FFS Tielens, A Trappe, N Vastel, C Yorke, HW Yu, S Zmuidzinas, J AF Crockett, N. R. Bergin, E. A. Wang, S. Lis, D. C. Bell, T. A. Blake, G. A. Boogert, A. Bumble, B. Cabrit, S. Caux, E. Ceccarelli, C. Cernicharo, J. Daniel, F. Daniel, F. Dubernet, M. -L. Emprechtinger, M. Encrenaz, P. Falgarone, E. Gerin, M. Giesen, T. F. Goicoechea, J. R. Goldsmith, P. F. Gupta, H. Guesten, R. Hartogh, P. Helmich, F. Herbst, E. Honingh, N. Joblin, C. Johnstone, D. Karpov, A. Kawamura, J. H. Kooi, J. Krieg, J. -M. Langer, W. D. Latter, W. D. Lord, S. D. Maret, S. Martin, P. G. Melnick, G. J. Menten, K. M. Morris, P. Mueller, H. S. P. Murphy, J. A. Neufeld, D. A. Ossenkopf, V. Pearson, J. C. Perault, M. Phillips, T. G. Plume, R. Qin, S. -L. Roelfsema, P. Schieder, R. Schilke, P. Schlemmer, S. Stutzki, J. van der Tak, F. F. S. Tielens, A. Trappe, N. Vastel, C. Yorke, H. W. Yu, S. Zmuidzinas, J. TI Herschel observations of EXtra-Ordinary Sources (HEXOS): The Terahertz spectrum of Orion KL seen at high spectral resolution SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE astrochemistry; ISM: general; ISM: clouds; ISM: molecules; submillimeter: ISM ID MOLECULAR LINE SURVEY; APERTURE SYNTHESIS; COLOGNE DATABASE; SUBMILLIMETER; SPECTROSCOPY; MILLIMETER; NEBULA; CLOUDS; CDMS; HIFI AB We present the first high spectral resolution observations of Orion KL in the frequency ranges 1573.4-1702.8 GHz (band 6b) and 1788.4-1906.8 GHz (band 7b) obtained using the HIFI instrument on board the Herschel Space Observatory. We characterize the main emission lines found in the spectrum, which primarily arise from a range of components associated with Orion KL including the hot core, but also see widespread emission from components associated with molecular outflows traced by H2O, SO2, and OH. We find that the density of observed emission lines is significantly diminished in these bands compared to lower frequency Herschel/HIFI bands. C1 [Crockett, N. R.; Bergin, E. A.; Wang, S.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Lis, D. C.; Bell, T. A.; Blake, G. A.; Emprechtinger, M.; Karpov, A.; Kooi, J.; Phillips, T. G.; Zmuidzinas, J.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Neufeld, D. A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Caux, E.; Joblin, C.; Vastel, C.] Univ Toulouse UPS, Ctr Etud Spatiale Rayonnements, F-31062 Toulouse 9, France. [Caux, E.; Joblin, C.; Vastel, C.] CNRS INSU, UMR 5187, F-31028 Toulouse 4, France. [Ceccarelli, C.; Maret, S.] Lab Astrophys Observ Grenoble, F-38041 Grenoble 9, France. [Cernicharo, J.; Daniel, F.; Goicoechea, J. R.] Ctr Astrobiol CSIC INTA, Lab Astrofis Mol, Madrid 28850, Spain. [Daniel, F.; Guesten, R.; Menten, K. M.; Schilke, P.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Daniel, F.; Encrenaz, P.; Gerin, M.; Krieg, J. -M.; Perault, M.] Observ Paris, UMR8112, CNRS, LERMA, F-75231 Paris 05, France. [Daniel, F.; Encrenaz, P.; Gerin, M.; Krieg, J. -M.; Perault, M.] Ecole Normale Super, F-75231 Paris 05, France. [Dubernet, M. -L.] Univ Paris 06, LPMAA, UMR7092, Paris, France. [Dubernet, M. -L.] Observ Paris, UMR8102, LUTH, Meudon, France. [Giesen, T. F.; Honingh, N.; Mueller, H. S. P.; Ossenkopf, V.; Qin, S. -L.; Schieder, R.; Schilke, P.; Schlemmer, S.; Stutzki, J.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Bumble, B.; Goldsmith, P. F.; Gupta, H.; Kawamura, J. H.; Langer, W. D.; Pearson, J. C.; Yorke, H. W.; Yu, S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Herbst, E.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Herbst, E.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Herbst, E.] Ohio State Univ, Dept Chem, Columbus, OH 43210 USA. [Johnstone, D.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Boogert, A.; Latter, W. D.; Lord, S. D.; Morris, P.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Martin, P. G.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Melnick, G. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Murphy, J. A.; Trappe, N.] Natl Univ Ireland Maynooth, Maynooth, Kildare, Ireland. [Helmich, F.; Ossenkopf, V.; Roelfsema, P.] Univ Groningen, SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [Plume, R.; van der Tak, F. F. S.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Hartogh, P.] MPI Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. [Tielens, A.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Cabrit, S.] Observ Paris, CNRS, UMR8112, F-75014 Paris, France. [Cabrit, S.] LERMA, F-75014 Paris, France. [Falgarone, E.] Observ Paris, UMR8112, CNRS, LERMA, F-75231 Paris 05, France. [Falgarone, E.] Ecole Normale Super, F-75231 Paris 05, France. RP Crockett, NR (reprint author), Univ Michigan, Dept Astron, 500 Church St, Ann Arbor, MI 48109 USA. EM ncrocket@umich.edu RI Giesen, Thomas /B-9476-2015; Schlemmer, Stephan/E-2903-2015; Trappe, Neil/C-9014-2016; Yu, Shanshan/D-8733-2016; Goldsmith, Paul/H-3159-2016 OI Mueller, Holger/0000-0002-0183-8927; Giesen, Thomas /0000-0002-2401-0049; Schlemmer, Stephan/0000-0002-1421-7281; Maret, Sebastien/0000-0003-1104-4554; Trappe, Neil/0000-0003-2527-9821; FU NASA; NSF [AST0540882] 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; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astron mico Nacional (IGN), Centro de Astrobiolog a (CSIC-INTA). Sweden: Chalmers University of Technology -MC2, RSS & GARD; Onsala Space Observatory; Swedish National Space Board, Stockholm University -Stockholm Observatory; Switzerland: ETH Zurich, FHNW; USA: Caltech, JPL, NHSC. Support for this work was provided by NASA through an award issued by JPL/Caltech. CSO is supported by the NSF, award AST0540882. NR 20 TC 17 Z9 17 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR L21 DI 10.1051/0004-6361/201015116 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900021 ER PT J AU Decin, L Justtanont, K De Beck, E Lombaert, R de Koter, A Waters, LBFM Marston, AP Teyssier, D Schoier, FL Bujarrabal, V Alcolea, J Cernicharo, J Dominik, C Melnick, G Menten, K Neufeld, DA Olofsson, H Planesas, P Schmidt, M Szczerba, R de Graauw, T Helmich, F Roelfsema, P Dieleman, P Morris, P Gallego, JD Diez-Gonzalez, MC Caux, E AF Decin, L. Justtanont, K. De Beck, E. Lombaert, R. de Koter, A. Waters, L. B. F. M. Marston, A. P. Teyssier, D. Schoier, F. L. Bujarrabal, V. Alcolea, J. Cernicharo, J. Dominik, C. Melnick, G. Menten, K. Neufeld, D. A. Olofsson, H. Planesas, P. Schmidt, M. Szczerba, R. de Graauw, T. Helmich, F. Roelfsema, P. Dieleman, P. Morris, P. Gallego, J. D. Diez-Gonzalez, M. C. Caux, E. TI Water content and wind acceleration in the envelope around the oxygen-rich AGB star IK Tauri as seen by Herschel/HIFI SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE line: profiles; radiative transfer; instrumentation: spectrographs; stars: AGB and post-AGB; circumstellar matter; submillimeter: stars ID GIANT BRANCH STARS; MASS-LOSS HISTORY; CIRCUMSTELLAR ENVELOPES; EVOLVED STARS; ISOTOPIC ABUNDANCES; LINE EMISSION; CARBON STARS; W-HYA; CO; VAPOR AB During their asymptotic giant branch evolution, low-mass stars lose a significant fraction of their mass through an intense wind, enriching the interstellar medium with products of nucleosynthesis. We observed the nearby oxygen-rich asymptotic giant branch star IK Tau using the high-resolution HIFI spectrometer onboard Herschel. We report on the first detection of (H2O)-O-16 and the rarer isotopologues (H2O)-O-17 and (H2O)-O-18 in both the ortho and para states. We deduce a total water content (relative to molecular hydrogen) of 6.6 x 10(-5), and an ortho-to-para ratio of 3:1. These results are consistent with the formation of H2O in thermodynamical chemical equilibrium at photospheric temperatures, and does not require pulsationally induced non-equilibrium chemistry, vaporization of icy bodies or grain surface reactions. High-excitation lines of (CO)-C-12, (CO)-C-13, (SiO)-Si-28, (SiO)-Si-29, (SiO)-Si-30, HCN, and SO have also been detected. From the observed line widths, the acceleration region in the inner wind zone can be characterized, and we show that the wind acceleration is slower than hitherto anticipated. C1 [Decin, L.; De Beck, E.; Lombaert, R.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Heverlee, Belgium. [Decin, L.; de Koter, A.; Waters, L. B. F. M.; Dominik, C.] Univ Amsterdam, Sterrenkundig Inst Anton Pannekoek, NL-1098 Amsterdam, Netherlands. [Justtanont, K.] Chalmers, Onsala Space Observ, Dept Radio & Spece Sci, S-43992 Onsala, Sweden. [de Koter, A.] Univ Utrecht, Astron Inst, NL-3584 CC Utrecht, Netherlands. [Marston, A. P.; Teyssier, D.] ESA, European Space Astron Ctr, Madrid, Spain. [Bujarrabal, V.] Observ Astron Nacl, Alcala De Henares 28803, Spain. [Alcolea, J.] Observ Astron Nacl IGN, Madrid 28014, Spain. [Cernicharo, J.] INTA CSIC, CAB, Lab Mol Astrophys, Madrid 28850, Spain. [Melnick, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Menten, K.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Neufeld, D. A.] Johns Hopkins Univ, Baltimore, MD 21218 USA. [Olofsson, H.] Stockholm Univ, Dept Astron, AlbaNova Univ Ctr, S-10691 Stockholm, Sweden. [Schoier, F. L.; Olofsson, H.] Chalmers, Dept Radio & Space Sci, Onsala Space Observ, S-43992 Onsala, Sweden. [Planesas, P.] Joint ALMA Observ, Santiago, Chile. [Schmidt, M.; Szczerba, R.] Nicholas Copernicus Astron Ctr, PL-87100 Torun, Poland. [de Graauw, T.] Joint ALMA Off, Santiago, Chile. [Helmich, F.; Roelfsema, P.; Dieleman, P.] Univ Groningen, SRON Netherlands Inst Space Res, NL-9747 AD Groningen, Netherlands. [Morris, P.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Gallego, J. D.; Diez-Gonzalez, M. C.] Ctr Astron Yebes, Observ Astron Nacl IGN, E-19080 Guadalajara, Spain. [Caux, E.] Univ Toulouse UPS, Ctr Etud Spatiale Rayonnements, F-31062 Toulouse 9, France. [Caux, E.] CNRS INSU, UMR 5187, F-31028 Toulouse 4, France. [Dominik, C.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands. RP Decin, L (reprint author), Katholieke Univ Leuven, Inst Sterrenkunde, Celestijnenlaan 200D, B-3001 Heverlee, Belgium. EM Leen.Decin@ster.kuleuven.be; v.bujarrabal@oan.es RI Planesas, Pere/G-7950-2015; OI Planesas, Pere/0000-0002-7808-3040; De Beck, Elvire/0000-0002-7441-7189; /0000-0003-1689-9201 FU Flanders (FWO); Spanish MICINN [CSD2009-00038]; Polish MNiSW [N 203 393334]; MICINN [AYA2009-07304]; National Aeronautics and Space Administration 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; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astronomico Nacional (IGN), Centro de Astrobiologia (CSIC-INTA); Sweden: Chalmers University of Technology - MC2, RSS & GARD; Onsala Space Observatory; Swedish National Space Board, Stockholm University - Stockholm Observatory; Switzerland: ETH Zurich, FHNW; USA: Caltech, JPL, NHSC. HCSS / HSpot / HIPE is a joint development by the Herschel Science Ground Segment Consortium, consisting of ESA, the NASA Herschel Science Center, and the HIFI, PACS and SPIRE consortia. LD acknowledges financial support from the Fund for Scientific Research - Flanders (FWO). This work has been partially supported by the Spanish MICINN, program CONSOLIDER INGENIO 2010, grant ASTROMOL (CSD2009-00038). R.Sz. and M.Sch. acknowledge support from grant N 203 393334 from Polish MNiSW. J.C. thanks funding from MICINN, grant AYA2009-07304. This research was performed, in part, through a JPL contract funded by the National Aeronautics and Space Administration. NR 36 TC 31 Z9 31 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 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR L4 DI 10.1051/0004-6361/201015069 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900004 ER PT J AU Guarcello, MG Damiani, F Micela, G Peres, G Prisinzano, L Sciortino, S AF Guarcello, M. G. Damiani, F. Micela, G. Peres, G. Prisinzano, L. Sciortino, S. TI Pre-main sequence stars with disks in the Eagle Nebula observed in scattered light SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE accretion, accretion disks; scattering; protoplanetary disks; circumstellar matter; stars: pre-main sequence; Hertzsprung-Russell and C-M diagrams ID SPECTRAL ENERGY-DISTRIBUTIONS; YOUNG STELLAR OBJECTS; T-TAURI STARS; ACCRETION DISKS; CIRCUMSTELLAR DISKS; SPATIAL-DISTRIBUTION; FORMING REGIONS; GALACTIC PLANE; MASSIVE STARS; GRAIN-GROWTH AB Context. NGC 6611 and its parental cloud, the Eagle Nebula (M 16), are well-studied star-forming regions, thanks to their large content of both OB stars and stars with disks and the observed ongoing star formation. In our previous studies of the Eagle Nebula, we identified 834 disk-bearing stars associated with the cloud, after detecting their excesses in NIR bands from J band to 8.0 mu m. Aims. In this paper, we study in detail the nature of a subsample of disk-bearing stars that show peculiar characteristics. They appear older than the other members in the V vs. V - I diagram, and/or they have one or more IRAC colors at pure photospheric values, despite showing NIR excesses, when optical and infrared colors are compared. Methods. We confirm the membership of these stars to M 16 by a spectroscopic analysis. The physical properties of these stars with disks are studied by comparing their spectral energy distributions (SEDs) with the SEDs predicted by models of T Tauri stars with disks and envelopes. Results. We show that the age of these stars estimated from the V vs. V - I diagram is unreliable since their V - I colors are altered by the light scattered by the disk into the line of sight. Only in a few cases their SEDs are compatible with models with excesses in V band caused by optical veiling. Candidate members with disks and photospheric IRAC colors are selected by the used NIR disk diagnostic, which is sensitive to moderate excesses, such as those produced by disks with low masses. In 1/3 of these cases, scattering of stellar flux by the disks can also be invoked. Conclusions. The photospheric light scattered by the disk grains into the line of sight can affect the derivation of physical parameters of Class II stars from photometric optical and NIR data. Besides, the disks diagnostic we defined are useful for selecting stars with disks, even those with moderate excesses or whose optical colors are altered by veiling or photospheric scattered light. C1 [Guarcello, M. G.; Damiani, F.; Micela, G.; Prisinzano, L.; Sciortino, S.] INAF Osservatorio Astron Palermo, I-90134 Palermo, Italy. [Guarcello, M. G.; Peres, G.] Univ Palermo, Dipartimento Sci Fis & Astron, I-90134 Palermo, Italy. RP Guarcello, MG (reprint author), Smithsonian Astrophys Observ, MS 3,60 Garden St, Cambridge, MA 02138 USA. EM mguarce@astropa.unipa.it OI Micela, Giuseppina/0000-0002-9900-4751; Prisinzano, Loredana/0000-0002-8893-2210; PERES, Giovanni/0000-0002-6033-8180; Damiani, Francesco/0000-0002-7065-3061 FU CONSTELLATION grant [YA 2007]; PRIN-INAF FX Support for this work has been provided by the CONSTELLATION grant YA 2007 and the contract PRIN-INAF (P. I.: Lanza). This work is based on data obtained as part of the UKIRT Infrared Deep Sky Survey, public data obtained with WFI@ESO, 2MASS Point Source Catalog and GLIMPSE survey with Spitzer/IRAC. The authors acknowledge M. Caramazza for her help in Spitzer data analysis. NR 34 TC 14 Z9 14 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR A18 DI 10.1051/0004-6361/201014237 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900079 ER PT J AU Gupta, H Rimmer, P Pearson, JC Yu, S Herbst, E Harada, N Bergin, EA Neufeld, DA Melnick, GJ Bachiller, R Baechtold, W Bell, TA Blake, GA Caux, E Ceccarelli, C Cernicharo, J Chattopadhyay, G Comito, C Cabrit, S Crockett, NR Daniel, F Falgarone, E Diez-Gonzalez, MC Dubernet, ML Erickson, N Emprechtinger, M Encrenaz, P Gerin, M Gill, JJ Giesen, TF Goicoechea, JR Goldsmith, PF Joblin, C Johnstone, D Langer, WD Larsson, B Latter, WB Lin, RH Lis, DC Liseau, R Lord, SD Maiwald, FW Maret, S Martin, PG Martin-Pintado, J Menten, KM Morris, P Muller, HSP Murphy, JA Nordh, LH Olberg, M Ossenkopf, V Pagani, L Perault, M Phillips, TG Plume, R Qin, SL Salez, M Samoska, LA Schilke, P Schlecht, E Schlemmer, S Szczerba, R Stutzki, J Trappe, N van der Tak, FFS Vastel, C Wang, S Yorke, HW Zmuidzinas, J Boogert, A Gusten, R Hartogh, P Honingh, N Karpov, A Kooi, J Krieg, JM Schieder, R Zaal, P AF Gupta, H. Rimmer, P. Pearson, J. C. Yu, S. Herbst, E. Harada, N. Bergin, E. A. Neufeld, D. A. Melnick, G. J. Bachiller, R. Baechtold, W. Bell, T. A. Blake, G. A. Caux, E. Ceccarelli, C. Cernicharo, J. Chattopadhyay, G. Comito, C. Cabrit, S. Crockett, N. R. Daniel, F. Falgarone, E. Diez-Gonzalez, M. C. Dubernet, M. -L. Erickson, N. Emprechtinger, M. Encrenaz, P. Gerin, M. Gill, J. J. Giesen, T. F. Goicoechea, J. R. Goldsmith, P. F. Joblin, C. Johnstone, D. Langer, W. D. Larsson, B. Latter, W. B. Lin, R. H. Lis, D. C. Liseau, R. Lord, S. D. Maiwald, F. W. Maret, S. Martin, P. G. Martin-Pintado, J. Menten, K. M. Morris, P. Mueller, H. S. P. Murphy, J. A. Nordh, L. H. Olberg, M. Ossenkopf, V. Pagani, L. Perault, M. Phillips, T. G. Plume, R. Qin, S. -L. Salez, M. Samoska, L. A. Schilke, P. Schlecht, E. Schlemmer, S. Szczerba, R. Stutzki, J. Trappe, N. van der Tak, F. F. S. Vastel, C. Wang, S. Yorke, H. W. Zmuidzinas, J. Boogert, A. Guesten, R. Hartogh, P. Honingh, N. Karpov, A. Kooi, J. Krieg, J. -M. Schieder, R. Zaal, P. TI Detection of OH+ and H2O+ towards Orion KL SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE astrochemistry; molecular processes; line: identification; ISM: abundances; submillimeter: ISM; stars: winds; outflows ID LASER MAGNETIC-RESONANCE; HERSCHEL OBSERVATIONS; INTERSTELLAR H3O+; STAR-FORMATION; DIFFUSE CLOUDS; COMET-KOHOUTEK; NEBULA; LINE; REGION; SPECTROSCOPY AB We report observations of the reactive molecular ions OH+, H2O+, and H3O+ towards Orion KL with Herschel/HIFI. All three N = 1-0 fine-structure transitions of OH+ at 909, 971, and 1033 GHz and both fine-structure components of the doublet ortho-H2O+ 1(11)-0(00) transition at 1115 and 1139 GHz were detected; an upper limit was obtained for H3O+, OH+ and H2O+ are observed purely in absorption, showing a narrow component at the source velocity of 9 km s(-1), and a broad blueshifted absorption similar to that reported recently for HF and para-(H2O)-O-18, and attributed to the low velocity outflow of Orion KL. We estimate column densities of OH+ and H2O+ for the 9 km s(-1) component of 9 +/- 3x10(12) cm(-2) and 7 +/- 2x10(12) cm(-2), and those in the outflow of 1.9 +/- 0.7x10(13) cm(-2) and 1.0 +/- 0.3x10(13) cm(-2). Upper limits of 2.4x10(12) cm(-2) and 8.7x10(12) cm(-2) were derived for the column densities of ortho and para-H3O+ from transitions near 985 and 1657 GHz. The column densities of the three ions are up to an order of magnitude lower than those obtained from recent observations of W31C and W49N. The comparatively low column densities may be explained by a higher gas density despite the assumption of a very high ionization rate. C1 [Gupta, H.; Pearson, J. C.; Yu, S.; Chattopadhyay, G.; Gill, J. J.; Goldsmith, P. F.; Langer, W. D.; Lin, R. H.; Samoska, L. A.; Schlecht, E.; Yorke, H. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Rimmer, P.; Herbst, E.; Harada, N.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Rimmer, P.; Herbst, E.; Harada, N.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Rimmer, P.; Herbst, E.; Harada, N.] Ohio State Univ, Dept Chem, Columbus, OH 43210 USA. [Bergin, E. A.; Crockett, N. R.; Wang, S.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Neufeld, D. A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Melnick, G. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bachiller, R.; Diez-Gonzalez, M. C.] Observ Astron Nacl IGN, Ctr Astron Yebes, Guadalajara 19080, Spain. [Baechtold, W.] ETH, Microwave Lab, CH-8092 Zurich, Switzerland. [Bell, T. A.; Blake, G. A.; Emprechtinger, M.; Lis, D. C.; Zmuidzinas, J.; Boogert, A.; Kooi, J.] CALTECH, Cahill Ctr Astron & Astrophys 301 17, Pasadena, CA 91125 USA. [Caux, E.; Joblin, C.; Vastel, C.] Univ Toulouse UPS, Ctr Etud Spatiale Rayonnements, F-31062 Toulouse 9, France. [Caux, E.; Joblin, C.; Vastel, C.] CNRS INSU, UMR 5187, F-31028 Toulouse 4, France. [Ceccarelli, C.; Maret, S.] Observ Grenoble, Astrophys Lab, F-38041 Grenoble 9, France. [Cernicharo, J.; Daniel, F.; Goicoechea, J. R.; Martin-Pintado, J.; Krieg, J. -M.] Ctr Astrobiol CSIC INTA, Lab Astrofis Mol, Madrid 28850, Spain. [Comito, C.; Goicoechea, J. R.; Menten, K. M.; Schilke, P.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Cabrit, S.; Pagani, L.; Salez, M.] Observ Paris, LERMA, F-75014 Paris, France. [Cabrit, S.; Pagani, L.; Salez, M.] Observ Paris, CNRS, UMR8112, F-75014 Paris, France. [Daniel, F.; Falgarone, E.; Encrenaz, P.; Gerin, M.; Perault, M.] Observ Paris, CNRS UMR8112, LERMA, F-75231 Paris 05, France. [Dubernet, M. -L.] Univ Paris 06, UMR7092, LPMAA, Paris, France. [Dubernet, M. -L.] Observ Paris, UMR8102, LUTH, Meudon, France. [Erickson, N.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Giesen, T. F.; Mueller, H. S. P.; Ossenkopf, V.; Qin, S. -L.; Schilke, P.; Schlemmer, S.; Stutzki, J.; Schieder, R.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Larsson, B.; Liseau, R.; Nordh, L. H.; Olberg, M.] Stockholm Univ, Dept Astron, S-10691 Stockholm, Sweden. [Johnstone, D.; Honingh, N.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Latter, W. B.; Lord, S. D.; Morris, P.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Liseau, R.; Olberg, M.] Chalmers, S-41296 Gothenburg, Sweden. [Martin, P. G.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Murphy, J. A.; Trappe, N.] Natl Univ Ireland, Maynooth, Kildare, Ireland. [Ossenkopf, V.; van der Tak, F. F. S.; Zaal, P.] Univ Groningen, SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [Szczerba, R.] Nicholas Copernicus Astron Ctr, PL-87100 Torun, Poland. [Plume, R.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Hartogh, P.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. RP Gupta, H (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM hgupta@jpl.nasa.gov RI Goldsmith, Paul/H-3159-2016; Martin-Pintado, Jesus/H-6107-2015; Giesen, Thomas /B-9476-2015; Schlemmer, Stephan/E-2903-2015; Trappe, Neil/C-9014-2016; Yu, Shanshan/D-8733-2016 OI Martin-Pintado, Jesus/0000-0003-4561-3508; Mueller, Holger/0000-0002-0183-8927; Rimmer, Paul/0000-0002-7180-081X; Giesen, Thomas /0000-0002-2401-0049; Schlemmer, Stephan/0000-0002-1421-7281; Trappe, Neil/0000-0003-2527-9821; FU JPL/Caltech 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; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astronomico Nacional (IGN), Centro de Astrobiologia (CSIC-INTA). Sweden: Chalmers University of Technology - MC2, RSS & GARD; Onsala Space Observatory; Swedish National Space Board, Stockholm University - Stockholm Observatory; Switzerland: ETH Zurich, FHNW; USA: Caltech, JPL, NHSC. Support for this work was provided by NASA through an award issued by JPL/Caltech. A part of the work described in this paper was done at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. Copyright 2010(C) California Institute of Technology. All rights reserved. NR 38 TC 33 Z9 33 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 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR L47 DI 10.1051/0004-6361/201015117 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900047 ER PT J AU Harwit, M Houde, M Sonnentrucker, P Boogert, ACA Cernicharo, J de Beck, E Decin, L Henkel, C Higgins, RD Jellema, W Kraus, A McCoey, C Melnick, GJ Menten, KM Risacher, C Teyssier, D Vaillancourt, JE Alcolea, J Bujarrabal, V Dominik, C Justtanont, K de Koter, A Marston, AP Olofsson, H Planesas, P Schmidt, M Schoier, FL Szczerba, R Waters, LBFM AF Harwit, M. Houde, M. Sonnentrucker, P. Boogert, A. C. A. Cernicharo, J. de Beck, E. Decin, L. Henkel, C. Higgins, R. D. Jellema, W. Kraus, A. McCoey, C. Melnick, G. J. Menten, K. M. Risacher, C. Teyssier, D. Vaillancourt, J. E. Alcolea, J. Bujarrabal, V. Dominik, C. Justtanont, K. de Koter, A. Marston, A. P. Olofsson, H. Planesas, P. Schmidt, M. Schoier, F. L. Szczerba, R. Waters, L. B. F. M. TI Polarisation observations of VY Canis Majoris H2O 5(32)-4(41) 620.701 GHz maser emission with HIFI SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: AGB and post-AGB; stars: winds, outflows; supergiants; circumstellar matter; masers; reference systems ID LATE-TYPE STARS; EVOLVED STARS; WATER MASERS; LINE; POLARIMETER; MILLIMETER; SHARP AB Context. Water vapour maser emission from evolved oxygen-rich stars remains poorly understood. Additional observations, including polarisation studies and simultaneous observation of different maser transitions may ultimately lead to greater insight. Aims. We have aimed to elucidate the nature and structure of the VY CMa water vapour masers in part by observationally testing a theoretical prediction of the relative strengths of the 620.701 GHz and the 22.235 GHz maser components of ortho H2O. Methods. In its high-resolution mode (HRS) the Herschel Heterodyne Instrument for the Far Infrared (HIFI) offers a frequency resolution of 0.125 MHz, corresponding to a line-of-sight velocity of 0.06 km s(-1), which we employed to obtain the strength and linear polarisation of maser spikes in the spectrum of VY CMa at 620.701 GHz. Simultaneous ground based observations of the 22.235 GHz maser with the Max-Planck-Institut fur Radioastronomie 100-m telescope at Effelsberg, provided a ratio of 620.701 GHz to 22.235 GHz emission. Results. We report the first astronomical detection to date of H2O maser emission at 620.701 GHz. In VY CMa both the 620.701 and the 22.235 GHz polarisation are weak. At 620.701 GHz the maser peaks are superposed on what appears to be a broad emission component, jointly ejected from the star. We observed the 620.701 GHz emission at two epochs 21 days apart, both to measure the potential direction of linearly polarised maser components and to obtain a measure of the longevity of these components. Although we do not detect significant polarisation levels in the core of the line, they rise up to approximately 6% in its wings. C1 [Harwit, M.] Cornell Univ, Ctr Radiophys & Space Res, Washington, DC 20024 USA. [Houde, M.; McCoey, C.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [Sonnentrucker, P.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Boogert, A. C. A.] CALTECH, IPAC, Pasadena, CA 91925 USA. [Cernicharo, J.] CSIC, Madrid 28006, Spain. [de Beck, E.; Decin, L.; Waters, L. B. F. M.] Katholieke Univ Leuven, Inst Sterrenkundeii, B-3001 Heverlee, Belgium. [Henkel, C.; Kraus, A.; Menten, K. M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Higgins, R. D.] Natl Univ Ireland, Dept Expt Phys, Maynooth, Kildare, Ireland. [Jellema, W.; Risacher, C.] Univ Groningen, SRON, NL-9700 AV Groningen, Netherlands. [McCoey, C.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [Melnick, G. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Teyssier, D.; Marston, A. P.] European Space Astron Ctr, Madrid 28080, Spain. [Vaillancourt, J. E.] NASA, SOFIA Sci Ctr, Univ Space Res Assoc, Ames Res Ctr, Moffett Field, CA 94035 USA. [Alcolea, J.] Observ Astron Nacl IGN, Madrid 28014, Spain. [Bujarrabal, V.; Planesas, P.] Observ Astron Nacl IGN, Alcala De Henares 28803, Spain. [Decin, L.; Dominik, C.; de Koter, A.; Waters, L. B. F. M.] Univ Amsterdam, Sterrenkundig Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. [Dominik, C.] Radboud Univ Nijmegen, Dept Astrophys, IMAPP, NL-6525 ED Nijmegen, Netherlands. [Justtanont, K.; Olofsson, H.; Schoier, F. L.] Chalmers, Dept Radio & Space Sci, Onsala Space Observ, S-43992 Onsala, Sweden. [de Koter, A.] Univ Utrecht, Netherlands & Astron Inst, NL-3584 CC Utrecht, Netherlands. [Olofsson, H.] Stockholm Univ, AlbaNova Univ Ctr, Dept Astron, S-10691 Stockholm, Sweden. [Planesas, P.] Joint ALMA Observ, Santiago, Chile. [Schmidt, M.; Szczerba, R.] Nicholas Copernicus Astron Ctr, PL-87100 Torun, Poland. RP Harwit, M (reprint author), Cornell Univ, Ctr Radiophys & Space Res, 511 H St SW, Washington, DC 20024 USA. EM harwit@verizon.net; houde@astro.uwo.ca RI Planesas, Pere/G-7950-2015; OI Planesas, Pere/0000-0002-7808-3040; De Beck, Elvire/0000-0002-7441-7189 FU NASA 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; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astronmico Nacional (IGN), Centro de Astrobiologia (CSIC-INTA). Sweden: Chalmers University of Technology - MC2, RSS & GARD; Onsala Space Observatory; Swedish National Space Board, Stockholm University - Stockholm Observatory; Switzerland: ETH Zurich, FHNW; USA: Caltech, JPL, NHSC. Support for this work was provided by NASA through an award issued by JPL/Caltech. We thank the HIFISTARS consortium for permission to use their VY CMa 556.9 GHz data for calibration purposes. We would like to acknowledge that Tom Phillips first pointed out to us that HIFI might yield useful polarisation observations. And, finally, we extend thanks to the anonymous referee for perceptive insights and suggestions that greatly improved this paper. NR 21 TC 11 Z9 11 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 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR L51 DI 10.1051/0004-6361/201015042 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900051 ER PT J AU Hily-Blant, P Maret, S Bacmann, A Bottinelli, S Parise, B Caux, E Faure, A Bergin, EA Blake, GA Castets, A Ceccarelli, C Cernicharo, J Coutens, A Crimier, N Demyk, K Dominik, C Gerin, M Hennebelle, P Henning, T Kahane, C Klotz, A Melnick, G Pagani, L Schilke, P Vastel, C Wakelam, V Walters, A Baudry, A Bell, T Benedettini, M Boogert, A Cabrit, S Caselli, P Codella, C Comito, C Encrenaz, P Falgarone, E Fuente, A Goldsmith, PF Helmich, F Herbst, E Jacq, T Kama, M Langer, W Lefloch, B Lis, D Lord, S Lorenzani, A Neufeld, D Nisini, B Pacheco, S Phillips, T Salez, M Saraceno, P Schuster, K Tielens, X van der Tak, F van der Wiel, MHD Viti, S Wyrowski, F Yorke, H AF Hily-Blant, P. Maret, S. Bacmann, A. Bottinelli, S. Parise, B. Caux, E. Faure, A. Bergin, E. A. Blake, G. A. Castets, A. Ceccarelli, C. Cernicharo, J. Coutens, A. Crimier, N. Demyk, K. Dominik, C. Gerin, M. Hennebelle, P. Henning, T. Kahane, C. Klotz, A. Melnick, G. Pagani, L. Schilke, P. Vastel, C. Wakelam, V. Walters, A. Baudry, A. Bell, T. Benedettini, M. Boogert, A. Cabrit, S. Caselli, P. Codella, C. Comito, C. Encrenaz, P. Falgarone, E. Fuente, A. Goldsmith, P. F. Helmich, F. Herbst, E. Jacq, T. Kama, M. Langer, W. Lefloch, B. Lis, D. Lord, S. Lorenzani, A. Neufeld, D. Nisini, B. Pacheco, S. Phillips, T. Salez, M. Saraceno, P. Schuster, K. Tielens, X. van der Tak, F. van der Wiel, M. H. D. Viti, S. Wyrowski, F. Yorke, H. TI Nitrogen hydrides in the cold envelope of IRAS 16293-2422 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: abundances; ISM: general; astrochemistry ID DISSOCIATIVE RECOMBINATION; PROTOSTAR IRAS16293-2422; INTERSTELLAR CLOUDS; DARK CLOUDS; CHEMISTRY; NH; MOLECULES; N2H+; SPECTROSCOPY; REGIONS AB Nitrogen is the fifth most abundant element in the Universe, yet the gas-phase chemistry of N-bearing species remains poorly understood. Nitrogen hydrides are key molecules of nitrogen chemistry. Their abundance ratios place strong constraints on the production pathways and reaction rates of nitrogen-bearing molecules. We observed the class 0 protostar IRAS 16293-2422 with the heterodyne instrument HIFI, covering most of the frequency range from 0.48 to 1.78 THz at high spectral resolution. The hyperfine structure of the amidogen radical o-NH2 is resolved and seen in absorption against the continuum of the protostar. Several transitions of ammonia from 1.2 to 1.8 THz are also seen in absorption. These lines trace the low-density envelope of the protostar. Column densities and abundances are estimated for each hydride. We find that NH:NH2:NH3 approximate to 5:1:300. Dark clouds chemical models predict steady-state abundances of NH2 and NH3 in reasonable agreement with the present observations, whilst that of NH is underpredicted by more than one order of magnitude, even using updated kinetic rates. Additional modelling of the nitrogen gas-phase chemistry in dark-cloud conditions is necessary before having recourse to heterogen processes. C1 [Hily-Blant, P.; Maret, S.; Bacmann, A.; Faure, A.; Castets, A.; Ceccarelli, C.; Crimier, N.; Kahane, C.; Lefloch, B.; Pacheco, S.] Univ Grenoble 1, CNRS, Lab Astrophys Grenoble, UMR 5571, Grenoble, France. [Bacmann, A.; Wakelam, V.; Baudry, A.; Jacq, T.] Univ Bordeaux, Lab Astrophys Bordeaux, CNRS, INSU,UMR 5804, Floirac, France. [Boogert, A.; Lord, S.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91109 USA. [Benedettini, M.; Saraceno, P.] Ist Fis Spazio Interplanetario, INAF, Rome, Italy. [Bottinelli, S.; Caux, E.; Coutens, A.; Demyk, K.; Vastel, C.; Walters, A.] Univ Toulouse 3, CNRS, Ctr Etud Spatiale Rayonnements, UMR 5187, F-31062 Toulouse, France. [Caselli, P.] Univ Leeds, Sch Phys & Astron, Leeds, W Yorkshire, England. [Pagani, L.; Cabrit, S.; Encrenaz, P.; Salez, M.] Observ Paris, CNRS, LERMA, F-75014 Paris, France. [Pagani, L.; Cabrit, S.; Encrenaz, P.; Salez, M.] Observ Paris, CNRS, UMR 8112, F-75014 Paris, France. [Cernicharo, J.; Crimier, N.] CSIC, INTA, Ctr Astrobiol, Madrid, Spain. [Parise, B.; Schilke, P.; Comito, C.; Wyrowski, F.] Max Planck Inst Radioastron, D-5300 Bonn, Germany. [Codella, C.; Lorenzani, A.] INAF Osservatorio Astrofis Arcetri, Florence, Italy. [Dominik, C.; Kama, M.] Univ Amsterdam, Astron Inst Anton Pannekoek, Amsterdam, Netherlands. [Dominik, C.] Radboud Univ Nijmegen, Dept Astrophys, IMAPP, NL-6525 ED Nijmegen, Netherlands. [Fuente, A.] IGN Observ Astron Nacl, Alcala De Henares, Spain. [Goldsmith, P. F.; Langer, W.; Yorke, H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Helmich, F.; van der Tak, F.; van der Wiel, M. H. D.] SRON Netherlands Inst Space Res, Groningen, Netherlands. [Herbst, E.] Ohio State Univ, Columbus, OH 43210 USA. [Melnick, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Neufeld, D.] Johns Hopkins Univ, Baltimore, MD USA. [Schilke, P.] Univ Cologne, Inst Phys, Cologne, Germany. [Schuster, K.] Inst Radio Astron Millimetr, Grenoble, France. [Tielens, X.] Leiden Univ, Leiden Observ, Leiden, Netherlands. [Viti, S.] UCL, Dept Phys & Astron, London, England. [Nisini, B.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy. [Bergin, E. A.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Henning, T.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [van der Tak, F.; van der Wiel, M. H. D.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AB Groningen, Netherlands. [Gerin, M.; Hennebelle, P.; Falgarone, E.] Ecole Normale Super, CNRS, LERMA, UMR 8112, Paris, France. RP Hily-Blant, P (reprint author), Univ Grenoble 1, CNRS, Lab Astrophys Grenoble, UMR 5571, Grenoble, France. RI van der Wiel, Matthijs/M-4531-2014; Coutens, Audrey/M-4533-2014; Fuente, Asuncion/G-1468-2016; Goldsmith, Paul/H-3159-2016; OI van der Wiel, Matthijs/0000-0002-4325-3011; Coutens, Audrey/0000-0003-1805-3920; Fuente, Asuncion/0000-0001-6317-6343; Lorenzani, Andrea/0000-0002-4685-3434; Wakelam, Valentine/0000-0001-9676-2605; Kama, Mihkel/0000-0003-0065-7267; Codella, Claudio/0000-0003-1514-3074; , Brunella Nisini/0000-0002-9190-0113; Maret, Sebastien/0000-0003-1104-4554 NR 38 TC 33 Z9 33 U1 0 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 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR L52 DI 10.1051/0004-6361/201015253 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900052 ER PT J AU Johnstone, D Fich, M McCoey, C van Kempen, TA Fuente, A Kristensen, LE Cernicharo, J Caselli, P Visser, R Plume, R Herczeg, GJ van Dishoeck, EF Wampfler, S Bachiller, R Baudry, A Benedettini, M Bergin, E Benz, AO Bjerkeli, P Blake, G Bontemps, S Braine, J Bruderer, S Codella, C Daniel, F di Giorgio, AM Dominik, C Doty, SD Encrenaz, P Giannini, T Goicoechea, JR de Graauw, T Helmich, F Herpin, F Hogerheijde, MR Jacq, T Jorgensen, JK Larsson, B Lis, D Liseau, R Marseille, M Melnick, G Neufeld, D Nisini, B Olberg, M Parise, B Pearson, J Risacher, C Santiago-Garcia, J Saraceno, P Shipman, R Tafalla, M van der Tak, F Wyrowski, F Yildiz, UA Caux, E Honingh, N Jellema, W Schieder, R Teyssier, D Whyborn, N AF Johnstone, D. Fich, M. McCoey, C. van Kempen, T. A. Fuente, A. Kristensen, L. E. Cernicharo, J. Caselli, P. Visser, R. Plume, R. Herczeg, G. J. van Dishoeck, E. F. Wampfler, S. Bachiller, R. Baudry, A. Benedettini, M. Bergin, E. Benz, A. O. Bjerkeli, P. Blake, G. Bontemps, S. Braine, J. Bruderer, S. Codella, C. Daniel, F. di Giorgio, A. M. Dominik, C. Doty, S. D. Encrenaz, P. Giannini, T. Goicoechea, J. R. de Graauw, Th. Helmich, F. Herpin, F. Hogerheijde, M. R. Jacq, T. Jorgensen, J. K. Larsson, B. Lis, D. Liseau, R. Marseille, M. Melnick, G. Neufeld, D. Nisini, B. Olberg, M. Parise, B. Pearson, J. Risacher, C. Santiago-Garcia, J. Saraceno, P. Shipman, R. Tafalla, M. van der Tak, F. Wyrowski, F. Yildiz, U. A. Caux, E. Honingh, N. Jellema, W. Schieder, R. Teyssier, D. Whyborn, N. TI Herschel/HIFI spectroscopy of the intermediate mass protostar NGC7129 FIRS 2 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE astrochemistry; stars: formation ID STAR-FORMING REGIONS; YOUNG STELLAR OBJECTS; PACS SPECTROSCOPY; HH 46; WATER; HIFI; EXCITATION; EVOLUTION AB Herschel/HIFI observations of water from the intermediate mass protostar NGC 7129 FIRS 2 provide a powerful diagnostic of the physical conditions in this star formation environment. Six spectral settings, covering four (H2O)-O-16 and two (H2O)-O-18 lines, were observed and all but one (H2O)-O-18 line were detected. The four (H2O)-O-16 lines discussed here share a similar morphology: a narrower, approximate to 6kms(-1), component centered slightly redward of the systemic velocity of NGC7129 FIRS 2 and a much broader, approximate to 25 km s(-1) component centered blueward and likely associated with powerful outflows. The narrower components are consistent with emission from water arising in the envelope around the intermediate mass protostar, and the abundance of H2O is constrained to approximate to 10(-7) for the outer envelope. Additionally, the presence of a narrow self-absorption component for the lowest energy lines is likely due to self-absorption from colder water in the outer envelope. The broader component, where the H2O/CO relative abundance is found to be approximate to 0.2, appears to be tracing the same energetic region that produces strong CO emission at high J. C1 [Johnstone, D.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Johnstone, D.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 1A1, Canada. [Fich, M.; McCoey, C.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G, Canada. [McCoey, C.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [van Kempen, T. A.; Kristensen, L. E.; Visser, R.; van Dishoeck, E. F.; Hogerheijde, M. R.; Yildiz, U. A.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [van Kempen, T. A.; Melnick, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fuente, A.; Bachiller, R.; Santiago-Garcia, J.; Tafalla, M.] Observ Astron Nacl IGN, Alcala De Henares 28800, Spain. [Cernicharo, J.] INTA CSIC, CAB, Dept Astrophys, Torrejon De Ardoz 28850, Spain. [Caselli, P.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Caselli, P.; Goicoechea, J. R.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Plume, R.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Herczeg, G. J.; van Dishoeck, E. F.] Max Planck Inst Extraterr Phys, D-37075 Garching, Germany. [Wampfler, S.; Baudry, A.; Benz, A. O.; Bruderer, S.] ETH, Inst Astron, CH-8093 Zurich, Switzerland. [Benedettini, M.; Codella, C.; di Giorgio, A. M.; Giannini, T.; Nisini, B.; Saraceno, P.] INAF Ist Fis Spazio Interplanetario, Area Ric Tor Vergata, I-00133 Rome, Italy. [Benedettini, M.; Bergin, E.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Bjerkeli, P.; Liseau, R.; Olberg, M.] Chalmers, Onsala Space Observ, Dept Radio & Space Sci, S-43992 Onsala, Sweden. [Blake, G.; Lis, D.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Bontemps, S.; Braine, J.; Herpin, F.; Jacq, T.] Univ Bordeaux, Lab Astrophys Bordeaux, Bordeaux, France. [Bontemps, S.; Braine, J.; Herpin, F.; Jacq, T.] CNRS INSU, UMR 5804, Floirac, France. [Daniel, F.] Observ Paris, LERMA UMR CNRS 8112, F-92195 Meudon, France. [Daniel, F.] CSIC, Dept Mol & Infrared Astrophys, E-28006 Madrid, Spain. [Dominik, C.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. [Doty, S. D.] Denison Univ, Dept Phys & Astron, Granville, OH 43023 USA. [Encrenaz, P.] Observ Paris, LERMA, F-75014 Paris, France. [Encrenaz, P.] Observ Paris, CNRS, UMR 8112, F-75014 Paris, France. [de Graauw, Th.; Whyborn, N.] Joint ALMA Off, Santiago, Chile. [Helmich, F.; Marseille, M.; Risacher, C.; Shipman, R.; van der Tak, F.; Jellema, W.] SRON Netherlands Inst Space Res, NL-9747 AD Groningen, Netherlands. [Jorgensen, J. K.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark. [Larsson, B.] Stockholm Univ, Dept Astron, S-10691 Stockholm, Sweden. [Parise, B.; Wyrowski, F.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Parise, B.; Honingh, N.; Schieder, R.] Univ Cologne, Inst Phys, KOSMA, D-50937 Cologne, Germany. [Neufeld, D.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Pearson, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [van der Tak, F.; Caux, E.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. Univ Toulouse UPS, Ctr Etud Spatiale Rayonnements, F-31062 Toulouse 9, France. CNRS INSU, UMR 5187, F-31028 Toulouse 4, France. [Teyssier, D.] ESA, European Space Astron Ctr, Madrid 28691, Spain. RP Johnstone, D (reprint author), Natl Res Council Canada, Herzberg Inst Astrophys, 5071 W Saanich Rd, Victoria, BC V9E 2E7, Canada. EM doug.johnstone@nrc-cnrc.gc.ca RI Yildiz, Umut/C-5257-2011; Kristensen, Lars/F-4774-2011; Visser, Ruud/J-8574-2012; Jorgensen, Jes Kristian/L-7936-2014; Wampfler, Susanne/D-2270-2015; Fuente, Asuncion/G-1468-2016; OI , Brunella Nisini/0000-0002-9190-0113; Codella, Claudio/0000-0003-1514-3074; Giannini, Teresa/0000-0002-0224-096X; Yildiz, Umut/0000-0001-6197-2864; Kristensen, Lars/0000-0003-1159-3721; Jorgensen, Jes Kristian/0000-0001-9133-8047; Wampfler, Susanne/0000-0002-3151-7657; Fuente, Asuncion/0000-0001-6317-6343; Bjerkeli, Per/0000-0002-7993-4118 FU Spanish MCINN [CSD2009-00038, AYA2006-14786, AYA2009-07304]; National Aeronautics and Space Administration FX We thank the HIFI ICC for all of their help with the data reduction, and both the referee and journal editor for critical comments and speed of response. J.C. and A.F. give thanks to Spanish MCINN for funding support under program CONSOLIDER INGENIO 2010 ref: CSD2009-00038, and J. C., under programs AYA2006-14786 and AYA2009-07304. 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. This program is made possible thanks to the HIFI guaranteed time program. HIFI has been designed and built by a consortium of institutes and university departments from across Europe, Canada and the United States under the leadership of SRON Netherlands Institute for Space Research Groningen, The Netherlands and with major contributions from Germany, France, and the US. Consortium members are: Canada: CSA, U. Waterloo; France: CESR, LAB, LERMA, IRAM; Germany: KOSMA, MPIfR, MPS; Ireland: NUI Maynooth; Italy: ASI, IFSI-INAF, Osservatorio Astrofisico di Arcetri-INAF; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astronomico Nacional (IGN), Centro de Astrobiologia (CSIC-INT); Sweden: Chalmers University of Technology - MC2, RSS & GARD, Onsala Space Observatory, Swedish National Space Board, Stockholm University - Stockholm Observatory; Switzerland: ETH Zurich, FHNW; USA: Caltech, JPL, NHSC. NR 18 TC 14 Z9 14 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 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR L41 DI 10.1051/0004-6361/201015122 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900041 ER PT J AU Justtanont, K Decin, L Schoier, FL Maercker, M Olofsson, H Bujarrabal, V Marston, AP Teyssier, D Alcolea, J Cernicharo, J Dominik, C de Koter, A Melnick, G Menten, K Neufeld, D Planesas, P Schmidt, M Szczerba, R Waters, R de Graauw, T Whyborn, N Finn, T Helmich, F Siebertz, O Schmulling, F Ossenkopf, V Lai, R AF Justtanont, K. Decin, L. Schoier, F. L. Maercker, M. Olofsson, H. Bujarrabal, V. Marston, A. P. Teyssier, D. Alcolea, J. Cernicharo, J. Dominik, C. de Koter, A. Melnick, G. Menten, K. Neufeld, D. Planesas, P. Schmidt, M. Szczerba, R. Waters, R. de Graauw, Th. Whyborn, N. Finn, T. Helmich, F. Siebertz, O. Schmuelling, F. Ossenkopf, V. Lai, R. TI A HIFI preview of warm molecular gas around chi Cygni: first detection of H2O emission toward an S-type AGB star SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: AGB and post-AGB; circumstellar matter; stars: kinematics and dynamics; stars: individual: chi Cyg; stars: late-type; stars: mass-loss ID GIANT BRANCH STARS; MASS-LOSS RATES; CIRCUMSTELLAR WATER-VAPOR; ROTATIONAL LINE-PROFILES; EVOLVED STARS; CARBON STARS; LOSS HISTORY; W-HYDRAE; ISO-SWS; CO AB Aims. A set of new, sensitive, and spectrally resolved, sub-millimeter line observations are used to probe the warm circumstellar gas around the S-type AGB star chi Cyg. The observed lines involve high rotational quantum numbers, which, combined with previously obtained lower-frequency data, make it posible to study in detail the chemical and physical properties of, essentially, the entire circumstellar envelope of chi Cyg. Methods. The data were obtained using the HIFI instrument aboard Herschel, whose high spectral resolution provides valuable information about the line profiles. Detailed, non-LTE, radiative transfer modelling, including dust radiative transfer coupled with a dynamical model, has been performed to derive the temperature, density, and velocity structure of the circumstellar envelope. Results. We report the first detection of circumstellar H2O rotational emission lines in an S-star. Using the high-J CO lines to derive the parameters for the circumstellar envelope, we modelled both the ortho-and para-H2O lines. Our modelling results are consistent with the velocity structure expected for a dust-driven wind. The derived total H2O abundance (relative to H-2) is (1.1 +/- 0.2) x 10(-5), much lower than that in O-rich stars. The derived ortho-to-para ratio of 2.1 +/- 0.6 is close to the high-temperature equilibrium limit, consistent with H2O being formed in the photosphere. C1 [Justtanont, K.; Schoier, F. L.; Olofsson, H.] Chalmers, Onsala Space Observ, Dept Radio & Spece Sci, S-43992 Onsala, Sweden. [Decin, L.; Waters, R.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium. [Decin, L.; Dominik, C.; de Koter, A.; Waters, R.] Univ Amsterdam, Sterrenkundig Inst Anton Pannekoek, NL-1098 Amsterdam, Netherlands. [Maercker, M.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany. [Olofsson, H.] Stockholm Univ, AlbaNova Univ Ctr, Dept Astron, S-10691 Stockholm, Sweden. [Bujarrabal, V.; Planesas, P.] Observ Astron Nacl, Alcala De Henares 28803, Spain. [Marston, A. P.; Teyssier, D.] ESA, European Space Astron Ctr, Madrid 28691, Spain. [Alcolea, J.] Observ Astron Nacl IGN, Madrid 28014, Spain. [de Koter, A.] INTA CSIC, CAB, Madrid 28850, Spain. [Dominik, C.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6525 ED Nijmegen, Netherlands. [de Koter, A.] Univ Utrecht, Astron Inst, NL-3584 CC Utrecht, Netherlands. [Melnick, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Menten, K.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Neufeld, D.] Johns Hopkins Univ, Baltimore, MD 21218 USA. [Planesas, P.] Joint ALMA Observ, Santiago, Chile. [Schmidt, M.; Szczerba, R.] Nicholas Copernicus Astron Ctr, PL-87100 Torun, Poland. [de Graauw, Th.; Whyborn, N.] Joint ALMA Off, Santiago, Chile. [Finn, T.] Natl Univ Ireland, Expt Phys Dept, Maynooth, Kildare, Ireland. [Helmich, F.] Univ Groningen, SRON Netherlands Inst Space Res, NL-9747 AD Groningen, Netherlands. [Siebertz, O.; Schmuelling, F.; Ossenkopf, V.] Univ Cologne, Inst Phys 1, KOSMA, D-50937 Cologne, Germany. [Lai, R.] Northrop Grumman Aerosp Syst, Redondo Beach, CA 90278 USA. [Maercker, M.] European So Observ, D-8046 Garching, Germany. RP Justtanont, K (reprint author), Chalmers, Onsala Space Observ, Dept Radio & Spece Sci, S-43992 Onsala, Sweden. EM justtanont@chalmers.se RI Planesas, Pere/G-7950-2015 OI Planesas, Pere/0000-0002-7808-3040 FU Swedish National Space Board; Spanish MICINN [CSD2009-00038]; Polish MNiSW [N 203 393334]; MICINN [AYA2009-07304]; National Aeronautics and Space Administration FX HCSS/HSpot/HIPE is a joint development (are joint developments) by the Herschel Science Ground Segment Consortium, consisting of ESA, the NASA Herschel Science Center, and the HIFI, PACS and SPIRE consortia. K.J., F.S., M.M., and H.O. acknowledge funding from the Swedish National Space Board. This work has been partially supported by the Spanish MICINN, within the program CONSOLIDER INGENIO 2010, under grant "Molecular Astrophysics: The Herschel and Alma Era - ASTROMOL" (Ref.: CSD2009-00038). R.Sz. and M.Sch. acknowledge support from grant N 203 393334 from Polish MNiSW. J.C. thanks funding from MICINN, grant AYA2009-07304. This research was performed, in part, through a JPL contract funded by the National Aeronautics and Space Administration. NR 45 TC 10 Z9 10 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 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR L6 DI 10.1051/0004-6361/201015092 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900006 ER PT J AU Kama, M Dominik, C Maret, S van der Tak, F Caux, E Ceccarelli, C Fuente, A Crimier, N Lord, S Bacmann, A Baudry, A Bell, T Benedettini, M Bergin, EA Blake, GA Boogert, A Bottinelli, S Cabrit, S Caselli, P Castets, A Cernicharo, J Codella, C Comito, C Coutens, A Demyk, K Encrenaz, P Falgarone, E Gerin, M Goldsmith, PF Helmich, F Hennebelle, P Henning, T Herbst, E Hily-Blant, P Jacq, T Kahane, C Klotz, A Langer, W Lefloch, B Lis, D Lorenzani, A Melnick, G Nisini, B Pacheco, S Pagani, L Parise, B Pearson, J Phillips, T Salez, M Saraceno, P Schilke, P Schuster, K Tielens, X van der Wiel, MHD Vastel, C Viti, S Wakelam, V Walters, A Wyrowski, F Yorke, H Cais, P Gusten, R Philipp, S Klein, T Helmich, F AF Kama, M. Dominik, C. Maret, S. van der Tak, F. Caux, E. Ceccarelli, C. Fuente, A. Crimier, N. Lord, S. Bacmann, A. Baudry, A. Bell, T. Benedettini, M. Bergin, E. A. Blake, G. A. Boogert, A. Bottinelli, S. Cabrit, S. Caselli, P. Castets, A. Cernicharo, J. Codella, C. Comito, C. Coutens, A. Demyk, K. Encrenaz, P. Falgarone, E. Gerin, M. Goldsmith, P. F. Helmich, F. Hennebelle, P. Henning, T. Herbst, E. Hily-Blant, P. Jacq, T. Kahane, C. Klotz, A. Langer, W. Lefloch, B. Lis, D. Lorenzani, A. Melnick, G. Nisini, B. Pacheco, S. Pagani, L. Parise, B. Pearson, J. Phillips, T. Salez, M. Saraceno, P. Schilke, P. Schuster, K. Tielens, X. van der Wiel, M. H. D. Vastel, C. Viti, S. Wakelam, V. Walters, A. Wyrowski, F. Yorke, H. Cais, P. Guesten, R. Philipp, S. Klein, T. Helmich, F. TI The methanol lines and hot core of OMC2-FIR4, an intermediate-mass protostar, with Herschel/HIFI SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: formation; ISM: abundances; ISM: kinematics and dynamics; ISM: molecules ID STAR-FORMING REGIONS; INTERSTELLAR CLOUDS; PACS SPECTROSCOPY; DIAGNOSTIC-TOOL; GAS; EXPLANATION; ENVELOPES; MOLECULES; ABUNDANCE; EMISSION AB In contrast with numerous studies on the physical and chemical structure of low-and high-mass protostars, much less is known about their intermediate-mass counterparts, a class of objects that could help to elucidate the mechanisms of star formation on both ends of the mass range. We present the first results from a rich HIFI spectral dataset on an intermediate-mass protostar, OMC2-FIR4, obtained in the CHESS (Chemical HErschel Survey of Star forming regions) key programme. The more than 100 methanol lines detected between 554 and 961 GHz cover a range in upper level energy of 40 to 540 K. Our physical interpretation focusses on the hot core, but likely the cold envelope and shocked regions also play a role in reality, because an analysis of the line profiles suggests the presence of multiple emission components. An upper limit of 10 (6) is placed on the methanol abundance in the hot core, using a population diagram, large-scale source model and other considerations. This value is consistent with abundances previously seen in low-mass hot cores. Furthermore, the highest energy lines at the highest frequencies display asymmetric profiles, which may arise from infall around the hot core. C1 [Kama, M.; Dominik, C.] Univ Amsterdam, Astron Inst Anton Pannekoek, Amsterdam, Netherlands. [Dominik, C.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6525 ED Nijmegen, Netherlands. [Maret, S.; Ceccarelli, C.; Crimier, N.; Bacmann, A.; Castets, A.; Hily-Blant, P.; Kahane, C.; Lefloch, B.; Pacheco, S.] Univ Grenoble 1, CNRS, UMR 5571, Lab Astrophys Grenoble, Grenoble, France. [van der Tak, F.; Helmich, F.; van der Wiel, M. H. D.; Helmich, F.] SRON Netherlands Inst Space Res, Groningen, Netherlands. [van der Tak, F.; van der Wiel, M. H. D.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AB Groningen, Netherlands. [Caux, E.; Bottinelli, S.; Coutens, A.; Demyk, K.; Klotz, A.; Vastel, C.; Walters, A.] Univ Toulouse 3, Ctr Etud Spatiale Rayonnements, F-31062 Toulouse, France. [Caux, E.; Bottinelli, S.; Coutens, A.; Demyk, K.; Klotz, A.; Vastel, C.; Walters, A.] CNRS INSU, UMR 5187, Toulouse, France. [Ceccarelli, C.; Bacmann, A.; Baudry, A.; Castets, A.; Jacq, T.; Wakelam, V.; Cais, P.] Univ Bordeaux, Lab Astrophys Bordeaux, Floirac, France. [Ceccarelli, C.; Bacmann, A.; Baudry, A.; Castets, A.; Jacq, T.; Wakelam, V.] CNRS INSU, UMR 5804, Floirac, France. [Fuente, A.] IGN Observ Astron Nacl, Alcala De Henares, Spain. [Crimier, N.; Cernicharo, J.] CSIC INTA, Ctr Astrobiol, Madrid, Spain. [Lord, S.; Boogert, A.] CALTECH, Infared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Benedettini, M.; Saraceno, P.] INAF Ist Fis Spazio Interplanetario, Rome, Italy. [Caselli, P.] Univ Leeds, Sch Phys & Astron, Leeds, W Yorkshire, England. [Cabrit, S.; Encrenaz, P.; Falgarone, E.; Gerin, M.; Hennebelle, P.; Pagani, L.; Salez, M.] UCP, UPMC, ENS,UMR CNRS INSU 8112, OP,Lab Etud Rayonnement & Matiere Astrophys, Paris, France. [Comito, C.; Parise, B.; Schilke, P.; Wyrowski, F.; Guesten, R.; Philipp, S.; Klein, T.] Max Planck Inst Radioastron, D-5300 Bonn, Germany. [Codella, C.; Lorenzani, A.] INAF Osservatorio Astrofis Arcetri, Florence, Italy. [Goldsmith, P. F.; Langer, W.; Pearson, J.; Yorke, H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Herbst, E.] Ohio State Univ, Columbus, OH 43210 USA. [Melnick, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Schilke, P.; Viti, S.] Univ Cologne, Inst Phys, Cologne, Germany. [Schuster, K.] Inst Radio Astron Millimetr, Grenoble, France. [Tielens, X.] Leiden Univ, Leiden Observ, Leiden, Netherlands. [Nisini, B.] INAF Osservatorio Astron Roma, Monte Porzio Catone, Italy. [Bergin, E. A.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Henning, T.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. RP Kama, M (reprint author), Univ Amsterdam, Astron Inst Anton Pannekoek, Amsterdam, Netherlands. RI van der Wiel, Matthijs/M-4531-2014; Coutens, Audrey/M-4533-2014; Fuente, Asuncion/G-1468-2016; Goldsmith, Paul/H-3159-2016; OI van der Wiel, Matthijs/0000-0002-4325-3011; Coutens, Audrey/0000-0003-1805-3920; Fuente, Asuncion/0000-0001-6317-6343; Lorenzani, Andrea/0000-0002-4685-3434; Wakelam, Valentine/0000-0001-9676-2605; Kama, Mihkel/0000-0003-0065-7267; Codella, Claudio/0000-0003-1514-3074; , Brunella Nisini/0000-0002-9190-0113; Maret, Sebastien/0000-0003-1104-4554 FU Netherlands Organisation for Scientific Research (NWO) [021.002.081]; Leids Kerkhoven-Bosscha Fonds FX The authors are grateful to the referee, Dr. Tim van Kempen, for constructive comments leading to a significant improvement of the paper, and to Rens Waters for helpful discussions. HIFI has been designed and built by a consortium of institutes and university departments from across Europe, Canada and the United States under the leadership of SRON Netherlands Institute for Space Research, Groningen, The Netherlands and with major contributions from Germany, France and the US. Consortium members are: Canada: CSA, U. Waterloo; France: CESR, LAB, LERMA, IRAM; Germany: KOSMA, MPIfR, MPS; Ireland, NUI Maynooth; Italy: ASI, IFSI-INAF, Osservatorio Astrofisico di Arcetri- INAF; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astron (U) over circle mico Nacional (IGN), Centro de Astrobiologia (CSIC-INTA). Sweden: Chalmers University of Technology - MC2, RSS & GARD; Onsala Space Observatory; Swedish National Space Board, Stockholm University - Stockholm Observatory; Switzerland: ETH Zurich, FHNW; USA: Caltech, JPL, NHSC, and we are deeply grateful to everyone involved in the designing, building, and exploitation of this fantastic instrument. HCSS, HSpot, and HIPE are joint developments by the Herschel Science Ground Segment Consortium, consisting of ESA, the NASA Herschel Science Center, and the HIFI, PACS, and SPIRE consortia. M. Kama gratefully acknowledges support from the Netherlands Organisation for Scientific Research (NWO) grant number 021.002.081 and the Leids Kerkhoven-Bosscha Fonds, and thanks SRON Groningen for hosting the HIFI ICC volunteers. NR 29 TC 11 Z9 11 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR L39 DI 10.1051/0004-6361/201015118 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900039 ER PT J AU Kristensen, LE Visser, R van Dishoeck, EF Yildiz, UA Doty, SD Herczeg, GJ Liu, FC Parise, B Jorgensen, JK van Kempen, TA Brinch, C Wampfler, SF Bruderer, S Benz, AO Hogerheijde, MR Deul, E Bachiller, R Baudry, A Benedettini, M Bergin, EA Bjerkeli, P Blake, GA Bontemps, S Braine, J Caselli, P Cernicharo, J Codella, C Daniel, F de Graauw, T di Giorgio, AM Dominik, C Encrenaz, P Fich, M Fuente, A Giannini, T Goicoechea, JR Helmich, F Herpin, F Jacq, T Johnstone, D Kaufman, MJ Larsson, B Lis, D Liseau, R Marseille, M McCoey, C Melnick, G Neufeld, D Nisini, B Olberg, M Pearson, JC Plume, R Risacher, C Santiago-Garcia, J Saraceno, P Shipman, R Tafalla, M Tielens, AGGM van der Tak, F Wyrowski, F Beintema, D de Jonge, A Dieleman, P Ossenkopf, V Roelfsema, P Stutzki, J Whyborn, N AF Kristensen, L. E. Visser, R. van Dishoeck, E. F. Yildiz, U. A. Doty, S. D. Herczeg, G. J. Liu, F. -C. Parise, B. Jorgensen, J. K. van Kempen, T. A. Brinch, C. Wampfler, S. F. Bruderer, S. Benz, A. O. Hogerheijde, M. R. Deul, E. Bachiller, R. Baudry, A. Benedettini, M. Bergin, E. A. Bjerkeli, P. Blake, G. A. Bontemps, S. Braine, J. Caselli, P. Cernicharo, J. Codella, C. Daniel, F. de Graauw, Th. di Giorgio, A. M. Dominik, C. Encrenaz, P. Fich, M. Fuente, A. Giannini, T. Goicoechea, J. R. Helmich, F. Herpin, F. Jacq, T. Johnstone, D. Kaufman, M. J. Larsson, B. Lis, D. Liseau, R. Marseille, M. McCoey, C. Melnick, G. Neufeld, D. Nisini, B. Olberg, M. Pearson, J. C. Plume, R. Risacher, C. Santiago-Garcia, J. Saraceno, P. Shipman, R. Tafalla, M. Tielens, A. G. G. M. van der Tak, F. Wyrowski, F. Beintema, D. de Jonge, A. Dieleman, P. Ossenkopf, V. Roelfsema, P. Stutzki, J. Whyborn, N. TI Water in low-mass star-forming regions with Herschel HIFI spectroscopy of NGC 1333 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE astrochemistry; stars: formation; ISM: molecules; ISM: jets and outflows; ISM: individual objects: NGC 1333 ID PROTOSTELLAR ENVELOPES; PHYSICAL STRUCTURE; NGC-1333 IRAS-4; SUBMILLIMETER; PROTOSTARS; EMISSION; OUTFLOW; ABUNDANCE; VAPOR; DISK AB "Water In Star-forming regions with Herschel" (WISH) is a key programme dedicated to studying the role of water and related species during the star-formation process and constraining the physical and chemical properties of young stellar objects. The Heterodyne Instrument for the Far-Infrared (HIFI) on the Herschel Space Observatory observed three deeply embedded protostars in the low-mass star-forming region NGC 1333 in several (H2O)-O-16, (H2O)-O-18, and CO transitions. Line profiles are resolved for five (H2O)-O-16 transitions in each source, revealing them to be surprisingly complex. The line profiles are decomposed into broad (>20 km s(-1)), medium-broad (similar to 5-10 km s(-1)), and narrow (<5 kms(-1)) components. The (H2O)-O-18 emission is only detected in broad 1(10)-1(01) lines (>20 km s(-1)), indicating that its physical origin is the same as for the broad (H2O)-O-16 component. In one of the sources, IRAS4A, an inverse P Cygni profile is observed, a clear sign of infall in the envelope. From the line profiles alone, it is clear that the bulk of emission arises from shocks, both on small (less than or similar to 1000 AU) and large scales along the outflow cavity walls (similar to 10 000 AU). The H2O line profiles are compared to CO line profiles to constrain the H2O abundance as a function of velocity within these shocked regions. The H2O/CO abundance ratios are measured to be in the range of similar to 0.1-1, corresponding to H2O abundances of similar to 10(-5)-10(-4) with respect to H-2. Approximately 5-10% of the gas is hot enough for all oxygen to be driven into water in warm post-shock gas, mostly at high velocities. C1 [Kristensen, L. E.; Visser, R.; van Dishoeck, E. F.; Yildiz, U. A.; Brinch, C.; Hogerheijde, M. R.; Deul, E.; Tielens, A. G. G. M.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [van Dishoeck, E. F.; Herczeg, G. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Doty, S. D.] Denison Univ, Dept Phys & Astron, Granville, OH 43023 USA. [Liu, F. -C.; Parise, B.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Jorgensen, J. K.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen K, Denmark. [van Kempen, T. A.; Melnick, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Wampfler, S. F.; Bruderer, S.; Benz, A. O.] ETH, Inst Astron, CH-8093 Zurich, Switzerland. [Bachiller, R.] Observ Astron Nacl IGN, Madrid 28014, Spain. [Baudry, A.; Bontemps, S.; Braine, J.; Herpin, F.; Jacq, T.] Univ Bordeaux, Lab Astrophys Bordeaux, Bordeaux, France. [Baudry, A.; Bontemps, S.; Braine, J.; Herpin, F.; Jacq, T.] CNRS INSU, UMR 5804, Floirac, France. [Benedettini, M.; di Giorgio, A. M.; Saraceno, P.] INAF Inst Fis Spazio Interplanetario, Area Ric Tor Vergata, I-00133 Rome, Italy. [Bergin, E. A.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Bjerkeli, P.; Liseau, R.; Olberg, M.] Chalmers, Onsala Space Observ, Dept Radio & Space Sci, S-43992 Onsala, Sweden. [Blake, G. A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Caselli, P.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Caselli, P.; Codella, C.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Cernicharo, J.; Daniel, F.; Goicoechea, J. R.] CSIC INTA, Dept Astrofis, Ctr Astrobiol, Madrid 28850, Spain. [de Graauw, Th.; Helmich, F.; Marseille, M.; Risacher, C.; Shipman, R.; van der Tak, F.; Beintema, D.; de Jonge, A.; Dieleman, P.; Roelfsema, P.] SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [Dominik, C.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. [Dominik, C.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands. [Encrenaz, P.] Observ Paris, LERMA, F-75014 Paris, France. [Encrenaz, P.] Observ Paris, CNRS, UMR 8112, F-75014 Paris, France. [Fich, M.; McCoey, C.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [Fuente, A.] Observ Astron Nacl, Alcala De Henares 28803, Spain. [Giannini, T.; Nisini, B.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy. [Johnstone, D.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Johnstone, D.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 1A1, Canada. [Kaufman, M. J.] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA. [Larsson, B.] Stockholm Univ, Dept Astron, S-10691 Stockholm, Sweden. [Lis, D.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [McCoey, C.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [Neufeld, D.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Pearson, J. C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Plume, R.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Santiago-Garcia, J.] Inst Radio Astron Millimetr, E-18012 Granada, Spain. [van der Tak, F.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Ossenkopf, V.; Stutzki, J.] Univ Cologne, Inst Phys 1, KOSMA, D-50937 Cologne, Germany. [Whyborn, N.] Joint ALMA Off, Santiago, Chile. RP Kristensen, LE (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. RI Yildiz, Umut/C-5257-2011; Kristensen, Lars/F-4774-2011; Visser, Ruud/J-8574-2012; Jorgensen, Jes Kristian/L-7936-2014; Wampfler, Susanne/D-2270-2015; Brinch, Christian/G-5157-2015; Fuente, Asuncion/G-1468-2016; OI Codella, Claudio/0000-0003-1514-3074; Yildiz, Umut/0000-0001-6197-2864; Kristensen, Lars/0000-0003-1159-3721; Jorgensen, Jes Kristian/0000-0001-9133-8047; Wampfler, Susanne/0000-0002-3151-7657; Brinch, Christian/0000-0002-5074-7183; Fuente, Asuncion/0000-0001-6317-6343; Bjerkeli, Per/0000-0002-7993-4118; Giannini, Teresa/0000-0002-0224-096X; , Brunella Nisini/0000-0002-9190-0113 NR 22 TC 62 Z9 62 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 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR L30 DI 10.1051/0004-6361/201015100 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900030 ER PT J AU Li, HN Christlieb, N Schorck, T Norris, JE Bessell, MS Yong, D Beers, TC Lee, YS Frebel, A Zhao, G AF Li, H. N. Christlieb, N. Schoerck, T. Norris, J. E. Bessell, M. S. Yong, D. Beers, T. C. Lee, Y. S. Frebel, A. Zhao, G. TI The stellar content of the Hamburg/ESO survey VI. Metallicity distribution of main-sequence turnoff stars in the Galactic halo SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE Galaxy: halo; surveys; stars: Population II; stars: statistics; stars: abundances ID METAL-POOR STARS; DIGITAL SKY SURVEY; MILKY-WAY TOMOGRAPHY; CHEMICAL EVOLUTION; ABUNDANCE ANALYSIS; HORIZONTAL-BRANCH; Y-2 ISOCHRONES; DATA RELEASE; DWARF STARS; GALAXY AB We determine the metallicity distribution function (MDF) of the Galactic halo based on metal-poor main-sequence turnoff-stars (MSTO) which were selected from the Hamburg/ESO objective-prism survey (HES) database. Corresponding follow-up moderate-resolution observations (R similar to 2000) of 682 stars (among which 617 were accepted program stars) were carried out with the 2.3 m telescope at the Siding Spring Observatory (SSO). Corrections for the survey volume covered by the sample stars were quantitatively estimated and applied to the observed MDF. The corrections are quite small, when compared with those for a previously studied sample of metal-poor giants. The corrected observational MDF of the turnoff sample was then compared with that of the giants, as well as with a number of theoretical predictions of Galactic chemical evolution, including the mass-loss modified simple model. Although the survey-volume corrected MDFs of the metal-poor turnoff and the halo giants notably differ in the region of [Fe/H] > -2.0, below [Fe/H] similar to -2.0, (the region we scientifically focus on most) both MDFs show a sharp drop at [Fe/H] similar to -3.6 and present rather similar distributions in the low-metallicity tail. Theoretical models can fit some parts of the observed MDF, but none is found to simultaneously reproduce the peak as well as the features in the metal-poor region with [Fe/H] between -2.0 to -3.6. Among the tested models only the GAMETE model, when normalized to the tail of the observed MDF below [Fe/H] similar to -3.0, and with Z(cr) = 10(-3.4) Z(circle dot), is able to predict the sharp drop at [Fe/H] similar to -3.6. C1 [Li, H. N.; Zhao, G.] Chinese Acad Sci, Natl Astron Observ, Key Lab Opt Astron, Beijing 100012, Peoples R China. [Li, H. N.; Christlieb, N.; Schoerck, T.] Univ Heidelberg, Zentrum Astron, D-69117 Heidelberg, Germany. [Li, H. N.] Chinese Acad Sci, Grad Univ, Beijing 100080, Peoples R China. [Norris, J. E.; Bessell, M. S.; Yong, D.] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [Beers, T. C.; Lee, Y. S.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Beers, T. C.; Lee, Y. S.] Michigan State Univ, JINA, E Lansing, MI 48824 USA. [Frebel, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Li, HN (reprint author), Chinese Acad Sci, Natl Astron Observ, Key Lab Opt Astron, A20 Datun Rd, Beijing 100012, Peoples R China. EM lhn@nao.cas.cn; N.Christlieb@lsw.uni-heidelberg.de; jen@mso.anu.edu.au; bessell@mso.anu.edu.au; yong@mso.anu.edu.au; beers@pa.msu.edu; lee@pa.msu.edu; afrebel@cfa.harvard.edu; gzhao@nao.cas.cn FU University of Heidelberg; Deutsche Forschungsgemeinschaft [CH 214/5-1]; Australian Research Council [DP0663562, DP0984924]; US National Science Foundation [PHY 02-16783, PHY 08-22648]; National Natural Science Foundation of China [10821061]; National Basic Research Program of China (973 Program) [2007CB815103]; National Aeronautics and Space Administration; National Science Foundation FX We express our sincere gratitude to the anonymous referee for the constructive comments. H. N. L. would like to thank N. Prantzos, T. Karlsson, and S. Salvadori for providing electronic versions of their theoretical MDF models and helpful comments. H. N. L. and N. C. acknowledge support from the Global Networks program of the University of Heidelberg and from Deutsche Forschungsgemeinschaft under grant CH 214/5-1. Studies at RSAA, ANU, of the most metal-poor stellar populations are supported by Australian Research Council grants DP0663562 and DP0984924, which J.E.N., M. S. B., and D.Y. are pleased to acknowledge. T. C. B. and Y.S.L. acknowledge partial funding of this work from grants PHY 02-16783 and PHY 08-22648: Physics Frontier Center/Joint Institute for Nuclear Astrophysics (JINA), awarded by the US National Science Foundation. This research is partly supported by the National Natural Science Foundation of China under grant No. 10821061 and National Basic Research Program of China (973 Program) under grant No. 2007CB815103, which H. N. L. and G.Z. would like to acknowledge. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. NR 68 TC 22 Z9 22 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 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR A10 DI 10.1051/0004-6361/201014797 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900071 ER PT J AU Lis, DC Phillips, TG Goldsmith, PF Neufeld, DA Herbst, E Comito, C Schilke, P Muller, HSP Bergin, EA Gerin, M Bell, TA Emprechtinger, M Black, JH Blake, GA Boulanger, F Caux, E Ceccarelli, C Cernicharo, J Coutens, A Crockett, NR Daniel, F Dartois, E De Luca, M Dubernet, ML Encrenaz, P Falgarone, E Geballe, TR Godard, B Giesen, TF Goicoechea, JR Gry, C Gupta, H Hennebelle, P Hily-Blant, P Kolos, R Krelowski, J Joblin, C Johnstone, D Kazmierczak, M Lord, SD Maret, S Martin, PG Martin-Pintado, J Melnick, GJ Menten, KM Monje, R Mookerjea, B Morris, P Murphy, JA Ossenkopf, V Pearson, JC Perault, M Persson, C Plume, R Qin, SL Salez, M Schlemmer, S Schmidt, M Sonnentrucker, P Stutzki, J Teyssier, D Trappe, N van der Tak, FFS Vastel, C Wang, S Yorke, HW Yu, S Zmuidzinas, J Boogert, A Erickson, N Karpov, A Kooi, J Maiwald, FW Schieder, R Zaal, P AF Lis, D. C. Phillips, T. G. Goldsmith, P. F. Neufeld, D. A. Herbst, E. Comito, C. Schilke, P. Mueller, H. S. P. Bergin, E. A. Gerin, M. Bell, T. A. Emprechtinger, M. Black, J. H. Blake, G. A. Boulanger, F. Caux, E. Ceccarelli, C. Cernicharo, J. Coutens, A. Crockett, N. R. Daniel, F. Dartois, E. De Luca, M. Dubernet, M. -L. Encrenaz, P. Falgarone, E. Geballe, T. R. Godard, B. Giesen, T. F. Goicoechea, J. R. Gry, C. Gupta, H. Hennebelle, P. Hily-Blant, P. Kolos, R. Krelowski, J. Joblin, C. Johnstone, D. Kazmierczak, M. Lord, S. D. Maret, S. Martin, P. G. Martin-Pintado, J. Melnick, G. J. Menten, K. M. Monje, R. Mookerjea, B. Morris, P. Murphy, J. A. Ossenkopf, V. Pearson, J. C. Perault, M. Persson, C. Plume, R. Qin, S. -L. Salez, M. Schlemmer, S. Schmidt, M. Sonnentrucker, P. Stutzki, J. Teyssier, D. Trappe, N. van der Tak, F. F. S. Vastel, C. Wang, S. Yorke, H. W. Yu, S. Zmuidzinas, J. Boogert, A. Erickson, N. Karpov, A. Kooi, J. Maiwald, F. W. Schieder, R. Zaal, P. TI Herschel/HIFI measurements of the ortho/para ratio in water towards Sagittarius B2(M) and W31C SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE astrochemistry; ISM: abundances; ISM: molecules; molecular processes; submillimeter: ISM ID MOLECULAR CLOUDS; COLOGNE DATABASE; SUBMILLIMETER; SPECTROSCOPY; ABSORPTION; ASTRONOMY; AMMONIA; OXYGEN; VAPOR; CDMS AB We present Herschel/HIFI observations of the fundamental rotational transitions of ortho- and para-(H2O)-O-16 and (H2O)-O-18 in absorption towards Sagittarius B2(M) and W31C. The ortho/para ratio in water in the foreground clouds on the line of sight towards these bright continuum sources is generally consistent with the statistical high-temperature ratio of 3, within the observational uncertainties. However, somewhat unexpectedly, we derive a low ortho/para ratio of 2.35 +/- 0.35, corresponding to a spin temperature of similar to 27 K, towards Sagittarius B2(M) at velocities of the expanding molecular ring. Water molecules in this region appear to have formed with, or relaxed to, an ortho/para ratio close to the value corresponding to the local temperature of the gas and dust. C1 [Lis, D. C.; Phillips, T. G.; Bell, T. A.; Emprechtinger, M.; Blake, G. A.; Monje, R.; Zmuidzinas, J.; Karpov, A.; Kooi, J.] CALTECH, Cahill Ctr Astron & Astrophys 301 17, Pasadena, CA 91125 USA. [Bergin, E. A.; Crockett, N. R.; Wang, S.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Neufeld, D. A.; Sonnentrucker, P.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Caux, E.; Coutens, A.; Joblin, C.; Vastel, C.] Univ Toulouse UPS, Ctr Etud Spatiale Rayonnements, F-31062 Toulouse 9, France. [Caux, E.; Coutens, A.; Joblin, C.; Vastel, C.] CNRS INSU, UMR 5187, F-31028 Toulouse 4, France. [Ceccarelli, C.] Observ Grenoble, Astrophys Lab, F-38041 Grenoble 9, France. [Cernicharo, J.; Daniel, F.; Goicoechea, J. R.; Martin-Pintado, J.] Ctr Astrobiol CSIC INTA, Lab Astrofis Mol, Madrid, Spain. [Comito, C.; Schilke, P.; Menten, K. M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Gerin, M.; Daniel, F.; De Luca, M.; Encrenaz, P.; Falgarone, E.; Godard, B.; Hennebelle, P.; Perault, M.; Salez, M.] Observ Paris, CNRS UMR8112, LERMA, F-75231 Paris 05, France. [Gerin, M.; Daniel, F.; De Luca, M.; Encrenaz, P.; Falgarone, E.; Godard, B.; Hennebelle, P.; Perault, M.; Salez, M.] Ecole Normale Super, F-75231 Paris 05, France. [Dubernet, M. -L.] Univ Paris 06, UMR7092, LPMAA, Paris, France. [Dubernet, M. -L.] Observ Paris, UMR8102, LUTH, Meudon, France. [Schilke, P.; Mueller, H. S. P.; Giesen, T. F.; Ossenkopf, V.; Qin, S. -L.; Schlemmer, S.; Stutzki, J.; Schieder, R.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Goldsmith, P. F.; Gry, C.; Gupta, H.; Pearson, J. C.; Yorke, H. W.; Yu, S.; Maiwald, F. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Herbst, E.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Herbst, E.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Herbst, E.] Ohio State Univ, Dept Chem, Columbus, OH 43210 USA. [Johnstone, D.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Lord, S. D.; Morris, P.; Boogert, A.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Martin, P. G.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Melnick, G. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Murphy, J. A.; Trappe, N.] Natl Univ Ireland Maynooth, Maynooth, Kildare, Ireland. [Ossenkopf, V.; van der Tak, F. F. S.; Zaal, P.] Univ Groningen, SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [Plume, R.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Erickson, N.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Black, J. H.; Persson, C.] Chalmers, S-41296 Gothenburg, Sweden. [Boulanger, F.; Dartois, E.] IAS, Orsay, France. [Krelowski, J.; Kazmierczak, M.] Nicholas Copernicus Univ, Torun, Poland. [Geballe, T. R.] Gemini Telescope, Hilo, HI USA. [Kolos, R.] Polish Acad Sci, Inst Phys Chem, Warsaw, Poland. [Mookerjea, B.] Tata Inst Fundamental Res, Bombay 400005, Maharashtra, India. [Teyssier, D.] ESA, European Space Astron Ctr, Madrid, Spain. RP Lis, DC (reprint author), CALTECH, Cahill Ctr Astron & Astrophys 301 17, Pasadena, CA 91125 USA. EM dcl@caltech.edu RI Goldsmith, Paul/H-3159-2016; Martin-Pintado, Jesus/H-6107-2015; Coutens, Audrey/M-4533-2014; Giesen, Thomas /B-9476-2015; Schlemmer, Stephan/E-2903-2015; Trappe, Neil/C-9014-2016; Yu, Shanshan/D-8733-2016 OI Martin-Pintado, Jesus/0000-0003-4561-3508; Coutens, Audrey/0000-0003-1805-3920; Giesen, Thomas /0000-0002-2401-0049; Mueller, Holger/0000-0002-0183-8927; Maret, Sebastien/0000-0003-1104-4554; Schlemmer, Stephan/0000-0002-1421-7281; Trappe, Neil/0000-0003-2527-9821; FU NASA through JPL/Caltech; NSF [AST-0540882]; National Aeronautics and Space Administration 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; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astronomico Nacional (IGN), Centro de Astrobiologia (CSIC-INTA). Sweden: Chalmers University of Technology-MC2, RSS & GARD; Onsala Space Observatory; Swedish National Space Board, Stockholm University - Stockholm Observatory; Switzerland: ETH Zurich, FHNW; USA: Caltech, JPL, NHSC. Support for this work was provided by NASA through an award issued by JPL/Caltech. D. C. L. is supported by the NSF, award AST-0540882 to the CSO. 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. NR 22 TC 40 Z9 40 U1 0 U2 8 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR L26 DI 10.1051/0004-6361/201015072 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900026 ER PT J AU Lis, DC Pearson, JC Neufeld, DA Schilke, P Muller, HSP Gupta, H Bell, TA Comito, C Phillips, TG Bergin, EA Ceccarelli, C Goldsmith, PF Blake, GA Bacmann, A Baudry, A Benedettini, M Benz, A Black, J Boogert, A Bottinelli, S Cabrit, S Caselli, P Castets, A Caux, E Cernicharo, J Codella, C Coutens, A Crimier, N Crockett, NR Daniel, F Demyk, K Dominic, C Dubernet, ML Emprechtinger, M Encrenaz, P Falgarone, E Fuente, A Gerin, M Giesen, TF Goicoechea, JR Helmich, F Hennebelle, P Henning, T Herbst, E Hily-Blant, P Hjalmarson, A Hollenbach, D Jack, T Joblin, C Johnstone, D Kahane, C Kama, M Kaufman, M Klotz, A Langer, WD Larsson, B Le Bourlot, J Lefloch, B Le Petit, F Li, D Liseau, R Lord, SD Lorenzani, A Maret, S Martin, PG Melnick, GJ Menten, KM Morris, P Murphy, JA Nagy, Z Nisini, B Ossenkopf, V Pacheco, S Pagani, L Parise, B Perault, M Plume, R Qin, SL Roueff, E Salez, M Sandqvist, A Saraceno, P Schlemmer, S Schuster, K Snell, R Stutzki, J Tielens, A Trappe, N van der Tak, FFS van der Wiel, MHD van Dishoeck, E Vastel, C Viti, S Wakelam, V Walters, A Wang, S Wyrowski, F Yorke, HW Yu, S Zmuidzinas, J Delorme, Y Desbat, JP Gusten, R Krieg, JM Delforge, B AF Lis, D. C. Pearson, J. C. Neufeld, D. A. Schilke, P. Mueller, H. S. P. Gupta, H. Bell, T. A. Comito, C. Phillips, T. G. Bergin, E. A. Ceccarelli, C. Goldsmith, P. F. Blake, G. A. Bacmann, A. Baudry, A. Benedettini, M. Benz, A. Black, J. Boogert, A. Bottinelli, S. Cabrit, S. Caselli, P. Castets, A. Caux, E. Cernicharo, J. Codella, C. Coutens, A. Crimier, N. Crockett, N. R. Daniel, F. Demyk, K. Dominic, C. Dubernet, M. -L. Emprechtinger, M. Encrenaz, P. Falgarone, E. Fuente, A. Gerin, M. Giesen, T. F. Goicoechea, J. R. Helmich, F. Hennebelle, P. Henning, Th. Herbst, E. Hily-Blant, P. Hjalmarson, A. Hollenbach, D. Jack, T. Joblin, C. Johnstone, D. Kahane, C. Kama, M. Kaufman, M. Klotz, A. Langer, W. D. Larsson, B. Le Bourlot, J. Lefloch, B. Le Petit, F. Li, D. Liseau, R. Lord, S. D. Lorenzani, A. Maret, S. Martin, P. G. Melnick, G. J. Menten, K. M. Morris, P. Murphy, J. A. Nagy, Z. Nisini, B. Ossenkopf, V. Pacheco, S. Pagani, L. Parise, B. Perault, M. Plume, R. Qin, S. -L. Roueff, E. Salez, M. Sandqvist, A. Saraceno, P. Schlemmer, S. Schuster, K. Snell, R. Stutzki, J. Tielens, A. Trappe, N. van der Tak, F. F. S. van der Wiel, M. H. D. van Dishoeck, E. Vastel, C. Viti, S. Wakelam, V. Walters, A. Wang, S. Wyrowski, F. Yorke, H. W. Yu, S. Zmuidzinas, J. Delorme, Y. Desbat, J. -P. Guesten, R. Krieg, J. -M. Delforge, B. TI Herschel/HIFI discovery of interstellar chloronium (H2Cl+) SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE astrochemistry; line: identification; ISM: abundances; ISM: molecules; molecular processes; submillimetre: ISM ID CHLORINE-BEARING MOLECULES; STAR-FORMING REGION; SPIRAL ARM CLOUDS; NGC 6334 I; HYDROGEN-CHLORIDE; COLOGNE DATABASE; ISOTOPIC RATIO; GROUND-STATE; SUBMILLIMETER; SPECTROSCOPY AB We report the first detection of chloronium, H2Cl+, in the interstellar medium, using the HIFI instrument aboard the Herschel Space Observatory. The 2(12)-1(01) lines of ortho-(H2Cl+)-Cl-35 and ortho-(H2Cl+)-Cl-37 are detected in absorption towards NGC 6334I, and the 1(11)-0(00) transition of para-(H2Cl+)-Cl-35 is detected in absorption towards NGC 6334I and Sgr B2(S). The H2Cl+ column densities are compared to those of the chemically-related species HCl. The derived HCl/H2Cl+ column density ratios, similar to 1-10, are within the range predicted by models of diffuse and dense photon dominated regions (PDRs). However, the observed H2Cl+ column densities, in excess of 10(13) cm(-2), are significantly higher than the model predictions. Our observations demonstrate the outstanding spectroscopic capabilities of HIFI for detecting new interstellar molecules and providing key constraints for astrochemical models. C1 [Lis, D. C.; Bell, T. A.; Phillips, T. G.; Blake, G. A.; Emprechtinger, M.; Zmuidzinas, J.] CALTECH, Cahill Ctr Astron & Astrophys 301 17, Pasadena, CA 91125 USA. [Bergin, E. A.; Crockett, N. R.; Wang, S.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Neufeld, D. A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Bottinelli, S.; Caux, E.; Coutens, A.; Demyk, K.; Joblin, C.; Klotz, A.; Vastel, C.; Walters, A.] Univ Toulouse UPS, Ctr Etud Spatiale Rayonnements, F-31062 Toulouse 9, France. [Bottinelli, S.; Caux, E.; Coutens, A.; Demyk, K.; Joblin, C.; Klotz, A.; Vastel, C.; Walters, A.] CNRS INSU, UMR 5187, F-31028 Toulouse 4, France. [Ceccarelli, C.; Bacmann, A.; Castets, A.; Crimier, N.; Hily-Blant, P.; Kahane, C.; Lefloch, B.; Maret, S.; Pacheco, S.] Observ Grenoble, Astrophys Lab, F-38041 Grenoble 9, France. [Cernicharo, J.; Crimier, N.; Daniel, F.; Goicoechea, J. R.] Ctr Astrobiol CSIC INTA, Lab Astrofis Mol, Madrid 28850, Spain. [Schilke, P.; Comito, C.; Menten, K. M.; Parise, B.; Wyrowski, F.; Guesten, R.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Daniel, F.; Falgarone, E.; Gerin, M.; Hennebelle, P.; Perault, M.] Observ Paris, UMR8112, CNRS, LERMA, F-75231 Paris 05, France. [Dubernet, M. -L.] Univ Paris 06, UMR7092, LPMAA, Paris, France. [Dubernet, M. -L.] Observ Paris, UMR8102, LUTH, Meudon, France. [Schilke, P.; Mueller, H. S. P.; Giesen, T. F.; Ossenkopf, V.; Qin, S. -L.; Schlemmer, S.; Stutzki, J.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Pearson, J. C.; Gupta, H.; Goldsmith, P. F.; Langer, W. D.; Li, D.; Morris, P.; Yorke, H. W.; Yu, S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Herbst, E.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Herbst, E.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Herbst, E.] Ohio State Univ, Dept Chem, Columbus, OH 43210 USA. [Daniel, F.; Falgarone, E.; Gerin, M.; Hennebelle, P.; Perault, M.] Ecole Normale Super, F-75231 Paris 05, France. [Johnstone, D.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Boogert, A.; Lord, S. D.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Martin, P. G.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Melnick, G. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Murphy, J. A.; Trappe, N.] Natl Univ Ireland, Maynooth, Kildare, Ireland. [Helmich, F.; Ossenkopf, V.] SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [Nagy, Z.; Plume, R.; van der Tak, F. F. S.; van der Wiel, M. H. D.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Snell, R.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Bacmann, A.; Baudry, A.; Jack, T.; Wakelam, V.; Desbat, J. -P.] Univ Bordeaux, Lab Astrophys Bordeaux, Bordeaux, France. [Bacmann, A.; Baudry, A.; Jack, T.; Wakelam, V.; Desbat, J. -P.] CNRS INSU, UMR 5804, Floirac, France. [Benedettini, M.; Lorenzani, A.; Saraceno, P.] INAF Ist Fis Spazio Interplanetario, Rome, Italy. [Cabrit, S.; Encrenaz, P.; Pagani, L.; Salez, M.] Observ Paris, LERMA, UMR 8112, CNRS, Paris, France. [Caselli, P.] Univ Leeds, Sch Phys & Astron, Leeds, W Yorkshire, England. [Codella, C.] INAF Osservatorio Astrofis Arcetri, Florence, Italy. [Dominic, C.; Kama, M.] Univ Amsterdam, Astron Inst Anton Pannekoek, Amsterdam, Netherlands. [Dominic, C.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6525 ED Nijmegen, Netherlands. [Fuente, A.] IGN Observ Astron Nacl, Alcala De Henares, Spain. [Nisini, B.] INAF Osservatorio Astron Roma, Monte Porzio Catone, Italy. [Schuster, K.] Inst RadioAstron Millimetr, Grenoble, France. [Tielens, A.; van Dishoeck, E.] Leiden Univ, Leiden Observ, Leiden, Netherlands. [Viti, S.] UCL, Dept Phys & Astron, London, England. [Black, J.; Liseau, R.] Chalmers, Dept Radio & Space Sci, Onsala, Sweden. [Benz, A.] ETH, Inst Astron, CH-8092 Zurich, Switzerland. [Hjalmarson, A.] Chalmers, Onsala Space Observ, Onsala, Sweden. [Hollenbach, D.] SETI Inst, Mountain View, CA USA. [Kaufman, M.] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA. [Larsson, B.] Stockholm Univ, Dept Astron, S-10691 Stockholm, Sweden. [Le Bourlot, J.; Le Petit, F.; Roueff, E.] Observ Paris, LUTH, Meudon, France. [Le Bourlot, J.; Le Petit, F.; Roueff, E.] Univ Paris 07, Meudon, France. [Salez, M.; Delorme, Y.; Krieg, J. -M.; Delforge, B.] UCP, UPMC, Inst Lab Etud Rayonnement & Mat Astrophys, UMR 8112,CNRS INSU,OP,ENS, Paris, France. [Henning, Th.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [van der Tak, F. F. S.; van der Wiel, M. H. D.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AB Groningen, Netherlands. RP Lis, DC (reprint author), CALTECH, Cahill Ctr Astron & Astrophys 301 17, Pasadena, CA 91125 USA. EM dcl@caltech.edu RI Schlemmer, Stephan/E-2903-2015; Trappe, Neil/C-9014-2016; Yu, Shanshan/D-8733-2016; Fuente, Asuncion/G-1468-2016; Goldsmith, Paul/H-3159-2016; van der Wiel, Matthijs/M-4531-2014; Coutens, Audrey/M-4533-2014; Giesen, Thomas /B-9476-2015 OI , Brunella Nisini/0000-0002-9190-0113; Schlemmer, Stephan/0000-0002-1421-7281; Trappe, Neil/0000-0003-2527-9821; Fuente, Asuncion/0000-0001-6317-6343; Lorenzani, Andrea/0000-0002-4685-3434; Mueller, Holger/0000-0002-0183-8927; Codella, Claudio/0000-0003-1514-3074; van der Wiel, Matthijs/0000-0002-4325-3011; Coutens, Audrey/0000-0003-1805-3920; Giesen, Thomas /0000-0002-2401-0049 FU NASA; NSF [AST-0540882] 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; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astronomico Nacional (IGN), Centro de Astrobiologia (CSIC-INTA). Sweden: Chalmers University of Technology - MC2, RSS & GARD; Onsala Space Observatory; Swedish National Space Board, Stockholm University - Stockholm Observatory; Switzerland: ETH Zurich, FHNW; USA: Caltech, JPL, NHSC. Support for this work was provided by NASA through an award issued by JPL/Caltech. D. C. L. is supported by the NSF, award AST-0540882 to the CSO. 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. NR 37 TC 48 Z9 48 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 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR L9 DI 10.1051/0004-6361/201014959 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900009 ER PT J AU Marseille, MG van der Tak, FFS Herpin, F Wyrowski, F Chavarria, L Pietropaoli, B Baudry, A Bontemps, S Cernicharo, J Jacq, T Frieswijk, W Shipman, R van Dishoeck, EF Bachiller, R Benedettini, M Benz, AO Bergin, E Bjerkeli, P Blake, GA Braine, J Bruderer, S Caselli, P Caux, E Codella, C Daniel, F Dieleman, P di Giorgio, AM Dominik, C Doty, SD Encrenaz, P Fich, M Fuente, A Gaier, T Giannini, T Goicoechea, JR de Graauw, T Helmich, F Herczeg, GJ Hogerheijde, MR Jackson, B Javadi, H Jellema, W Johnstone, D Jorgensen, JK Kester, D Kristensen, LE Larsson, B Laauwen, W Lis, D Liseau, R Luinge, W McCoey, C Megej, A Melnick, G Neufeld, D Nisini, B Olberg, M Parise, B Pearson, JC Plume, R Risacher, C Roelfsema, P Santiago-Garcia, J Saraceno, P Siegel, P Stutzki, J Tafalla, M van Kempen, TA Visser, R Wampfler, SF Yildiz, UA AF Marseille, M. G. van der Tak, F. F. S. Herpin, F. Wyrowski, F. Chavarria, L. Pietropaoli, B. Baudry, A. Bontemps, S. Cernicharo, J. Jacq, T. Frieswijk, W. Shipman, R. van Dishoeck, E. F. Bachiller, R. Benedettini, M. Benz, A. O. Bergin, E. Bjerkeli, P. Blake, G. A. Braine, J. Bruderer, S. Caselli, P. Caux, E. Codella, C. Daniel, F. Dieleman, P. di Giorgio, A. M. Dominik, C. Doty, S. D. Encrenaz, P. Fich, M. Fuente, A. Gaier, T. Giannini, T. Goicoechea, J. R. de Graauw, Th. Helmich, F. Herczeg, G. J. Hogerheijde, M. R. Jackson, B. Javadi, H. Jellema, W. Johnstone, D. Jorgensen, J. K. Kester, D. Kristensen, L. E. Larsson, B. Laauwen, W. Lis, D. Liseau, R. Luinge, W. McCoey, C. Megej, A. Melnick, G. Neufeld, D. Nisini, B. Olberg, M. Parise, B. Pearson, J. C. Plume, R. Risacher, C. Roelfsema, P. Santiago-Garcia, J. Saraceno, P. Siegel, P. Stutzki, J. Tafalla, M. van Kempen, T. A. Visser, R. Wampfler, S. F. Yildiz, U. A. TI Water abundances in high-mass protostellar envelopes: Herschel observations with HIFI SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE dust, extinction; ISM: molecules; ISM: abundances ID MONTE-CARLO METHOD; RADIATIVE-TRANSFER; STAR-FORMATION; PROTOSTARS; REGION; EXCITATION; EVOLUTION; EMISSION; CORES; H2O AB Aims. We derive the dense core structure and the water abundance in four massive star-forming regions in the hope of understanding the earliest stages of massive star formation. Methods. We present Herschel/HIFI observations of the para-H2O 1(11)-0(00) and 2(02)-1(11) and the para-(H2O)-O-18 1(11)-0(00) transitions. The envelope contribution to the line profiles is separated from contributions by outflows and foreground clouds. The envelope contribution is modeled with Monte-Carlo radiative transfer codes for dust and molecular lines (MC3D and RATRAN), and the water abundance and the turbulent velocity width as free parameters. Results. While the outflows are mostly seen in emission in high-J lines, envelopes are seen in absorption in ground-state lines, which are almost saturated. The derived water abundances range from 5 x 10(-10) to 4 x 10(-8) in the outer envelopes. We detect cold clouds surrounding the protostar envelope, thanks to the very high quality of the Herschel/HIFI data and the unique ability of water to probe them. Several foreground clouds are also detected along the line of sight. Conclusions. The low H2O abundances in massive dense cores are in accordance with the expectation that high densities and low temperatures lead to freeze-out of water on dust grains. The spread in abundance values is not clearly linked to physical properties of the sources. C1 [Marseille, M. G.; van der Tak, F. F. S.; Frieswijk, W.; Shipman, R.; Dieleman, P.; de Graauw, Th.; Helmich, F.; Jackson, B.; Jellema, W.; Kester, D.; Laauwen, W.; Luinge, W.; Risacher, C.; Roelfsema, P.] SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [van Dishoeck, E. F.; Hogerheijde, M. R.; Kristensen, L. E.; Visser, R.; Yildiz, U. A.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [van Dishoeck, E. F.; Herczeg, G. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Benz, A. O.; Bruderer, S.; Wampfler, S. F.] ETH, Inst Astron, CH-8093 Zurich, Switzerland. [Caselli, P.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Jacq, T.; Caselli, P.; Codella, C.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Herpin, F.; Chavarria, L.; Pietropaoli, B.; Baudry, A.; Bontemps, S.; Braine, J.] Univ Bordeaux, Lab Astrophys Bordeaux, Bordeaux, France. [Herpin, F.; Chavarria, L.; Pietropaoli, B.; Baudry, A.; Bontemps, S.; Braine, J.] CNRS INSU, UMR 5804, Floirac, France. [Johnstone, D.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Johnstone, D.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 1A1, Canada. [Bjerkeli, P.; Liseau, R.; Olberg, M.] Chalmers, Onsala Space Observ, Dept Radio & Space Sci, S-43992 Onsala, Sweden. [van der Tak, F. F. S.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Bachiller, R.; Tafalla, M.] Observ Astron Nacl IGN, Madrid 28014, Spain. [Benedettini, M.; di Giorgio, A. M.; Saraceno, P.] INAF Ist Fis Spazio Interplanetario, Area Ric Tor Vergata, I-00133 Rome, Italy. [Bergin, E.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Blake, G. A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Cernicharo, J.; Daniel, F.; Goicoechea, J. R.] CSIC INTA, Dept Astrofis, Ctr Astrobiol, Madrid 28850, Spain. [Dominik, C.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. [Dominik, C.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands. [Doty, S. D.] Denison Univ, Dept Phys & Astron, Granville, OH 43023 USA. [Encrenaz, P.] Observ Paris, LERMA, F-75014 Paris, France. [Encrenaz, P.] Observ Paris, CNRS, UMR 8112, F-75014 Paris, France. [Fich, M.; McCoey, C.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [Fuente, A.] Observ Astron Nacl, Alcala De Henares 28803, Spain. [Giannini, T.; Nisini, B.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy. [Jorgensen, J. K.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen K, Denmark. [Larsson, B.] Stockholm Univ, Dept Astron, S-10691 Stockholm, Sweden. [Lis, D.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [McCoey, C.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [Melnick, G.; van Kempen, T. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Neufeld, D.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Wyrowski, F.; Parise, B.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Gaier, T.; Javadi, H.; Pearson, J. C.; Siegel, P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Plume, R.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Santiago-Garcia, J.] Inst Radio Astron Millimetr, Granada 18012, Spain. [Stutzki, J.] Univ Cologne, Inst Phys 1, KOSMA, D-50937 Cologne, Germany. [Megej, A.] ETH, Microwave Lab, CH-8092 Zurich, Switzerland. [Caux, E.] Univ Toulouse UPS, Ctr Etud Spatiale Rayonnements, F-31062 Toulouse 9, France. [Caux, E.] CNRS INSU, UMR 5187, F-31028 Toulouse 4, France. RP Marseille, MG (reprint author), SRON Netherlands Inst Space Res, POB 800, NL-9700 AV Groningen, Netherlands. EM M.Marseille@sron.nl RI Yildiz, Umut/C-5257-2011; Kristensen, Lars/F-4774-2011; Visser, Ruud/J-8574-2012; Wampfler, Susanne/D-2270-2015; Fuente, Asuncion/G-1468-2016; OI Yildiz, Umut/0000-0001-6197-2864; Kristensen, Lars/0000-0003-1159-3721; Wampfler, Susanne/0000-0002-3151-7657; Fuente, Asuncion/0000-0001-6317-6343; Bjerkeli, Per/0000-0002-7993-4118; Codella, Claudio/0000-0003-1514-3074; Giannini, Teresa/0000-0002-0224-096X; , Brunella Nisini/0000-0002-9190-0113 NR 20 TC 17 Z9 17 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR L32 DI 10.1051/0004-6361/201015103 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900032 ER PT J AU Melnick, GJ Tolls, V Neufeld, DA Bergin, EA Phillips, TG Wang, S Crockett, NR Bell, TA Blake, GA Cabrit, S Caux, E Ceccarelli, C Cernicharo, J Comito, C Daniel, F Dubernet, ML Emprechtinger, M Encrenaz, P Falgarone, E Gerin, M Giesen, TF Goicoechea, JR Goldsmith, PF Herbst, E Joblin, C Johnstone, D Langer, WD Latter, WD Lis, DC Lord, SD Maret, S Martin, PG Menten, KM Morris, P Muller, HSP Murphy, JA Ossenkopf, V Pagani, L Pearson, JC Perault, M Plume, R Qin, SL Salez, M Schilke, P Schlemmer, S Stutzki, J Trappe, N van der Tak, FFS Vastel, C Yorke, HW Yu, S Zmuidzinas, J AF Melnick, G. J. Tolls, V. Neufeld, D. A. Bergin, E. A. Phillips, T. G. Wang, S. Crockett, N. R. Bell, T. A. Blake, G. A. Cabrit, S. Caux, E. Ceccarelli, C. Cernicharo, J. Comito, C. Daniel, F. Dubernet, M. -L. Emprechtinger, M. Encrenaz, P. Falgarone, E. Gerin, M. Giesen, T. F. Goicoechea, J. R. Goldsmith, P. F. Herbst, E. Joblin, C. Johnstone, D. Langer, W. D. Latter, W. D. Lis, D. C. Lord, S. D. Maret, S. Martin, P. G. Menten, K. M. Morris, P. Mueller, H. S. P. Murphy, J. A. Ossenkopf, V. Pagani, L. Pearson, J. C. Perault, M. Plume, R. Qin, S. -L. Salez, M. Schilke, P. Schlemmer, S. Stutzki, J. Trappe, N. van der Tak, F. F. S. Vastel, C. Yorke, H. W. Yu, S. Zmuidzinas, J. TI Herschel observations of EXtra-Ordinary Sources (HEXOS): Observations of H2O and its isotopologues towards Orion KL SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: abundances; ISM: molecules ID WAVE-ASTRONOMY-SATELLITE; WATER-VAPOR; SUBMILLIMETER; INSTRUMENT; ABSORPTION; EMISSION; OUTFLOWS; REGION; OMC-1; SWAS AB We report the detection of more than 48 velocity-resolved ground rotational state transitions of (H2O)-O-16, (H2O)-O-18, and (H2O)-O-17 - most for the first time - in both emission and absorption toward Orion KL using Herschel/HIFI. We show that a simple fit, constrained to match the known emission and absorption components along the line of sight, is in excellent agreement with the spectral profiles of all the water lines. Using the measured (H2O)-O-18 line fluxes, which are less affected by line opacity than their (H2O)-O-16 counterparts, and an escape probability method, the column densities of (H2O)-O-18 associated with each emission component are derived. We infer total water abundances of 7.4 x 10(-5), 1.0 x 10(-5), and 1.6 x 10(-5) for the plateau, hot core, and extended warm gas, respectively. In the case of the plateau, this value is consistent with previous measures of the Orion-KL water abundance as well as those of other molecular outflows. In the case of the hot core and extended warm gas, these values are somewhat higher than water abundances derived for other quiescent clouds, suggesting that these regions are likely experiencing enhanced water-ice sublimation from (and reduced freeze-out onto) grain surfaces due to the warmer dust in these sources. C1 [Melnick, G. J.; Tolls, V.] Harvard Smithsonian Ctr Astrophys CfA, Cambridge, MA 02138 USA. [Neufeld, D. A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Bergin, E. A.; Wang, S.; Crockett, N. R.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Phillips, T. G.; Bell, T. A.; Emprechtinger, M.; Joblin, C.; Lis, D. C.; Zmuidzinas, J.] CALTECH, Cahill Ctr Astron & Astrophys 301 17, Pasadena, CA 91125 USA. [Blake, G. A.; Joblin, C.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Caux, E.; Vastel, C.] Univ Toulouse UPS, Ctr Etud Spatiale Rayonnements, F-31062 Toulouse 9, France. [Caux, E.; Vastel, C.] CNRS INSU, UMR 5187, F-31028 Toulouse 4, France. [Ceccarelli, C.; Maret, S.] Observ Grenoble, Astrophys Lab, F-38041 Grenoble 9, France. [Cernicharo, J.; Daniel, F.; Goicoechea, J. R.] Ctr Astrobiol CSIC INTA, Lab Astrofis Mol, Madrid, Spain. [Comito, C.; Menten, K. M.; Schilke, P.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Daniel, F.; Encrenaz, P.; Falgarone, E.; Gerin, M.; Perault, M.] Observ Paris, CNRS UMR8112, LERMA, F-75231 Paris 05, France. [Daniel, F.; Encrenaz, P.; Falgarone, E.; Gerin, M.; Perault, M.] Ecole Normale Super, F-75231 Paris 05, France. [Dubernet, M. -L.] Univ Paris 06, UMR7092, LPMAA, Paris, France. [Dubernet, M. -L.] Observ Paris, UMR8102, LUTH, Meudon, France. [Giesen, T. F.; Mueller, H. S. P.; Ossenkopf, V.; Qin, S. -L.; Schilke, P.; Schlemmer, S.; Stutzki, J.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Goldsmith, P. F.; Langer, W. D.; Pearson, J. C.; Yorke, H. W.; Yu, S.] Jet Prop Lab, CALTECH, Pasadena, CA 91109 USA. [Herbst, E.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Herbst, E.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Herbst, E.] Ohio State Univ, Dept Chem, Columbus, OH 43210 USA. [Johnstone, D.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Latter, W. D.; Lord, S. D.; Morris, P.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Martin, P. G.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Murphy, J. A.; Trappe, N.] Natl Univ Ireland Maynooth, Maynooth, Kildare, Ireland. [Ossenkopf, V.; van der Tak, F. F. S.] Univ Groningen, SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [Plume, R.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Cabrit, S.; Pagani, L.; Salez, M.] Observ Paris, LERMA, F-75014 Paris, France. [Cabrit, S.; Pagani, L.; Salez, M.] Observ Paris, CNRS, UMR8112, F-75014 Paris, France. RP Melnick, GJ (reprint author), Harvard Smithsonian Ctr Astrophys CfA, 60 Garden St,Mail Stop 66, Cambridge, MA 02138 USA. EM gmelnick@cfa.harvard.edu RI Goldsmith, Paul/H-3159-2016; Giesen, Thomas /B-9476-2015; Schlemmer, Stephan/E-2903-2015; Trappe, Neil/C-9014-2016; Yu, Shanshan/D-8733-2016 OI Mueller, Holger/0000-0002-0183-8927; Giesen, Thomas /0000-0002-2401-0049; Schlemmer, Stephan/0000-0002-1421-7281; Trappe, Neil/0000-0003-2527-9821; FU NASA through JPL/Caltech; NSF [AST-0540882] 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; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astronomico Nacional (IGN), Centro de Astrobiologia (CSIC-INTA). Sweden: Chalmers University of Technology - MC2, RSS & GARD; Onsala Space Observatory; Swedish National Space Board, Stockholm University - Stockholm Observatory; Switzerland: ETH Zurich, FHNW; USA: Caltech, JPL, NHSC. Support for this work was provided by NASA through an award issued by JPL/Caltech. CSO is supported by the NSF, award AST-0540882. NR 20 TC 23 Z9 23 U1 1 U2 4 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR L27 DI 10.1051/0004-6361/201015085 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900027 ER PT J AU Menten, KM Wyrowski, F Alcolea, J De Beck, E Decin, L Marston, AP Bujarrabal, V Cernicharo, J Dominik, C Justtanont, K de Koter, A Melnick, G Neufeld, DA Olofsson, H Planesas, P Schmidt, M Schoier, FL Szczerba, R Teyssier, D Waters, LBFM Edwards, K Olberg, M Phillips, TG Morris, P Salez, M Caux, E AF Menten, K. M. Wyrowski, F. Alcolea, J. De Beck, E. Decin, L. Marston, A. P. Bujarrabal, V. Cernicharo, J. Dominik, C. Justtanont, K. de Koter, A. Melnick, G. Neufeld, D. A. Olofsson, H. Planesas, P. Schmidt, M. Schoier, F. L. Szczerba, R. Teyssier, D. Waters, L. B. F. M. Edwards, K. Olberg, M. Phillips, T. G. Morris, P. Salez, M. Caux, E. TI Herschel/HIFI deepens the circumstellar NH3 enigma SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: AGB and post-AGB; supergiants; circumstellar matter ID VY CANIS MAJORIS; INFRARED OBSERVATIONS; INTERSTELLAR AMMONIA; BEARING MOLECULES; INVERSION LINES; MASS-LOSS; IRC+10216; STARS; EMISSION; WATER AB Context. Circumstellar envelopes (CSEs) of a variety of evolved stars have been found to contain ammonia (NH3) in amounts that exceed predictions from conventional chemical models by many orders of magnitude. Aims. The observations reported here were performed in order to better constrain the NH3 abundance in the CSEs of four, quite diverse, oxygen-rich stars using the NH3 ortho J(K) = 1(0)-0(0) ground-state line. Methods. We used the Heterodyne Instrument for the Far Infrared aboard Herschel to observe the NH3 J(K) = 1(0)-0(0) transition near 572.5 GHz, simultaneously with the ortho-H2O J(Ka,Kc) = 1(1,0)-1(0,1) transition, toward VY CMa, OH 26.5+0.6, IRC+10420, and IK Tau. We conducted non-LTE radiative transfer modeling with the goal to derive the NH3 abundance in these objects' CSEs. For the last two stars, Very Large Array imaging of NH3 radio-wavelength inversion lines were used to provide further constraints, particularly on the spatial extent of the NH3-emitting regions. Results. We find remarkably strong NH3 emission in all of our objects with the NH3 line intensities rivaling those of the ground state H2O line. The NH3 abundances relative to H-2 are very high and range from 2 x 10(-7) to 3 x 10(-6) for the objects we have studied. Conclusions. Our observations confirm and even deepen the circumstellar NH3 enigma. While our radiative transfer modeling does not yield satisfactory fits to the observed line profiles, it does lead to abundance estimates that confirm the very high values found in earlier studies. New ways to tackle this mystery will include further Herschel observations of more NH3 lines and imaging with the Expanded Very Large Array. C1 [Menten, K. M.; Wyrowski, F.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Alcolea, J.] Observ Astron Nacl IGN, Madrid 28014, Spain. [De Beck, E.; Decin, L.; Waters, L. B. F. M.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium. [Decin, L.; Waters, L. B. F. M.] Univ Amsterdam, Sterrenkundig Inst Anton Pannekoek, NL-1098 Amsterdam, Netherlands. [Marston, A. P.; Dominik, C.; de Koter, A.; Teyssier, D.] ESA, European Space Astron Ctr, Madrid 28691, Spain. [Bujarrabal, V.; Planesas, P.] Observ Astron Nacl IGN, Alcala De Henares 28803, Spain. [Cernicharo, J.] INTA CSIC, CAB, Madrid 28850, Spain. [Dominik, C.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, Nijmegen, Netherlands. [Justtanont, K.; Olofsson, H.; Schoier, F. L.; Olberg, M.] Chalmers, Onsala Space Observ, Dept Radio & Space Sci, S-43992 Onsala, Sweden. [de Koter, A.] Univ Utrecht, Astron Inst, NL-3584 CC Utrecht, Netherlands. [Melnick, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Neufeld, D. A.] Johns Hopkins Univ, Baltimore, MD 21218 USA. [Olofsson, H.] Stockholm Univ, AlbaNova Univ Ctr, Dept Astron, S-10691 Stockholm, Sweden. [Schmidt, M.; Szczerba, R.] Nicholas Copernicus Astron Ctr, PL-87100 Torun, Poland. [Planesas, P.] Joint ALMA Observ, Santiago, Chile. [Edwards, K.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [Edwards, K.; Olberg, M.] Univ Groningen, SRON Netherlands Inst Space Res, NL-9747 AD Groningen, Netherlands. [Phillips, T. G.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Morris, P.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Salez, M.] UCP, UPMC, Lab Etud Rayonnement & Mat Astrophys, UMR 8112,CNRS INSU,OP,ENS, Paris, France. [Salez, M.] Observ Paris, LERMA, F-75014 Paris, France. [Caux, E.] Univ Toulouse UPS, Inst Ctr Etud Spatiale Rayonnements, F-31062 Toulouse 9, France. [Caux, E.] CNRS INSU, UMR 5187, F-31028 Toulouse 4, France. RP Menten, KM (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. EM kmenten@mpifr.de RI Planesas, Pere/G-7950-2015; OI Planesas, Pere/0000-0002-7808-3040; De Beck, Elvire/0000-0002-7441-7189 FU Spanish MICINN [CSD2009-00038]; Polish MNiSW [N 203 393334]; SNSB; 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; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astronomico Nacional (IGN), Centro de Astrobiologia (CSIC-INTA); Sweden: Chalmers University of Technology - MC2, RSS & GARD; Onsala Space Observatory; Swedish National Space Board, Stockholm University - Stockholm Observatory; Switzerland: ETH Zurich, FHNW; USA: Caltech, JPL, NHSC. HCSS / HSpot / HIPE is a joint development by the Herschel Science Ground Segment Consortium, consisting of ESA, the NASA Herschel Science Center, and the HIFI, PACS and SPIRE consortia. This work has been partially supported by the Spanish MICINN, within the program CONSOLIDER INGENIO 2010, under grant "Molecular Astrophysics: The Herschel and ALMA Era - ASTROMOL" (ref.: CSD2009-00038). R. Sz. and M. Sch. acknowledge support from grant N 203 393334 from the Polish MNiSW. K. J. acknowledges the funding from SNSB. J. C. thanks funding from MICINN, grant AYA2009-07304. NR 41 TC 25 Z9 25 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 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR L7 DI 10.1051/0004-6361/201015108 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900007 ER PT J AU Neufeld, DA Gonzalez-Alfonso, E Melnick, G Pulecka, M Schmidt, M Szczerba, R Bujarrabal, V Alcolea, J Cernicharo, J Decin, L Dominik, C Justtanont, K de Koter, A Marston, AP Menten, K Olofsson, H Planesas, P Schoier, FL Teyssier, D Waters, LBFM Edwards, K McCoey, C Shipman, R Jellema, W de Graauw, T Ossenkopf, V Schieder, R Philipp, S AF Neufeld, D. A. Gonzalez-Alfonso, E. Melnick, G. Pulecka, M. Schmidt, M. Szczerba, R. Bujarrabal, V. Alcolea, J. Cernicharo, J. Decin, L. Dominik, C. Justtanont, K. de Koter, A. Marston, A. P. Menten, K. Olofsson, H. Planesas, P. Schoier, F. L. Teyssier, D. Waters, L. B. F. M. Edwards, K. McCoey, C. Shipman, R. Jellema, W. de Graauw, T. Ossenkopf, V. Schieder, R. Philipp, S. TI Discovery of water vapour in the carbon star V Cygni from observations with Herschel/HIFI SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: AGB and post-AGB; circumstellar matter; submillimeter: stars ID GIANT BRANCH STARS; CIRCUMSTELLAR ENVELOPES; IRC+10216; EMISSION; SUBMILLIMETER; CHEMISTRY AB We report the discovery of water vapour toward the carbon star V Cygni. We have used Herschel's HIFI instrument, in dual beam switch mode, to observe the 1(11)-0(00) para-water transition at 1113.3430 GHz in the upper sideband of the Band 4b receiver. The observed spectral line profile is nearly parabolic, but with a slight asymmetry associated with blueshifted absorption, and the integrated antenna temperature is 1.69 +/- 0.17 K km s(-1). This detection of thermal water vapour emission, carried out as part of a small survey of water in carbon-rich stars, is only the second such detection toward a carbon-rich AGB star, the first having been obtained by the Submillimeter Wave Astronomy Satellite toward IRC+ 10216. For an assumed ortho-to-para ratio of 3 for water, the observed line intensity implies a water outflow rate similar to 3-6 x 10(-5) Earth masses per year and a water abundance relative to H-2 of similar to 2-5 x 10(-6). This value is a factor of at least 10(4) larger than the expected photospheric abundance in a carbon-rich environment, and - as in IRC+ 10216 - raises the intriguing possibility that the observed water is produced by the vapourisation of orbiting comets or dwarf planets. However, observations of the single line observed to date do not permit us to place strong constraints upon the spatial distribution or origin of the observed water, but future observations of additional transitions will allow us to determine the inner radius of the H2O-emitting zone, and the H2O ortho-to-para ratio, and thereby to place important constraints upon the origin of the observed water emission. C1 [Neufeld, D. A.] Johns Hopkins Univ, Baltimore, MD 21218 USA. [Gonzalez-Alfonso, E.] Univ Alcala de Henares, Dept Fis, Madrid 28871, Spain. [Melnick, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Pulecka, M.; Schmidt, M.; Szczerba, R.] Nicholas Copernicus Astron Ctr, PL-87100 Torun, Poland. [Bujarrabal, V.] Observ Astron Nacl IGN, Alcala De Henares 28803, Spain. [Alcolea, J.] Observ Astron Nacl IGN, Madrid 28014, Spain. [Cernicharo, J.] INTA CSIC, CAB, Madrid 28850, Spain. [Decin, L.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium. [Decin, L.; Dominik, C.; de Koter, A.; Waters, L. B. F. M.] Univ Amsterdam, Sterrenkundig Inst Anton Pannekoek, NL-1098 Amsterdam, Netherlands. [Justtanont, K.; Olofsson, H.; Schoier, F. L.] Chalmers, Dept Radio & Space Sci, Onsala Space Observ, S-43992 Onsala, Sweden. [Marston, A. P.; Teyssier, D.] ESA, European Space Astron Ctr, Madrid 28691, Spain. [Menten, K.; Philipp, S.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Olofsson, H.] Stockholm Univ, AlbaNova Univ Ctr, Dept Astron, S-10691 Stockholm, Sweden. [Planesas, P.] Joint ALMA Observ, Santiago, Chile. [Dominik, C.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, Nijmegen, Netherlands. [de Koter, A.] Univ Utrecht, Astron Inst, NL-3584 CC Utrecht, Netherlands. [Edwards, K.; McCoey, C.] Univ Western Ontario, London, ON N6A 3K7, Canada. [Shipman, R.; Jellema, W.] Univ Groningen, SRON Netherlands Inst Space Res, NL-9747 AD Groningen, Netherlands. [de Graauw, T.] Joint ALMA Off, Santiago, Chile. [Ossenkopf, V.; Schieder, R.] Univ Cologne, KOSMA, Inst Phys 1, D-50937 Cologne, Germany. [Edwards, K.; McCoey, C.] Univ Waterloo, Waterloo, ON N2L 3G1, Canada. RP Neufeld, DA (reprint author), Johns Hopkins Univ, 3400 N Charles St, Baltimore, MD 21218 USA. EM neufeld@pha.jhu.edu RI Planesas, Pere/G-7950-2015; OI Planesas, Pere/0000-0002-7808-3040; /0000-0003-1689-9201 FU National Aeronautics and Space Administration; Polish MNiSW [N 203 393334]; Spanish MICINN [CSD2009-00038] FX HIFI has been designed and built by a consortium of institutes and university departments from acrossEurope, 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 Astronomico 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, JPL, NHSC. This research was performed, in part, through a JPL contract funded by the National Aeronautics and Space Administration. R.Sz. and M.Sch. acknowledge support from grant N 203 393334 from Polish MNiSW. E.G.-A. is a Research Associate at the Harvard-Smithsonian Center for Astrophysics. This work has been partially supported by the Spanish MICINN, program CONSOLIDER INGENIO 2010, grant ASTROMOL (CSD2009-00038). NR 21 TC 11 Z9 11 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 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR L5 DI 10.1051/0004-6361/201015080 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900005 ER PT J AU O'Dwyer, B Del Zanna, G Mason, HE Weber, MA Tripathi, D AF O'Dwyer, B. Del Zanna, G. Mason, H. E. Weber, M. A. Tripathi, D. TI SDO/AIA response to coronal hole, quiet Sun, active region, and flare plasma SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE Sun: activity; Sun: atmosphere; Sun: corona; Sun: UV radiation ID ATOMIC DATABASE; EMISSION-LINES; SOLAR; SPECTROMETER; ANGSTROM; CHIANTI; EIT AB Aims. We examine the contribution of spectral lines and continuum emission to the EUV channels of the Atmospheric Imaging Assembly (AIA) on the Solar Dynamics Observatory (SDO) in different regions of the solar atmosphere. Methods. Synthetic spectra were obtained using the CHIANTI atomic database and sample differential emission measures for coronal hole, quiet Sun, active region and flare plasma. These synthetic spectra were convolved with the effective area of each channel, in order to determine the dominant contribution in different regions of the solar atmosphere. Results. We highlight the contribution of particular spectral lines which under certain conditions can affect the interpretation of SDO/AIA data. C1 [O'Dwyer, B.; Del Zanna, G.; Mason, H. E.; Tripathi, D.] Dept Appl Math & Theoret Phys, Cambridge CB3 0WA, England. [Weber, M. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP O'Dwyer, B (reprint author), Dept Appl Math & Theoret Phys, Wilberforce Rd, Cambridge CB3 0WA, England. EM B.O-Dwyer@damtp.cam.ac.uk; G.Del-Zanna@damtp.cam.ac.uk; H.E.Mason@damtp.cam.ac.uk; mweber@cfa.harvard.edu; D.Tripathi@damtp.cam.ac.uk RI Tripathi, Durgesh/D-9390-2012 OI Tripathi, Durgesh/0000-0003-1689-6254 FU Lockheed-Martin [SP02H1701R]; Gates Cambridge Trust; SAO FX B.O.D., G.D.Z., H.E.M., D.T. acknowledge STFC. M.W. was supported under AIA subcontract SP02H1701R from Lockheed-Martin. B.O.D. was supported by funding from the Gates Cambridge Trust. B.O.D. would like to thank the SAO for providing support for a visit during which this work was initiated. The authors thank Dr. Paul Boerner of the AIA Team for calculating the AIA effective areas. CHIANTI is a collaborative project involving researchers at NRL (USA), and the Universities of: Cambridge (UK), George Mason (USA), and Florence (Italy). NR 18 TC 156 Z9 156 U1 1 U2 6 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 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR A21 DI 10.1051/0004-6361/201014872 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900082 ER PT J AU Qin, SL Schilke, P Comito, C Moller, T Rolffs, R Muller, HSP Belloche, A Menten, KM Lis, DC Phillips, TG Bergin, EA Bell, TA Crockett, NR Blake, GA Cabrit, S Caux, E Ceccarelli, C Cernicharo, J Daniel, F Dubernet, ML Emprechtinger, M Encrenaz, P Falgarone, E Gerin, M Giesen, TF Goicoechea, JR Goldsmith, PF Gupta, H Herbst, E Joblin, C Johnstone, D Langer, WD Lord, SD Maret, S Martin, PG Melnick, GJ Morris, P Murphy, JA Neufeld, DA Ossenkopf, V Pagani, L Pearson, JC Perault, M Plume, R Salez, M Schlemmer, S Stutzki, J Trappe, N van der Tak, FFS Vastel, C Wang, S Yorke, HW Yu, S Zmuidzinas, J Boogert, A Gusten, R Hartogh, P Honingh, N Karpov, A Kooi, J Krieg, JM Schieder, R Diez-Gonzalez, MC Bachiller, R Martin-Pintado, J Baechtold, W Olberg, M Nordh, LH Gill, JL Chattopadhyay, G AF Qin, S. -L. Schilke, P. Comito, C. Moeller, T. Rolffs, R. Mueller, H. S. P. Belloche, A. Menten, K. M. Lis, D. C. Phillips, T. G. Bergin, E. A. Bell, T. A. Crockett, N. R. Blake, G. A. Cabrit, S. Caux, E. Ceccarelli, C. Cernicharo, J. Daniel, F. Dubernet, M. -L. Emprechtinger, M. Encrenaz, P. Falgarone, E. Gerin, M. Giesen, T. F. Goicoechea, J. R. Goldsmith, P. F. Gupta, H. Herbst, E. Joblin, C. Johnstone, D. Langer, W. D. Lord, S. D. Maret, S. Martin, P. G. Melnick, G. J. Morris, P. Murphy, J. A. Neufeld, D. A. Ossenkopf, V. Pagani, L. Pearson, J. C. Perault, M. Plume, R. Salez, M. Schlemmer, S. Stutzki, J. Trappe, N. van der Tak, F. F. S. Vastel, C. Wang, S. Yorke, H. W. Yu, S. Zmuidzinas, J. Boogert, A. Guesten, R. Hartogh, P. Honingh, N. Karpov, A. Kooi, J. Krieg, J. -M. Schieder, R. Diez-Gonzalez, M. C. Bachiller, R. Martin-Pintado, J. Baechtold, W. Olberg, M. Nordh, L. H. Gill, J. L. Chattopadhyay, G. TI Herschel observations of EXtra-Ordinary Sources (HEXOS): detecting spiral arm clouds by CH absorption lines SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: abundances; ISM: molecules ID MOLECULAR CLOUDS; SAGITTARIUS B2; COLOGNE DATABASE; SIGHT-LINE; SUBMILLIMETER; SPECTROSCOPY; G10.6-0.4; CHEMISTRY; MICROWAVE; HYDROGEN AB We have observed CH absorption lines (J = 3/2, N = 1 <- J = 1/2, N = 1) against the continuum source Sgr B2(M) using the Herschel/HIFI instrument. With the high spectral resolution and wide velocity coverage provided by HIFI, 31 CH absorption features with different radial velocities and line widths are detected and identified. The narrower line width and lower column density clouds show "spiral arm" cloud characteristics, while the absorption component with the broadest line width and highest column density corresponds to the gas from the Sgr B2 envelope. The observations show that each "spiral arm" harbors multiple velocity components, indicating that the clouds are not uniform and that they have internal structure. This line-of-sight through almost the entire Galaxy offers unique possibilities to study the basic chemistry of simple molecules in diffuse clouds, as a variety of different cloud classes are sampled simultaneously. We find that the linear relationship between CH and H-2 column densities found at lower AV by UV observations does not continue into the range of higher visual extinction. There, the curve flattens, which probably means that CH is depleted in the denser cores of these clouds. C1 [Qin, S. -L.; Schilke, P.; Moeller, T.; Mueller, H. S. P.; Giesen, T. F.; Ossenkopf, V.; Schlemmer, S.; Stutzki, J.; Honingh, N.; Schieder, R.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Schilke, P.; Comito, C.; Rolffs, R.; Belloche, A.; Menten, K. M.; Guesten, R.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Lis, D. C.; Phillips, T. G.; Bell, T. A.; Blake, G. A.; Emprechtinger, M.; Zmuidzinas, J.; Karpov, A.; Kooi, J.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Bergin, E. A.; Crockett, N. R.; Wang, S.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Cabrit, S.; Pagani, L.; Salez, M.] LERMA, F-75014 Paris, France. [Cabrit, S.; Pagani, L.; Salez, M.] Observ Paris, CNRS, UMR8112, F-75014 Paris, France. [Caux, E.; Joblin, C.; Vastel, C.] Univ Toulouse UPS, Ctr Etud Spatiale Rayonnements, F-31062 Toulouse 9, France. [Caux, E.; Joblin, C.; Vastel, C.] CNRS INSU, UMR 5187, F-31028 Toulouse 4, France. [Ceccarelli, C.; Maret, S.] Lab Astrophys Observ Grenoble, F-38041 Grenoble 9, France. [Cernicharo, J.; Daniel, F.; Goicoechea, J. R.; Martin-Pintado, J.] Ctr Astrobiol CSIC INTA, Lab Astrofis Mol, Madrid 28850, Spain. [Daniel, F.; Encrenaz, P.; Falgarone, E.; Gerin, M.; Perault, M.; Krieg, J. -M.] Observ Paris, UMR8112, CNRS, LERMA, F-75231 Paris 05, France. [Daniel, F.; Encrenaz, P.; Falgarone, E.; Gerin, M.; Perault, M.; Krieg, J. -M.] Ecole Normale Super, F-75231 Paris 05, France. [Dubernet, M. -L.] Univ Paris 06, LPMAA, UMR7092, Paris, France. [Dubernet, M. -L.] Observ Paris, LUTH, UMR8102, Meudon, France. [Goldsmith, P. F.; Gupta, H.; Langer, W. D.; Morris, P.; Pearson, J. C.; Yorke, H. W.; Yu, S.; Gill, J. L.; Chattopadhyay, G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Herbst, E.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Herbst, E.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Herbst, E.] Ohio State Univ, Dept Chem, Columbus, OH 43210 USA. [Johnstone, D.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Lord, S. D.; Boogert, A.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Martin, P. G.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Melnick, G. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Murphy, J. A.; Trappe, N.] Natl Univ Ireland Maynooth, Maynooth, Kildare, Ireland. [Neufeld, D. A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Ossenkopf, V.; van der Tak, F. F. S.] Univ Groningen, SRON Netherlands Inst Space Res, Groningen, Netherlands. [Plume, R.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Hartogh, P.] MPI Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. [Diez-Gonzalez, M. C.; Bachiller, R.] Ctr Astron Yebes, Observ Astron Nacl IGN, E-19080 Guadalajara, Spain. [Baechtold, W.] ETH, Microwave Lab, CH-8092 Zurich, Switzerland. [Olberg, M.] Univ Groningen, SRON Netherlands Inst Space Res, NL-9747 AD Groningen, Netherlands. [Olberg, M.] Chalmers, S-41296 Gteborg, Sweden. [Nordh, L. H.] Stockholm Univ, Dept Astron, S-10691 Stockholm, Sweden. RP Qin, SL (reprint author), Univ Cologne, Inst Phys 1, Zulpicher Str 77, D-50937 Cologne, Germany. EM qin@ph1.uni-koeln.de RI Trappe, Neil/C-9014-2016; Yu, Shanshan/D-8733-2016; Goldsmith, Paul/H-3159-2016; Martin-Pintado, Jesus/H-6107-2015; Giesen, Thomas /B-9476-2015; Schlemmer, Stephan/E-2903-2015 OI Trappe, Neil/0000-0003-2527-9821; Martin-Pintado, Jesus/0000-0003-4561-3508; Mueller, Holger/0000-0002-0183-8927; Maret, Sebastien/0000-0003-1104-4554; Giesen, Thomas /0000-0002-2401-0049; Schlemmer, Stephan/0000-0002-1421-7281 NR 41 TC 14 Z9 14 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 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR L14 DI 10.1051/0004-6361/201015107 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900014 ER PT J AU Rolffs, R Schilke, P Comito, C Bergin, EA van der Tak, FFS Lis, DC Qin, SL Menten, KM Gusten, R Bell, TA Blake, GA Caux, E Ceccarelli, C Cernicharo, J Crockett, NR Daniel, F Dubernet, ML Emprechtinger, M Encrenaz, P Gerin, M Giesen, TF Goicoechea, JR Goldsmith, PF Gupta, H Herbst, E Joblin, C Johnstone, D Langer, WD Latter, WD Lord, SD Maret, S Martin, PG Melnick, GJ Morris, P Muller, HSP Murphy, JA Ossenkopf, V Pearson, JC Perault, M Phillips, TG Plume, R Schlemmer, S Stutzki, J Trappe, N Vastel, C Wang, S Yorke, HW Yu, S Zmuidzinas, J Diez-Gonzalez, MC Bachiller, R Martin-Pintado, J Baechtold, W Olberg, M Nordh, LH Gill, JJ Chattopadhyay, G AF Rolffs, R. Schilke, P. Comito, C. Bergin, E. A. van der Tak, F. F. S. Lis, D. C. Qin, S. -L. Menten, K. M. Guesten, R. Bell, T. A. Blake, G. A. Caux, E. Ceccarelli, C. Cernicharo, J. Crockett, N. R. Daniel, F. Dubernet, M. -L. Emprechtinger, M. Encrenaz, P. Gerin, M. Giesen, T. F. Goicoechea, J. R. Goldsmith, P. F. Gupta, H. Herbst, E. Joblin, C. Johnstone, D. Langer, W. D. Latter, W. D. Lord, S. D. Maret, S. Martin, P. G. Melnick, G. J. Morris, P. Mueller, H. S. P. Murphy, J. A. Ossenkopf, V. Pearson, J. C. Perault, M. Phillips, T. G. Plume, R. Schlemmer, S. Stutzki, J. Trappe, N. Vastel, C. Wang, S. Yorke, H. W. Yu, S. Zmuidzinas, J. Diez-Gonzalez, M. C. Bachiller, R. Martin-Pintado, J. Baechtold, W. Olberg, M. Nordh, L. H. Gill, J. J. Chattopadhyay, G. TI Reversal of infall in SgrB2(M) revealed by Herschel/HIFI observations of HCN lines at THz frequencies SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: formation; ISM: kinematics and dynamics; ISM: structure; ISM: molecules; ISM: individual objects: SgrB2(M); submillimeter: ISM ID MOLECULAR-SPECTROSCOPY; COLOGNE DATABASE; STAR-FORMATION; FACILITY; OUTFLOW; CDMS; HIFI; B2 AB Aims. To investigate the accretion and feedback processes in massive star formation, we analyze the shapes of emission lines from hot molecular cores, whose asymmetries trace infall and expansion motions. Methods. The high-mass star forming region SgrB2(M) was observed with Herschel/HIFI (HEXOS key project) in various lines of HCN and its isotopologues, complemented by APEX data. The observations are compared to spherically symmetric, centrally heated models with density power-law gradient and different velocity fields (infall or infall+expansion), using the radiative transfer code RATRAN. Results. The HCN line profiles are asymmetric, with the emission peak shifting from blue to red with increasing J and decreasing line opacity (HCN to (HCN)-C-13). This is most evident in the HCN 12-11 line at 1062 GHz. These line shapes are reproduced by a model whose velocity field changes from infall in the outer part to expansion in the inner part. Conclusions. The qualitative reproduction of the HCN lines suggests that infall dominates in the colder, outer regions, but expansion dominates in the warmer, inner regions. We are thus witnessing the onset of feedback in massive star formation, starting to reverse the infall and finally disrupting the whole molecular cloud. To obtain our result, the THz lines uniquely covered by HIFI were critically important. C1 [Rolffs, R.; Schilke, P.; Comito, C.; Menten, K. M.; Guesten, R.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Rolffs, R.; Schilke, P.; Qin, S. -L.; Giesen, T. F.; Mueller, H. S. P.; Ossenkopf, V.; Schlemmer, S.; Stutzki, J.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Bergin, E. A.; Crockett, N. R.; Wang, S.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [van der Tak, F. F. S.; Ossenkopf, V.; Olberg, M.] Univ Groningen, SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [Lis, D. C.; Bell, T. A.; Emprechtinger, M.; Phillips, T. G.; Zmuidzinas, J.] CALTECH, Cahill Ctr Astron & Astrophys 301 17, Pasadena, CA 91125 USA. [Ceccarelli, C.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Caux, E.; Joblin, C.; Vastel, C.] Univ Toulouse UPS, Ctr Etud Spatiale Rayonnements, F-31062 Toulouse 9, France. [Caux, E.; Joblin, C.; Vastel, C.] CNRS INSU, UMR 5187, F-31028 Toulouse 4, France. [Ceccarelli, C.; Maret, S.] Observ Grenoble, Astrophys Lab, F-38041 Grenoble 9, France. [Daniel, F.; Goicoechea, J. R.] Ctr Astrobiol CSIC INTA, Lab Astrofis Mol, Madrid 28850, Spain. [Daniel, F.; Encrenaz, P.; Gerin, M.; Perault, M.] Observ Paris, CNRS UMR8112, LERMA, F-75231 Paris 05, France. [Daniel, F.; Encrenaz, P.; Gerin, M.; Perault, M.] Ecole Normale Super, F-75231 Paris 05, France. [Dubernet, M. -L.] Univ Paris 06, UMR7092, LPMAA, Paris, France. [Dubernet, M. -L.] Observ Paris, UMR8102, LUTH, Meudon, France. [Goldsmith, P. F.; Gupta, H.; Langer, W. D.; Pearson, J. C.; Yorke, H. W.; Yu, S.; Gill, J. J.; Chattopadhyay, G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Herbst, E.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Herbst, E.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Herbst, E.] Ohio State Univ, Dept Chem, Columbus, OH 43210 USA. [Johnstone, D.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Latter, W. D.; Lord, S. D.; Morris, P.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Martin, P. G.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Melnick, G. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Murphy, J. A.; Trappe, N.] Natl Univ Ireland Maynooth, Maynooth, Kildare, Ireland. [Plume, R.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Diez-Gonzalez, M. C.; Bachiller, R.] Observ Astron Nacl IGN, Ctr Astron Yebes, Guadalajara 19080, Spain. [Martin-Pintado, J.] CSIC, Inst Estruct Mat, Dept Astrofis Mol & Infrarroja, E-28006 Madrid, Spain. [Baechtold, W.] ETH, Microwave Lab, CH-8092 Zurich, Switzerland. [Olberg, M.] Chalmers, S-41296 Gothenburg, Sweden. [Nordh, L. H.] Stockholm Univ, Dept Astron, S-10691 Stockholm, Sweden. RP Rolffs, R (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. EM rrolffs@mpifr.de RI Goldsmith, Paul/H-3159-2016; Martin-Pintado, Jesus/H-6107-2015; Giesen, Thomas /B-9476-2015; Schlemmer, Stephan/E-2903-2015; Trappe, Neil/C-9014-2016; Yu, Shanshan/D-8733-2016 OI Martin-Pintado, Jesus/0000-0003-4561-3508; Mueller, Holger/0000-0002-0183-8927; Maret, Sebastien/0000-0003-1104-4554; Giesen, Thomas /0000-0002-2401-0049; Schlemmer, Stephan/0000-0002-1421-7281; Trappe, Neil/0000-0003-2527-9821; FU NASA through JPL/Caltech; NSF [AST-0540882] 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; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astronomico Nacional (IGN), Centro de Astrobiologia (CSIC-INTA). Sweden: Chalmers University of Technology - MC2, RSS & GARD; Onsala Space Observatory; Swedish National Space Board, Stockholm University - Stockholm Observatory; Switzerland: ETH Zurich, FHNW; USA: Caltech, JPL, NHSC. Support for this work was provided by NASA through an award issued by JPL/Caltech. CSO is supported by the NSF, award AST-0540882. NR 20 TC 16 Z9 16 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR L46 DI 10.1051/0004-6361/201015106 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900046 ER PT J AU Salter, DM Kospal, A Getman, KV Hogerheijde, MR van Kempen, TA Carpenter, JM Blake, GA Wilner, D AF Salter, D. M. Kospal, A. Getman, K. V. Hogerheijde, M. R. van Kempen, T. A. Carpenter, J. M. Blake, G. A. Wilner, D. TI Recurring millimeter flares as evidence for star-star magnetic reconnection events in the DQ Tauri PMS binary system SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: individual: DQ Tau; stars: pre-main sequence; binaries: spectroscopic; stars: flare; stars: magnetic field; radio continuum: stars ID CLASSICAL T-TAURI; SPECTROSCOPIC BINARY; SYNCHROTRON RADIATION; UBVRI PHOTOMETRY; SOLAR-FLARES; EMISSION; WAVELENGTHS; FIELDS; BREMSSTRAHLUNG; MODELS AB Observations of the T Tauri spectroscopic binary DQ Tau in April 2008 captured an unusual flare at 3 mm, which peaked at an observed maximum flux of similar to 0.5 Jy (about 27 times the quiescent value). Here we present follow-up millimeter observations that demonstrate a periodicity to the phenomenon. While monitoring 3 new periastron encounters, we have detected flares within 17.5 h (or 4.6%) of the orbital phase of the first reported flare and constrained the main emitting region to a stellar height of 3.7-6.8 R-star. The recorded activity is consistent with the proposed picture for synchrotron emission initiated by a magnetic reconnection event when the two stellar magnetospheres of the highly eccentric (e = 0.556) binary are believed to collide near periastron as the stars approach a minimum separation of 8 R-star (similar to 13 R-circle dot). The similar light curve decay profiles allow us to estimate an average flare duration of 30 h. Assuming one millimeter flare per orbit, DQ Tau could spend approximately 8% of its 15.8-day orbital period in an elevated flux state. These findings continue to serve as a small caution for millimeter flux points in spectral energy distributions that could contain unrecognized flare contributions. Our analysis of the millimeter emission provides an upper limit of 5% on the linear polarization. We discuss the extent to which a severely entangled magnetic field structure and Faraday rotation effects are likely to reduce the observed polarization fraction. We also predict that, for the current picture, the stellar magnetospheres must be misaligned at a significant angle or, alternatively, that the topologies of the outer magnetospheres are poorly described by a well-ordered dipole inside a radius of 7 R-star. Finally, to investigate whether reorganization of the magnetic field during the interaction affects mass accretion, we also present simultaneous optical (VRI) monitoring of the binary, as an established tracer of accretion activity in this system. We find that an accretion event can occur coincident in both time and duration with the synchrotron fallout of a magnetic reconnection event. While the pulsed accretion mechanism has been attributed previously to the dynamical motions of the stars alone, the similarities between the millimeter and optical light curves evoke the possibility of a causal or co-dependent relationship between the magnetospheric and dynamical processes. C1 [Salter, D. M.; Kospal, A.; Hogerheijde, M. R.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Getman, K. V.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [van Kempen, T. A.; Wilner, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Carpenter, J. M.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Blake, G. A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. RP Salter, DM (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. EM demerese@strw.leidenuniv.nl FU Leids Sterrekunde Fonds; Netherlands Organization for Scientific Research FX We would like to thank Vincent Pietu and Jan-Martin Winters at IRAM for their assistance in scheduling and carrying out the observations, as well as Sascha Trippe for help with the PdBI data reduction and analysis. At CARMA we are grateful to Lee Mundy and Nikolaus Volgenau for their assistance in acquiring the data in Director's discretionary time. We would like to thank the observing staff at Teide Observatory for the IAC80 observations, including Alex Oscoz Abad, Cristina Zurita, and Rafael Barrena Delgado. At Wellesley College, we are grateful to Kim McLeod, Wendy Bauer, Steve Slivan and the undergraduate observers Kirsten Levandowski, Kelsey Turbeville, and Kathryn Neugent. Finally, we thank Y. Boehler, A. Dutrey, V. Pietu and S. Guilloteau for communicating data prior to publication. Financial support for travel to Wellesley and IRAM for observational duties was provided by a Leids Sterrekunde Fonds grant. The research of D. M. S., A. K., and M. R. H. is supported through a VIDI grant from the Netherlands Organization for Scientific Research. NR 45 TC 17 Z9 17 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR A32 DI 10.1051/0004-6361/201015197 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900093 ER PT J AU Schilke, P Comito, C Muller, HSP Bergin, EA Herbst, E Lis, DC Neufeld, DA Phillips, TG Bell, TA Blake, GA Cabrit, S Caux, E Ceccarelli, C Cernicharo, J Crockett, NR Daniel, F Dubernet, ML Emprechtinger, M Encrenaz, P Falgarone, E Gerin, M Giesen, TF Goicoechea, JR Goldsmith, PF Gupta, H Joblin, C Johnstone, D Langer, WD Latter, WB Lord, SD Maret, S Martin, PG Melnick, GJ Menten, KM Morris, P Murphy, JA Ossenkopf, V Pagani, L Pearson, JC Perault, M Plume, R Qin, SL Salez, M Schlemmer, S Stutzki, J Trappe, N van der Tak, FFS Vastel, C Wang, S Yorke, HW Yu, S Erickson, N Maiwald, FW Kooi, J Karpov, A Zmuidzinas, J Boogert, A Schieder, R Zaal, P AF Schilke, P. Comito, C. Mueller, H. S. P. Bergin, E. A. Herbst, E. Lis, D. C. Neufeld, D. A. Phillips, T. G. Bell, T. A. Blake, G. A. Cabrit, S. Caux, E. Ceccarelli, C. Cernicharo, J. Crockett, N. R. Daniel, F. Dubernet, M. -L. Emprechtinger, M. Encrenaz, P. Falgarone, E. Gerin, M. Giesen, T. F. Goicoechea, J. R. Goldsmith, P. F. Gupta, H. Joblin, C. Johnstone, D. Langer, W. D. Latter, W. B. Lord, S. D. Maret, S. Martin, P. G. Melnick, G. J. Menten, K. M. Morris, P. Murphy, J. A. Ossenkopf, V. Pagani, L. Pearson, J. C. Perault, M. Plume, R. Qin, S. -L. Salez, M. Schlemmer, S. Stutzki, J. Trappe, N. van der Tak, F. F. S. Vastel, C. Wang, S. Yorke, H. W. Yu, S. Erickson, N. Maiwald, F. W. Kooi, J. Karpov, A. Zmuidzinas, J. Boogert, A. Schieder, R. Zaal, P. TI Herschel observations of ortho- and para-oxidaniumyl (H2O+) in spiral arm clouds toward Sagittarius B2(M) SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE astrochemistry; line: profiles; molecular processes ID LASER MAGNETIC-RESONANCE; MOLECULAR-SPECTROSCOPY; COLOGNE DATABASE; SUBMILLIMETER; LINE; BAND; SPECTRUM; B2; HYDROGEN; SPACE AB H2O+ has been observed in its ortho- and para- states toward the massive star forming core Sgr B2(M), located close to the Galactic center. The observations show absorption in all spiral arm clouds between the Sun and Sgr B2. The average o/p ratio of H2O+ in most velocity intervals is 4.8, which corresponds to a nuclear spin temperature of 21 K. The relationship of this spin temperature to the formation temperature and current physical temperature of the gas hosting H2O+ is discussed, but no firm conclusion is reached. In the velocity interval 0-60 km s(-1), an ortho/para ratio of below unity is found, but if this is due to an artifact of contamination by other species or real is not clear. C1 [Schilke, P.; Mueller, H. S. P.; Giesen, T. F.; Schlemmer, S.; Stutzki, J.; Schieder, R.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Schilke, P.; Comito, C.; Menten, K. M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Bergin, E. A.; Crockett, N. R.; Wang, S.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Lis, D. C.; Phillips, T. G.; Bell, T. A.; Emprechtinger, M.; Kooi, J.; Karpov, A.; Zmuidzinas, J.; Boogert, A.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Blake, G. A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Caux, E.; Joblin, C.; Vastel, C.] Univ Toulouse UPS, Ctr Etud Spatiale Rayonnements, F-31062 Toulouse 9, France. [Caux, E.; Joblin, C.; Vastel, C.] CNRS INSU, UMR 5187, F-31028 Toulouse 4, France. [Ceccarelli, C.; Maret, S.] Observ Grenoble, Astrophys Lab, F-38041 Grenoble 9, France. [Cernicharo, J.; Daniel, F.; Goicoechea, J. R.] Lab Astrofis Mol, Ctr Astrobiol CSIC INTA, Madrid, Spain. [Daniel, F.; Encrenaz, P.; Falgarone, E.; Gerin, M.; Perault, M.] Observ Paris, UMR8112, CNRS, LERMA, F-75231 Paris 05, France. [Daniel, F.; Encrenaz, P.; Falgarone, E.; Gerin, M.; Perault, M.] Ecole Normale Super, F-75231 Paris 05, France. [Dubernet, M. -L.] Univ Paris 06, UMR7092, LPMAA, Paris, France. [Dubernet, M. -L.; Ossenkopf, V.] Observ Paris, LUTH, UMR8102, Meudon, France. [Goldsmith, P. F.; Gupta, H.; Langer, W. D.; Pearson, J. C.; Qin, S. -L.; Yorke, H. W.; Yu, S.; Maiwald, F. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Herbst, E.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Herbst, E.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Herbst, E.] Ohio State Univ, Dept Chem, Columbus, OH 43210 USA. [Johnstone, D.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Latter, W. B.; Lord, S. D.; Morris, P.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Martin, P. G.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Melnick, G. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Murphy, J. A.; Trappe, N.] Natl Univ Ireland Maynooth, Maynooth, Kildare, Ireland. [Neufeld, D. A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Ossenkopf, V.; van der Tak, F. F. S.; Zaal, P.] Univ Groningen, SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [Plume, R.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Erickson, N.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Cabrit, S.; Pagani, L.; Salez, M.] Observ Paris, LERMA, F-75014 Paris, France. [Cabrit, S.; Pagani, L.; Salez, M.; Boogert, A.] Observ Paris, UMR8112, CNRS, F-75014 Paris, France. RP Schilke, P (reprint author), Univ Cologne, Inst Phys 1, Zulpicher Str 77, D-50937 Cologne, Germany. EM schilke@ph1.uni-koeln.de RI Giesen, Thomas /B-9476-2015; Schlemmer, Stephan/E-2903-2015; Trappe, Neil/C-9014-2016; Yu, Shanshan/D-8733-2016; Goldsmith, Paul/H-3159-2016 OI Giesen, Thomas /0000-0002-2401-0049; Schlemmer, Stephan/0000-0002-1421-7281; Mueller, Holger/0000-0002-0183-8927; Trappe, Neil/0000-0003-2527-9821; FU NASA; NSF [AST-0540882]; Bundesministerium fur Bildung und Forschung (BMBF); Deutsches Zentrum fur Luft- und Raumfahrt (DLR) 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; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astronomico Nacional (IGN), Centro de Astrobiologia (CSIC-INTA). Sweden: Chalmers University of Technology - MC2, RSS & GARD; Onsala Space Observatory; Swedish National Space Board, Stockholm University - Stockholm Observatory; Switzerland: ETH Zurich, FHNW; USA: Caltech, JPL, NHSC. Support for this work was provided by NASA through an award issued by JPL/Caltech. CSO is supported by the NSF, award AST-0540882.; H.S.P.M. is very grateful to the Bundesministerium fur Bildung und Forschung (BMBF) for financial support aimed at maintaining the Cologne Database for Molecular Spectroscopy, CDMS. This support has been administered by the Deutsches Zentrum fur Luft- und Raumfahrt (DLR). We appreciate funding for the ASTRONET Project CATS through the Bundesministerium fur Bildung und Forschung (BMBF). NR 37 TC 25 Z9 25 U1 0 U2 7 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR L11 DI 10.1051/0004-6361/201015087 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900011 ER PT J AU van der Wiel, MHD van der Tak, FFS Lis, DC Bell, T Bergin, EA Comito, C Emprechtinger, M Schilke, P Caux, E Ceccarelli, C Baudry, A Goldsmith, PF Herbst, E Langer, W Lord, S Neufeld, D Pearson, J Phillips, T Rolffs, R Yorke, H Bacmann, A Benedettini, M Blake, GA Boogert, A Bottinelli, S Cabrit, S Caselli, P Castets, A Cernicharo, J Codella, C Coutens, A Crimier, N Demyk, K Dominik, C Encrenaz, P Falgarone, E Fuente, A Gerin, M Helmich, F Hennebelle, P Henning, T Hily-Blant, P Jacq, T Kahane, C Kama, M Klotz, A Lefloch, B Lorenzani, A Maret, S Melnick, G Nisini, B Pacheco, S Pagani, L Parise, B Salez, M Saraceno, P Schuster, K Tielens, AGGM Vastel, C Viti, S Wakelam, V Walters, A Wyrowski, F Edwards, K Zmuidzinas, J Morris, P Samoska, LA Teyssier, D AF van der Wiel, M. H. D. van der Tak, F. F. S. Lis, D. C. Bell, T. Bergin, E. A. Comito, C. Emprechtinger, M. Schilke, P. Caux, E. Ceccarelli, C. Baudry, A. Goldsmith, P. F. Herbst, E. Langer, W. Lord, S. Neufeld, D. Pearson, J. Phillips, T. Rolffs, R. Yorke, H. Bacmann, A. Benedettini, M. Blake, G. A. Boogert, A. Bottinelli, S. Cabrit, S. Caselli, P. Castets, A. Cernicharo, J. Codella, C. Coutens, A. Crimier, N. Demyk, K. Dominik, C. Encrenaz, P. Falgarone, E. Fuente, A. Gerin, M. Helmich, F. Hennebelle, P. Henning, T. Hily-Blant, P. Jacq, T. Kahane, C. Kama, M. Klotz, A. Lefloch, B. Lorenzani, A. Maret, S. Melnick, G. Nisini, B. Pacheco, S. Pagani, L. Parise, B. Salez, M. Saraceno, P. Schuster, K. Tielens, A. G. G. M. Vastel, C. Viti, S. Wakelam, V. Walters, A. Wyrowski, F. Edwards, K. Zmuidzinas, J. Morris, P. Samoska, L. A. Teyssier, D. TI Herschel/HIFI observations of spectrally resolved methylidyne signatures toward the high-mass star-forming core NGC 6334I SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: formation; ISM: molecules; ISM: individual objects: NGC 6334I ID INTERSTELLAR CLOUDS; MOLECULAR CLOUDS; GROUND-STATE; CH; SPECTROSCOPY; REGIONS; MODELS; ABUNDANCES; NGC-6334; I(N) AB Context. In contrast to the more extensively studied dense star-forming cores, little is known about diffuse gas surrounding star-forming regions. Aims. We study the molecular gas in the Galactic high-mass star-forming region NGC 6334I, which contains diffuse, quiescent components that are inconspicuous in widely used molecular tracers such as CO. Methods. We present Herschel/HIFI observations of methylidyne (CH) toward NGC 6334I observed as part of the "Chemical HErschel Survey of Star forming regions" (CHESS) key program. HIFI resolves each of the six hyperfine components of the lowest rotational transition (J = 3/2-1/2) of CH, observed in both emission and absorption. Results. The CH emission features appear close to the systemic velocity of NGC 6334I, while its measured FWHM linewidth of 3 km s(-1) is smaller than previously observed in dense gas tracers such as NH3 and SiO. The CH abundance in the hot core is similar to 7 x 10(-11), two to three orders of magnitude lower than in diffuse clouds. While other studies find distinct outflows in, e. g., CO and H2O toward NGC 6334I, we do not detect any outflow signatures in CH. At least two redshifted components of cold absorbing material must be present at -3.0 and +6.5 km s(-1) to explain the absorption signatures. We derive a CH column density (N-CH) of 7 x 10(13) and 3 x 10(13) cm(-2) for these two absorbing clouds. We find evidence of two additional absorbing clouds at +8.0 and 0.0 km s(-1), both with N-CH approximate to 2 x 10(13) cm(-2). Turbulent linewidths for the four absorption components vary between 1.5 and 5.0 km s(-1) in FWHM. We constrain the physical properties and locations of the clouds by matching our CH absorbers with the absorption signatures seen in other molecular tracers. Conclusions. In the hot core, molecules such as H2O and CO trace gas that is heated and dynamically influenced by outflow activity, whereas the CH molecule traces more quiescent material. The four CH absorbing clouds have column densities and turbulent properties that are consistent with those of diffuse clouds: two are located in the direct surroundings of NGC 6334, and two are unrelated foreground clouds. Local density and dynamical effects influence the chemical composition of the physical components of NGC 6334, which causes some components to be seen in CH but not in other tracers, and vice versa. C1 [van der Wiel, M. H. D.; van der Tak, F. F. S.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [van der Wiel, M. H. D.; van der Tak, F. F. S.; Helmich, F.] SRON Netherlands Inst Space Res, Groningen, Netherlands. [Goldsmith, P. F.; Langer, W.; Pearson, J.; Yorke, H.; Samoska, L. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bergin, E. A.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Comito, C.; Schilke, P.; Rolffs, R.; Parise, B.; Wyrowski, F.] Max Planck Inst Radioastron, D-5300 Bonn, Germany. [Schilke, P.; Rolffs, R.] Univ Cologne, Inst Phys, Cologne, Germany. [Caux, E.; Bottinelli, S.; Coutens, A.; Demyk, K.; Klotz, A.; Vastel, C.; Walters, A.] Univ Toulouse 3, Ctr Etud Spatiale Rayonnements, F-31062 Toulouse, France. [Caux, E.; Bottinelli, S.; Coutens, A.; Demyk, K.; Klotz, A.; Vastel, C.; Walters, A.] CNRS INSU, UMR 5187, Toulouse, France. [Ceccarelli, C.; Bacmann, A.; Castets, A.; Crimier, N.; Hily-Blant, P.; Kahane, C.; Lefloch, B.; Maret, S.; Pacheco, S.] Univ Grenoble 1, CNRS, UMR 5571, Lab Astrophys Grenoble, Grenoble, France. [Ceccarelli, C.; Baudry, A.; Bacmann, A.; Castets, A.; Jacq, T.; Wakelam, V.] Univ Bordeaux, Lab Astrophys Bordeaux, Floirac, France. [Ceccarelli, C.; Baudry, A.; Bacmann, A.; Castets, A.; Jacq, T.; Wakelam, V.] CNRS INSU, UMR 5804, Floirac, France. [Herbst, E.] Ohio State Univ, Columbus, OH 43210 USA. [Benedettini, M.; Saraceno, P.] INAF Ist Fis Spazio Interplanetario, Rome, Italy. [Lord, S.; Boogert, A.] CALTECH, Infared Proc & Anal Ctr, Pasadena, CA 91109 USA. [Neufeld, D.] Johns Hopkins Univ, Baltimore, MD USA. [Cabrit, S.; Encrenaz, P.; Falgarone, E.; Gerin, M.; Hennebelle, P.; Pagani, L.; Salez, M.] UCP, UPMC, ENS,Lab Etud Rayonnement & Matiere Astrophys, OP,UMR CNRS INSU 8112, Paris, France. [Caselli, P.] Univ Leeds, Sch Phys & Astron, Leeds, W Yorkshire, England. [Cernicharo, J.; Crimier, N.] CSIC INTA, Ctr Astrobiol, Madrid, Spain. [Codella, C.; Lorenzani, A.] INAF Osservatorio Astrofis Arcetri, Florence, Italy. [Dominik, C.; Kama, M.] Univ Amsterdam, Astron Inst Anton Pannekoek, Amsterdam, Netherlands. [Dominik, C.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6525 ED Nijmegen, Netherlands. [Fuente, A.] IGN Observ Astron Nacl, Alcala De Henares, Spain. [Henning, T.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Melnick, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Nisini, B.] INAF Osservatorio Astron Roma, Monte Porzio Catone, Italy. [Schuster, K.] Inst Radio Astron Millimetr, Grenoble, France. [Viti, S.] Leiden Univ, Leiden Observ, Leiden, Netherlands. [Edwards, K.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [Teyssier, D.] ESA, European Space Astron Ctr, Madrid, Spain. RP van der Wiel, MHD (reprint author), Univ Groningen, Kapteyn Astron Inst, POB 800, NL-9700 AV Groningen, Netherlands. EM wiel@astro.rug.nl RI Coutens, Audrey/M-4533-2014; Fuente, Asuncion/G-1468-2016; Goldsmith, Paul/H-3159-2016; van der Wiel, Matthijs/M-4531-2014 OI Coutens, Audrey/0000-0003-1805-3920; Fuente, Asuncion/0000-0001-6317-6343; Lorenzani, Andrea/0000-0002-4685-3434; Wakelam, Valentine/0000-0001-9676-2605; Kama, Mihkel/0000-0003-0065-7267; Codella, Claudio/0000-0003-1514-3074; , Brunella Nisini/0000-0002-9190-0113; Maret, Sebastien/0000-0003-1104-4554; van der Wiel, Matthijs/0000-0002-4325-3011 NR 32 TC 13 Z9 13 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR L43 DI 10.1051/0004-6361/201015096 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900043 ER PT J AU Vastel, C Ceccarelli, C Caux, E Coutens, A Cernicharo, J Bottinelli, S Demyk, K Faure, A Wiesenfeld, L Scribano, Y Bacmann, A Hily-Blant, P Maret, S Walters, A Bergin, EA Blake, GA Castets, A Crimier, N Dominik, C Encrenaz, P Gerin, M Hennebelle, P Kahane, C Klotz, A Melnick, G Pagani, L Parise, B Schilke, P Wakelam, V Baudry, A Bell, T Benedettini, M Boogert, A Cabrit, S Caselli, P Codella, C Comito, C Falgarone, E Fuente, A Goldsmith, PF Helmich, F Henning, T Herbst, E Jacq, T Kama, M Langer, W Lefloch, B Lis, D Lord, S Lorenzani, A Neufeld, D Nisini, B Pacheco, S Pearson, J Phillips, T Salez, M Saraceno, P Schuster, K Tielens, X van der Tak, F van der Wiel, MHD Viti, S Wyrowski, F Yorke, H Cais, P Krieg, JM Olberg, M Ravera, L AF Vastel, C. Ceccarelli, C. Caux, E. Coutens, A. Cernicharo, J. Bottinelli, S. Demyk, K. Faure, A. Wiesenfeld, L. Scribano, Y. Bacmann, A. Hily-Blant, P. Maret, S. Walters, A. Bergin, E. A. Blake, G. A. Castets, A. Crimier, N. Dominik, C. Encrenaz, P. Gerin, M. Hennebelle, P. Kahane, C. Klotz, A. Melnick, G. Pagani, L. Parise, B. Schilke, P. Wakelam, V. Baudry, A. Bell, T. Benedettini, M. Boogert, A. Cabrit, S. Caselli, P. Codella, C. Comito, C. Falgarone, E. Fuente, A. Goldsmith, P. F. Helmich, F. Henning, T. Herbst, E. Jacq, T. Kama, M. Langer, W. Lefloch, B. Lis, D. Lord, S. Lorenzani, A. Neufeld, D. Nisini, B. Pacheco, S. Pearson, J. Phillips, T. Salez, M. Saraceno, P. Schuster, K. Tielens, X. van der Tak, F. van der Wiel, M. H. D. Viti, S. Wyrowski, F. Yorke, H. Cais, P. Krieg, J. M. Olberg, M. Ravera, L. TI Ortho-to-para ratio of interstellar heavy water SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE astrochemistry; ISM: molecules; submillimeter: ISM; ISM: abundances; molecular processes; line: identification ID PROTOSTAR IRAS 16293-2422; SPECTROSCOPY; CONSTRAINTS; ENVELOPE AB Context. Despite the low elemental deuterium abundance in the Galaxy, enhanced molecular D/H ratios have been found in the environments of low-mass star-forming regions, and in particular the Class 0 protostar IRAS 16293-2422. Aims. The CHESS (Chemical HErschel Surveys of Star forming regions) key program aims to study the molecular complexity of the interstellar medium. The high sensitivity and spectral resolution of the Herschel/HIFI instrument provide a unique opportunity to observe the fundamental 1(1,1)-0(0,0) transition of the ortho-D2O molecule, which is inaccessible from the ground, and determine the ortho-to-para D2O ratio. Methods. We detected the fundamental transition of the ortho-D2O molecule at 607.35 GHz towards IRAS 16293-2422. The line is seen in absorption with a line opacity of 0.62 +/- 0.11 (1 sigma). From the previous ground-based observations of the fundamental 1(1,0)-1(0,1) transition of para-D2O seen in absorption at 316.80 GHz, we estimate a line opacity of 0.26 +/- 0.05 (1 sigma). Results. We show that the observed absorption is caused by the cold gas in the envelope of the protostar. Using these new observations, we estimate for the first time the ortho-to-para D2O ratio to be lower than 2.6 at a 3 sigma level of uncertainty, which should be compared with the thermal equilibrium value of 2:1. C1 [Vastel, C.; Caux, E.; Coutens, A.; Bottinelli, S.; Demyk, K.; Walters, A.; Klotz, A.; Ravera, L.] Univ Toulouse 3, Ctr Etud Spatiale Rayonnements, F-31062 Toulouse, France. [Vastel, C.; Caux, E.; Coutens, A.; Bottinelli, S.; Demyk, K.; Walters, A.; Klotz, A.; Ravera, L.] CNRS INSU, UMR 5187, Toulouse, France. [Ceccarelli, C.; Faure, A.; Wiesenfeld, L.; Bacmann, A.; Hily-Blant, P.; Maret, S.; Castets, A.; Crimier, N.; Kahane, C.; Lefloch, B.; Pacheco, S.] Univ Grenoble 1, CNRS, UMR 5571, Lab Astrophys Grenoble, Grenoble, France. [Ceccarelli, C.; Bacmann, A.; Castets, A.; Wakelam, V.; Baudry, A.; Jacq, T.; Cais, P.] Univ Bordeaux, Lab Astrophys Bordeaux, Floirac, France. [Ceccarelli, C.; Bacmann, A.; Castets, A.; Wakelam, V.; Baudry, A.; Cais, P.] CNRS INSU, UMR 5804, Floirac, France. [Cernicharo, J.; Crimier, N.] CSIC INTA, Ctr Astrobiol, Madrid, Spain. [Scribano, Y.] CNRS, UMR 5209, Lab Interdisciplinaire Carnot Bourgogne, Dijon, France. [Bergin, E. A.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Boogert, A.; Lord, S.] CALTECH, Infared Proc & Anal Ctr, Pasadena, CA 91109 USA. [Dominik, C.; Kama, M.] Univ Amsterdam, Astron Inst Anton Pannekoek, Amsterdam, Netherlands. [Dominik, C.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6525 ED Nijmegen, Netherlands. [Encrenaz, P.; Gerin, M.; Hennebelle, P.; Pagani, L.; Cabrit, S.; Falgarone, E.; Salez, M.; Krieg, J. M.] UCP, UPMC, ENS,UMR CNRS INSU 8112, Lab Etudes Rayonnement & Matiere Astrophys,OP, Paris, France. [Melnick, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Parise, B.; Schilke, P.; Comito, C.; Wyrowski, F.] Max Planck Inst Radioastron, D-5300 Bonn, Germany. [Schilke, P.] Univ Cologne, Inst Phys, Cologne, Germany. [Benedettini, M.; Saraceno, P.] INAF Ist Fis Spazio Interplanetario, Rome, Italy. [Caselli, P.] Univ Leeds, Sch Phys & Astron, Leeds, W Yorkshire, England. [Codella, C.; Lorenzani, A.] INAF Osservatorio Astrofis Arcetri, Florence, Italy. [Fuente, A.] IGN Observ Astron Nacl, Alcala De Henares, Spain. [Goldsmith, P. F.; Langer, W.; Pearson, J.; Yorke, H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Helmich, F.; van der Tak, F.; van der Wiel, M. H. D.; Olberg, M.] SRON Netherlands Inst Space Res, Groningen, Netherlands. [Henning, T.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Neufeld, D.] Ohio State Univ, Columbus, OH 43210 USA. [Nisini, B.] INAF Osservatorio Astron Roma, Monte Porzio Catone, Italy. [Schuster, K.] Inst Radio Astron Millimetr, Grenoble, France. [Tielens, X.] Leiden Univ, Leiden Observ, Leiden, Netherlands. [van der Tak, F.; van der Wiel, M. H. D.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AB Groningen, Netherlands. [Viti, S.] UCL, Dept Phys & Astron, London, England. [Olberg, M.] Chalmers, Goterborg, Sweden. RP Vastel, C (reprint author), Univ Toulouse 3, Ctr Etud Spatiale Rayonnements, F-31062 Toulouse, France. EM vastel@cesr.fr RI van der Wiel, Matthijs/M-4531-2014; Coutens, Audrey/M-4533-2014; Fuente, Asuncion/G-1468-2016; Goldsmith, Paul/H-3159-2016; OI van der Wiel, Matthijs/0000-0002-4325-3011; Coutens, Audrey/0000-0003-1805-3920; Fuente, Asuncion/0000-0001-6317-6343; Lorenzani, Andrea/0000-0002-4685-3434; Wakelam, Valentine/0000-0001-9676-2605; Kama, Mihkel/0000-0003-0065-7267; Codella, Claudio/0000-0003-1514-3074; , Brunella Nisini/0000-0002-9190-0113; Maret, Sebastien/0000-0003-1104-4554 NR 21 TC 29 Z9 29 U1 1 U2 7 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR L31 DI 10.1051/0004-6361/201015101 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900031 ER PT J AU Wampfler, SF Herczeg, GJ Bruderer, S Benz, AO van Dishoeck, EF Kristensen, LE Visser, R Doty, SD Melchior, M van Kempen, TA Yildiz, UA Dedes, C Goicoechea, JR Baudry, A Melnick, G Bachiller, R Benedettini, M Bergin, E Bjerkeli, P Blake, GA Bontemps, S Braine, J Caselli, P Cernicharo, J Codella, C Daniel, F di Giorgio, AM Dominik, C Encrenaz, P Fich, M Fuente, A Giannini, T de Graauw, T Helmich, F Herpin, F Hogerheijde, MR Jacq, T Johnstone, D Jorgensen, JK Larsson, B Lis, D Liseau, R Marseille, M Mc Coey, C Neufeld, D Nisini, B Olberg, M Parise, B Pearson, JC Plume, R Risacher, C Santiago-Garcia, J Saraceno, P Shipman, R Tafalla, M van der Tak, FFS Wyrowski, F Roelfsema, P Jellema, W Dieleman, P Caux, E Stutzki, J AF Wampfler, S. F. Herczeg, G. J. Bruderer, S. Benz, A. O. van Dishoeck, E. F. Kristensen, L. E. Visser, R. Doty, S. D. Melchior, M. van Kempen, T. A. Yildiz, U. A. Dedes, C. Goicoechea, J. R. Baudry, A. Melnick, G. Bachiller, R. Benedettini, M. Bergin, E. Bjerkeli, P. Blake, G. A. Bontemps, S. Braine, J. Caselli, P. Cernicharo, J. Codella, C. Daniel, F. di Giorgio, A. M. Dominik, C. Encrenaz, P. Fich, M. Fuente, A. Giannini, T. de Graauw, Th. Helmich, F. Herpin, F. Hogerheijde, M. R. Jacq, T. Johnstone, D. Jorgensen, J. K. Larsson, B. Lis, D. Liseau, R. Marseille, M. Mc Coey, C. Neufeld, D. Nisini, B. Olberg, M. Parise, B. Pearson, J. C. Plume, R. Risacher, C. Santiago-Garcia, J. Saraceno, P. Shipman, R. Tafalla, M. van der Tak, F. F. S. Wyrowski, F. Roelfsema, P. Jellema, W. Dieleman, P. Caux, E. Stutzki, J. TI Herschel observations of the hydroxyl radical (OH) in young stellar objects SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE astrochemistry; stars: formation; ISM: molecules; ISM: jets and outflows; ISM: individual objects: HH 46 ID PHYSICAL STRUCTURE; PACS SPECTROSCOPY; MOLECULAR CLOUD; MASS PROTOSTARS; CLASS-0 SOURCES; CO OBSERVATIONS; FIRS 2; HH 46; EMISSION; PHOTODISSOCIATION AB Aims. "Water In Star-forming regions with Herschel" (WISH) is a Herschel key program investigating the water chemistry in young stellar objects (YSOs) during protostellar evolution. Hydroxyl (OH) is one of the reactants in the chemical network most closely linked to the formation and destruction of H2O. High-temperature (T greater than or similar to 250 K) chemistry connects OH and H2O through the OH + H-2 double left right arrow H2O + H reactions. Formation of H2O from OH is efficient in the high-temperature regime found in shocks and the innermost part of protostellar envelopes. Moreover, in the presence of UV photons, OH can be produced from the photo-dissociation of H2O through H2O + gamma(UV) double right arrow OH + H. Methods. High-resolution spectroscopy of the 163.12 mu m triplet of OH towards HH 46 and NGC 1333 IRAS 2A was carried out with the Heterodyne Instrument for the Far Infrared (HIFI) on board the Herschel Space Observatory. The low-and intermediate-mass protostars HH 46, TMR 1, IRAS 15398-3359, DK Cha, NGC 7129 FIRS 2, and NGC 1333 IRAS 2A were observed with the Photodetector Array Camera and Spectrometer (PACS) on Herschel in four transitions of OH and two [OI] lines. Results. The OH transitions at 79, 84, 119, and 163 mu m and [OI] emission at 63 and 145 mu m were detected with PACS towards the class I low-mass YSOs as well as the intermediate-mass and class I Herbig Ae sources. No OH emission was detected from the class 0 YSO NGC 1333 IRAS 2A, though the 119 mu m was detected in absorption. With HIFI, the 163.12 mu m was not detected from HH 46 and only tentatively detected from NGC 1333 IRAS 2A. The combination of the PACS and HIFI results for HH 46 constrains the line width (FWHM greater than or similar to 11 km s(-1)) and indicates that the OH emission likely originates from shocked gas. This scenario is supported by trends of the OH flux increasing with the [OI] flux and the bolometric luminosity, as found in our sample. Similar OH line ratios for most sources suggest that OH has comparable excitation temperatures despite the different physical properties of the sources. C1 [Wampfler, S. F.; Bruderer, S.; Benz, A. O.; Melchior, M.; Dedes, C.] ETH, Inst Astron, CH-8093 Zurich, Switzerland. [Herczeg, G. J.; van Dishoeck, E. F.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [van Dishoeck, E. F.; Kristensen, L. E.; Visser, R.; Yildiz, U. A.; Hogerheijde, M. R.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Doty, S. D.] Denison Univ, Dept Phys & Astron, Granville, OH 43023 USA. [Melchior, M.] Univ Appl Sci NW, Inst Technol 4D, CH-5210 Windisch, Switzerland. [van Kempen, T. A.; Melnick, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Goicoechea, J. R.; Cernicharo, J.; Daniel, F.] CSIC INTA, Dept Astrofis, Ctr Astrobiol, Madrid 28850, Spain. [Baudry, A.; Bontemps, S.; Braine, J.; Herpin, F.; Jacq, T.] Univ Bordeaux, Lab Astrophys Bordeaux, Bordeaux, France. [Baudry, A.; Bontemps, S.; Braine, J.; Herpin, F.; Jacq, T.] CNRS INSU, UMR 5804, Floirac, France. [Bachiller, R.; Tafalla, M.] Observ Astron Nacl IGN, Madrid 28014, Spain. [Benedettini, M.; di Giorgio, A. M.; Saraceno, P.] INAF Ist Fis Spazio Interplanetario, Area Ric Tor Vergata, I-00133 Rome, Italy. [Bergin, E.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Bjerkeli, P.; Liseau, R.; Olberg, M.] Chalmers, Onsala Space Observ, Dept Radio & Space Sci, S-43992 Onsala, Sweden. [Blake, G. A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Caselli, P.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Caselli, P.; Codella, C.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Dominik, C.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. [Dominik, C.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands. [Encrenaz, P.] Observ Paris, LERMA, F-75014 Paris, France. [Encrenaz, P.] Observ Paris, CNRS, UMR 8112, F-75014 Paris, France. [Fich, M.; Mc Coey, C.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [Fuente, A.] Observ Astron Nacl, Alcala De Henares 28803, Spain. [Giannini, T.; Nisini, B.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy. [de Graauw, Th.; Helmich, F.; Marseille, M.; Risacher, C.; Shipman, R.; van der Tak, F. F. S.; Roelfsema, P.; Jellema, W.; Dieleman, P.] SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [Johnstone, D.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Johnstone, D.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 1A1, Canada. [Jorgensen, J. K.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen K, Denmark. [Larsson, B.] Stockholm Univ, Dept Astron, S-10691 Stockholm, Sweden. [Lis, D.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Mc Coey, C.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [Neufeld, D.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Parise, B.; Wyrowski, F.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Pearson, J. C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Plume, R.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Santiago-Garcia, J.] IRAM, E-18012 Granada, Spain. [van der Tak, F. F. S.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Caux, E.] Univ Toulouse UPS, Ctr Etud Spatiale Rayonnements, F-31062 Toulouse 9, France. [Caux, E.] CNRS INSU, UMR 5187, F-31028 Toulouse 4, France. [Stutzki, J.] Univ Cologne, Inst Phys 1, KOSMA, D-50937 Cologne, Germany. RP Wampfler, SF (reprint author), ETH, Inst Astron, CH-8093 Zurich, Switzerland. EM wsusanne@astro.phys.ethz.ch RI Kristensen, Lars/F-4774-2011; Visser, Ruud/J-8574-2012; Jorgensen, Jes Kristian/L-7936-2014; Wampfler, Susanne/D-2270-2015; Fuente, Asuncion/G-1468-2016; Yildiz, Umut/C-5257-2011; OI Kristensen, Lars/0000-0003-1159-3721; Jorgensen, Jes Kristian/0000-0001-9133-8047; Wampfler, Susanne/0000-0002-3151-7657; Fuente, Asuncion/0000-0001-6317-6343; Bjerkeli, Per/0000-0002-7993-4118; Codella, Claudio/0000-0003-1514-3074; Yildiz, Umut/0000-0001-6197-2864; Giannini, Teresa/0000-0002-0224-096X; , Brunella Nisini/0000-0002-9190-0113 FU Swiss National Science Foundation [200020-113556] FX The work on star formation at ETH Zurich is partially funded by the Swiss National Science Foundation (grant nr. 200020-113556). This program is made possible thanks to the Swiss HIFI guaranteed time program. HIFI has been designed and built by a consortium of institutes and university departments from across Europe, Canada and the United States under the leadership of SRON Netherlands Institute for Space Research, Groningen, The Netherlands and with major contributions from Germany, France and the US. Consortium members are: Canada: CSA, U. Waterloo; France: CESR, LAB, LERMA, IRAM; Germany: KOSMA, MPIfR, MPS; Ireland, NUI Maynooth; Italy: ASI, IFSI-INAF, Osservatorio Astrofisico di Arcetri-INAF; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio 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, JPL, NHSC. NR 35 TC 23 Z9 23 U1 0 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 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR L36 DI 10.1051/0004-6361/201015112 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900036 ER PT J AU Wyrowski, F van der Tak, F Herpin, F Baudry, A Bontemps, S Chavarria, L Frieswijk, W Jacq, T Marseille, M Shipman, R van Dishoeck, EF Benz, AO Caselli, P Hogerheijde, MR Johnstone, D Liseau, R Bachiller, R Benedettini, M Bergin, E Bjerkeli, P Blake, G Braine, J Bruderer, S Cernicharo, J Codella, C Daniel, F di Giorgio, AM Dominik, C Doty, SD Encrenaz, P Fich, M Fuente, A Giannini, T Goicoechea, JR de Graauw, T Helmich, F Herczeg, GJ Jorgensen, JK Kristensen, LE Larsson, B Lis, D McCoey, C Melnick, G Nisini, B Olberg, M Parise, B Pearson, JC Plume, R Risacher, C Santiago, J Saraceno, P Tafalla, M van Kempen, TA Visser, R Wampfler, S Yildiz, UA Black, JH Falgarone, E Gerin, M Roelfsema, P Dieleman, P Beintema, D De Jonge, A Whyborn, N Stutzki, J Ossenkopf, V AF Wyrowski, F. van der Tak, F. Herpin, F. Baudry, A. Bontemps, S. Chavarria, L. Frieswijk, W. Jacq, T. Marseille, M. Shipman, R. van Dishoeck, E. F. Benz, A. O. Caselli, P. Hogerheijde, M. R. Johnstone, D. Liseau, R. Bachiller, R. Benedettini, M. Bergin, E. Bjerkeli, P. Blake, G. Braine, J. Bruderer, S. Cernicharo, J. Codella, C. Daniel, F. di Giorgio, A. M. Dominik, C. Doty, S. D. Encrenaz, P. Fich, M. Fuente, A. Giannini, T. Goicoechea, J. R. de Graauw, Th. Helmich, F. Herczeg, G. J. Jorgensen, J. K. Kristensen, L. E. Larsson, B. Lis, D. McCoey, C. Melnick, G. Nisini, B. Olberg, M. Parise, B. Pearson, J. C. Plume, R. Risacher, C. Santiago, J. Saraceno, P. Tafalla, M. van Kempen, T. A. Visser, R. Wampfler, S. Yildiz, U. A. Black, J. H. Falgarone, E. Gerin, M. Roelfsema, P. Dieleman, P. Beintema, D. De Jonge, A. Whyborn, N. Stutzki, J. Ossenkopf, V. TI Variations in H2O+/H2O ratios toward massive star-forming regions SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: clouds; ISM: molecules; submillimeter: ISM; stars: formation ID LASER MAGNETIC-RESONANCE; LINE; ASTRONOMY; CHEMISTRY; SIGHT; DR21; HIFI; W51 AB Early results from the Herschel Space Observatory revealed the water cation H2O+ to be an abundant ingredient of the interstellar medium. Here we present new observations of the H2O and H2O+ lines at 1113.3 and 1115.2 GHz using the Herschel Space Observatory toward a sample of high-mass star-forming regions to observationally study the relation between H2O and H2O+. Nine out of ten sources show absorption from H2O+ in a range of environments: the molecular clumps surrounding the forming and newly formed massive stars, bright high-velocity outflows associated with the massive protostars, and unrelated low-density clouds along the line of sight. Column densities per velocity component of H2O+ are found in the range of 10(12) to a few 10(13) cm(-2). The highest N(H2O+) column densities are found in the outflows of the sources. The ratios of H2O+/H2O are determined in a range from 0.01 to a few and are found to differ strongly between the observed environments with much lower ratios in the massive (proto) cluster envelopes (0.01-0.1) than in outflows and diffuse clouds. Remarkably, even for source components detected in H2O in emission, H2O+ is still seen in absorption. C1 [Wyrowski, F.; Parise, B.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [van der Tak, F.; Marseille, M.; Shipman, R.; Helmich, F.; Dieleman, P.; Beintema, D.; De Jonge, A.] SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [van der Tak, F.; Frieswijk, W.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Herpin, F.; Baudry, A.; Bontemps, S.; Chavarria, L.; Jacq, T.; Braine, J.] Univ Bordeaux, Lab Astrophys Bordeaux, Bordeaux, France. [Herpin, F.; Baudry, A.; Bontemps, S.; Chavarria, L.; Jacq, T.; Braine, J.] CNRS INSU, UMR 5804, Floirac, France. [van Dishoeck, E. F.; Herczeg, G. J.] Max Planck Inst Extraterestr Phys, Garching, Germany. [van Dishoeck, E. F.; Hogerheijde, M. R.; Visser, R.; Yildiz, U. A.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Benz, A. O.; Bruderer, S.; Wampfler, S.] ETH, Inst Astron, CH-8093 Zurich, Switzerland. [Caselli, P.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Johnstone, D.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Johnstone, D.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 1A1, Canada. [Liseau, R.; Bjerkeli, P.; Olberg, M.; Black, J. H.] Chalmers, Onsala Space Observ, Dept Radio & Space Sci, S-43992 Onsala, Sweden. [Bachiller, R.; Fuente, A.; Santiago, J.; Tafalla, M.] IGN Observ Astron Nacl, Alcala De Henares 28800, Spain. [Benedettini, M.; Codella, C.; di Giorgio, A. M.; Giannini, T.; Nisini, B.; Saraceno, P.] INAF Ist Fis Spazio Interplanetario, Area Ric Tor Vergata, I-00133 Rome, Italy. [Benedettini, M.; Bergin, E.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Blake, G.; Lis, D.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Cernicharo, J.; Goicoechea, J. R.] INTA CSIC, CAB, Dept Astrophys, Torrejon De Ardoz 28850, Spain. [Daniel, F.; Falgarone, E.; Gerin, M.] Observ Paris, LERMA UMR CNRS 8112, F-92195 Meudon, France. [Daniel, F.] CSIC, Dept Mol & Infrared Astrophys, E-28006 Madrid, Spain. [Dominik, C.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. [Doty, S. D.] Denison Univ, Dept Phys & Astron, Granville, OH 43023 USA. [Encrenaz, P.] Observ Paris, LERMA, F-75014 Paris, France. [Encrenaz, P.] Observ Paris, CNRS, UMR 8112, F-75014 Paris, France. [Fich, M.; McCoey, C.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [de Graauw, Th.; Whyborn, N.] Joint ALMA Off, Santiago, Chile. [Jorgensen, J. K.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark. [Larsson, B.] Stockholm Univ, Dept Astron, S-10691 Stockholm, Sweden. [Melnick, G.; van Kempen, T. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Pearson, J. C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Plume, R.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Stutzki, J.; Ossenkopf, V.] Univ Cologne, Inst Phys, D-50937 Cologne, Germany. RP Wyrowski, F (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. EM wyrowski@mpifr-bonn.mpg.de RI Yildiz, Umut/C-5257-2011; Kristensen, Lars/F-4774-2011; Visser, Ruud/J-8574-2012; Jorgensen, Jes Kristian/L-7936-2014; Wampfler, Susanne/D-2270-2015; Fuente, Asuncion/G-1468-2016; OI Yildiz, Umut/0000-0001-6197-2864; Kristensen, Lars/0000-0003-1159-3721; Jorgensen, Jes Kristian/0000-0001-9133-8047; Wampfler, Susanne/0000-0002-3151-7657; Fuente, Asuncion/0000-0001-6317-6343; Bjerkeli, Per/0000-0002-7993-4118; Codella, Claudio/0000-0003-1514-3074; Giannini, Teresa/0000-0002-0224-096X; , Brunella Nisini/0000-0002-9190-0113 NR 20 TC 22 Z9 22 U1 0 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR L34 DI 10.1051/0004-6361/201015110 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900034 ER PT J AU Yildiz, UA van Dishoeck, EF Kristensen, LE Visser, R Jorgensen, JK Herczeg, GJ van Kempen, TA Hogerheijde, MR Doty, SD Benz, AO Bruderer, S Wampfler, SF Deul, E Bachiller, R Baudry, A Benedettini, M Bergin, E Bjerkeli, P Blake, GA Bontemps, S Braine, J Caselli, P Cernicharo, J Codella, C Daniel, F di Giorgio, AM Dominik, C Encrenaz, P Fich, M Fuente, A Giannini, T Goicoechea, JR de Graauw, T Helmich, F Herpin, F Jacq, T Johnstone, D Larsson, B Lis, D Liseau, R Liu, FC Marseille, M McCoey, C Melnick, G Neufeld, D Nisini, B Olberg, M Parise, B Pearson, JC Plume, R Risacher, C Santiago-Garcia, J Saraceno, P Shipman, R Tafalla, M Tielens, AGGM van der Tak, F Wyrowski, F Dieleman, P Jellema, W Ossenkopf, V Schieder, R Stutzki, J AF Yildiz, U. A. van Dishoeck, E. F. Kristensen, L. E. Visser, R. Jorgensen, J. K. Herczeg, G. J. van Kempen, T. A. Hogerheijde, M. R. Doty, S. D. Benz, A. O. Bruderer, S. Wampfler, S. F. Deul, E. Bachiller, R. Baudry, A. Benedettini, M. Bergin, E. Bjerkeli, P. Blake, G. A. Bontemps, S. Braine, J. Caselli, P. Cernicharo, J. Codella, C. Daniel, F. di Giorgio, A. M. Dominik, C. Encrenaz, P. Fich, M. Fuente, A. Giannini, T. Goicoechea, J. R. de Graauw, Th. Helmich, F. Herpin, F. Jacq, T. Johnstone, D. Larsson, B. Lis, D. Liseau, R. Liu, F. -C. Marseille, M. McCoey, C. Melnick, G. Neufeld, D. Nisini, B. Olberg, M. Parise, B. Pearson, J. C. Plume, R. Risacher, C. Santiago-Garcia, J. Saraceno, P. Shipman, R. Tafalla, M. Tielens, A. G. G. M. van der Tak, F. Wyrowski, F. Dieleman, P. Jellema, W. Ossenkopf, V. Schieder, R. Stutzki, J. TI Herschel/HIFI observations of high-J CO lines in the NGC 1333 low-mass star-forming region SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE astrochemistry; stars: formation; ISM: jets and outflows; ISM: molecules ID NGC-1333 IRAS-4; DENSE CORES; PROTOSTARS; ENVELOPES; ABUNDANCE; H2CO; EVOLUTION; WATER; DUST; HIFI AB Herschel/HIFI observations of high-J lines (up to J(u) = 10) of (CO)-C-12, (CO)-C-13 and (CO)-O-18 are presented toward three deeply embedded low-mass protostars, NGC 1333 IRAS 2A, IRAS 4A, and IRAS 4B, obtained as part of the Water In Star-forming regions with Herschel (WISH) key program. The spectrally-resolved HIFI data are complemented by ground-based observations of lower-J CO and isotopologue lines. The (CO)-C-12 10-9 profiles are dominated by broad (FWHM 25-30 km s(-1)) emission. Radiative transfer models are used to constrain the temperature of this shocked gas to 100-200 K. Several CO and (CO)-C-13 line profiles also reveal a medium-broad component (FWHM5-10 km s(-1)), seen prominently in H2O lines. Column densities for both components are presented, providing a reference for determining abundances of other molecules in the same gas. The narrow (CO)-O-18 9-8 lines probe the warmer part of the quiescent envelope. Their intensities require a jump in the CO abundance at an evaporation temperature around 25 K, thus providing new direct evidence for a CO ice evaporation zone around low-mass protostars. C1 [Yildiz, U. A.; van Dishoeck, E. F.; Kristensen, L. E.; Visser, R.; van Kempen, T. A.; Hogerheijde, M. R.; Deul, E.; Tielens, A. G. G. M.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [van Dishoeck, E. F.; Herczeg, G. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Jorgensen, J. K.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen K, Denmark. [van Kempen, T. A.; Melnick, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Doty, S. D.] Denison Univ, Dept Phys & Astron, Granville, OH 43023 USA. [Benz, A. O.; Bruderer, S.; Wampfler, S. F.] ETH, Inst Astron, CH-8093 Zurich, Switzerland. [Bachiller, R.; Tafalla, M.] Observ Astron Nacl IGN, Madrid 28014, Spain. [Baudry, A.; Bontemps, S.; Braine, J.; Herpin, F.; Jacq, T.] Univ Bordeaux, Lab Astrophys Bordeaux, Bordeaux, France. [Baudry, A.; Bontemps, S.; Braine, J.; Herpin, F.; Jacq, T.] CNRS INSU, UMR 5804, Floirac, France. [Benedettini, M.; di Giorgio, A. M.; Saraceno, P.] INAF Ist Fis Spazio Interplanetario, Area Ric Tor Vergata, I-00133 Rome, Italy. [Bergin, E.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Bjerkeli, P.; Liseau, R.; Olberg, M.] Chalmers, Onsala Space Observ, Dept Radio & Space Sci, S-43992 Onsala, Sweden. [Blake, G. A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Caselli, P.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Caselli, P.; Codella, C.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Cernicharo, J.; Daniel, F.; Goicoechea, J. R.] CSIC INTA, Ctr Astrobiol, Dept Astrofis, Madrid 28850, Spain. [Dominik, C.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. [Dominik, C.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands. [Encrenaz, P.] Observ Paris, LERMA, F-75014 Paris, France. [Encrenaz, P.] Observ Paris, CNRS, UMR 8112, F-75014 Paris, France. [Fich, M.; McCoey, C.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [Fuente, A.] Observ Astron Nacl, Alcala De Henares 28803, Spain. [Giannini, T.; Nisini, B.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy. [de Graauw, Th.; Helmich, F.; Marseille, M.; Risacher, C.; Shipman, R.; van der Tak, F.; Dieleman, P.; Jellema, W.] SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [Johnstone, D.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Johnstone, D.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 1A1, Canada. [Larsson, B.] Stockholm Univ, Dept Astron, S-10691 Stockholm, Sweden. [Lis, D.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Liu, F. -C.; Parise, B.; Wyrowski, F.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Neufeld, D.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [Pearson, J. C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Plume, R.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Santiago-Garcia, J.] IRAM, E-18012 Granada, Spain. [van der Tak, F.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Ossenkopf, V.; Schieder, R.; Stutzki, J.] Univ Cologne, Inst Phys 1, KOSMA, D-50937 Cologne, Germany. RP Yildiz, UA (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. EM yildiz@strw.leidenuniv.nl RI Jorgensen, Jes Kristian/L-7936-2014; Wampfler, Susanne/D-2270-2015; Fuente, Asuncion/G-1468-2016; Yildiz, Umut/C-5257-2011; Kristensen, Lars/F-4774-2011; Visser, Ruud/J-8574-2012; OI Jorgensen, Jes Kristian/0000-0001-9133-8047; Wampfler, Susanne/0000-0002-3151-7657; Fuente, Asuncion/0000-0001-6317-6343; Bjerkeli, Per/0000-0002-7993-4118; Codella, Claudio/0000-0003-1514-3074; Yildiz, Umut/0000-0001-6197-2864; Kristensen, Lars/0000-0003-1159-3721; Giannini, Teresa/0000-0002-0224-096X; , Brunella Nisini/0000-0002-9190-0113 NR 31 TC 38 Z9 38 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 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR L40 DI 10.1051/0004-6361/201015119 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900040 ER PT J AU Dunham, MM Evans, NJ Bourke, TL Myers, PC Huard, TL Stutz, AM AF Dunham, Michael M. Evans, Neal J. Bourke, Tyler L. Myers, Philip C. Huard, Tracy L. Stutz, Amelia M. TI THE SPITZER c2d SURVEY OF NEARBY DENSE CORES. IX. DISCOVERY OF A VERY LOW LUMINOSITY OBJECT DRIVING A MOLECULAR OUTFLOW IN THE DENSE CORE L673-7 SO ASTROPHYSICAL JOURNAL LA English DT Article DE brown dwarfs; ISM: individual objects (L673-7); stars: formation; stars: low-mass ID YOUNG STELLAR OBJECTS; SPECTRAL ENERGY-DISTRIBUTIONS; MULTIBAND IMAGING PHOTOMETER; MASS STAR-FORMATION; T-TAURI STARS; BIPOLAR FLOWS; PROTOSTELLAR ACCRETION; SPACE-TELESCOPE; EMBEDDED SOURCE; LINE FORMATION AB We present new infrared, submillimeter, and millimeter observations of the dense core L673-7 and report the discovery of a low-luminosity, embedded Class 0 protostar driving a molecular outflow. L673-7 is seen in absorption against the mid-infrared background in 5.8, 8, and 24 mu m Spitzer images, allowing for a derivation of the column density profile and total enclosed mass of L673-7, independent of dust temperature assumptions. Estimates of the core mass from these absorption profiles range from 0.2 to 4.5M(circle dot). Millimeter continuum emission indicates a mass of similar to 2M(circle dot), both from a direct calculation assuming isothermal dust and from dust radiative transfer models constrained by the millimeter observations. We use dust radiative transfer models to constrain the internal luminosity of L673-7, defined to be the luminosity of the central source and excluding the luminosity from external heating, to be L-int = 0.01-0.045L(circle dot), with L-int similar to 0.04L(circle dot) the most likely value. L673-7 is thus classified as a very low luminosity object (VeLLO), and is among the lowest luminosity VeLLOs yet studied. We calculate the kinematic and dynamic properties of the molecular outflow in the standard manner. From the outflow properties and standard assumptions regarding the driving of outflows, we calculate the time-averaged protostellar mass accretion rate, total protostellar mass accreted, and expected accretion luminosity to be < M-acc > >= 1.2 x 10(-6) sin i/cos(2) i M-circle dot yr(-1), M-acc >= 0.07 1/cos i M-circle dot, and L-acc >= 0.36L(circle dot), respectively. The discrepancy between this calculated L-acc and the L-int derived from dust radiative transfer models indicates that the current accretion rate is much lower than the average rate over the lifetime of the outflow. Although the protostar embedded within L673-7 is consistent with currently being substellar, it is unlikely to remain as such given the substantial mass reservoir remaining in the core. C1 [Dunham, Michael M.; Evans, Neal J.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Bourke, Tyler L.; Myers, Philip C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Huard, Tracy L.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Stutz, Amelia M.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Stutz, Amelia M.] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. [Stutz, Amelia M.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Dunham, MM (reprint author), Univ Texas Austin, Dept Astron, 1 Univ Stn,C1400, Austin, TX 78712 USA. EM mdunham@astro.as.utexas.edu OI Stutz, Amelia/0000-0003-2300-8200 FU NASA [1224608, 1288664, 1288658, RSA 1377304, NNX 07-AJ72G, 1279198, 1288806]; NSF [AST-0607793]; UT Austin University FX This work is based partly on observations obtained with the Spitzer Space Telescope, operated by the Jet Propulsion Laboratory, California Institute of Technology, and the Caltech Submillimeter Observatory. The authors gratefully acknowledge the assistance of Miranda Dunham in obtaining the CSO 12CO J = 2-1 data, and that of Miwa Block of the MIPS instrument team at Steward Observatory with data reduction. We thank Cornelis Dullemond for reading a draft of this work and providing helpful comments, Jes Jorgensen for his IDL scripts to display three-color images, and the Lorentz Center in Leiden for hosting several meetings that contributed to this paper. This research has made use of NASA's Astrophysics Data System (ADS) Abstract Service and of the SIMBAD database, operated at CDS, Strasbourg, France. Support for this work, part of the Spitzer Legacy Science Program, was provided by NASA through contracts 1224608, 1288664, 1288658, and RSA 1377304. Support was also provided by NASA Origins grant NNX 07-AJ72G and NSF grant AST-0607793. M. M. D. acknowledges partial support from a UT Austin University Continuing Fellowship. Partial support for T. L. B. was provided by NASA through contracts 1279198 and 1288806 issued by the Jet Propulsion Laboratory, California Institute of Technology, to the Smithsonian Astronomical Observatory. NR 108 TC 28 Z9 28 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2010 VL 721 IS 2 BP 995 EP 1013 DI 10.1088/0004-637X/721/2/995 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 654TP UT WOS:000282193600007 ER PT J AU MacLeod, CL Ivezic, Z Kochanek, CS Kozlowski, S Kelly, B Bullock, E Kimball, A Sesar, B Westman, D Brooks, K Gibson, R Becker, AC de Vries, WH AF MacLeod, C. L. Ivezic, Z. Kochanek, C. S. Kozlowski, S. Kelly, B. Bullock, E. Kimball, A. Sesar, B. Westman, D. Brooks, K. Gibson, R. Becker, A. C. de Vries, W. H. TI MODELING THE TIME VARIABILITY OF SDSS STRIPE 82 QUASARS AS A DAMPED RANDOM WALK SO ASTROPHYSICAL JOURNAL LA English DT Article DE quasars: general ID DIGITAL SKY SURVEY; ACTIVE GALACTIC NUCLEI; BLACK-HOLE MASSES; X-RAY VARIABILITY; OPTICAL VARIABILITY; CONTINUUM VARIABILITY; SPECTRAL VARIABILITY; EDDINGTON RATIO; STELLAR OBJECTS; ACCRETION DISC AB We model the time variability of similar to 9000 spectroscopically confirmed quasars in SDSS Stripe 82 as a damped random walk (DRW). Using 2.7 million photometric measurements collected over 10 yr, we confirm the results of Kelly et al. and Kozlowski et al. that this model can explain quasar light curves at an impressive fidelity level (0.01-0.02 mag). The DRW model provides a simple, fast (O(N) for N data points), and powerful statistical description of quasar light curves by a characteristic timescale (tau) and an asymptotic rms variability on long timescales (SF infinity). We searched for correlations between these two variability parameters and physical parameters such as luminosity and black hole mass, and rest-frame wavelength. Our analysis shows SF infinity to increase with decreasing luminosity and rest-frame wavelength as observed previously, and without a correlation with redshift. We find a correlation between SF infinity and black hole mass with a power-law index of 0.18 +/- 0.03, independent of the anti-correlation with luminosity. We find that t increases with increasing wavelength with a power-law index of 0.17, remains nearly constant with redshift and luminosity, and increases with increasing black hole mass with a power-law index of 0.21 +/- 0.07. The amplitude of variability is anti-correlated with the Eddington ratio, which suggests a scenario where optical fluctuations are tied to variations in the accretion rate. However, we find an additional dependence on luminosity and/or black hole mass that cannot be explained by the trend with Eddington ratio. The radio-loudest quasars have systematically larger variability amplitudes by about 30%, when corrected for the other observed trends, while the distribution of their characteristic timescale is indistinguishable from that of the full sample. We do not detect any statistically robust differences in the characteristic timescale and variability amplitude between the full sample and the small subsample of quasars detected by ROSAT. Our results provide a simple quantitative framework for generating mock quasar light curves, such as currently used in LSST image simulations. C1 [MacLeod, C. L.; Ivezic, Z.; Bullock, E.; Kimball, A.; Sesar, B.; Westman, D.; Brooks, K.; Gibson, R.; Becker, A. C.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Kochanek, C. S.; Kozlowski, S.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Kochanek, C. S.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Kelly, B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Westman, D.] James Cook Univ, Ctr Astron, Townsville, Qld 4811, Australia. [de Vries, W. H.] Univ Calif Davis, Davis, CA 95616 USA. RP MacLeod, CL (reprint author), Univ Washington, Dept Astron, Box 351580, Seattle, WA 98195 USA. EM cmacleod@astro.washington.edu RI Kozlowski, Szymon/G-4799-2013 OI Kozlowski, Szymon/0000-0003-4084-880X FU NSF [AST-0807500, AST-0551161, AST-0708082]; NASA [HF-51243.01, NAS 5-26555, AR9-0015X, AR0-11014X]; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy; National Aeronautics and Space Administration; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England; American Museum of Natural History; Astrophysical Institute Potsdam; University of Basel; University of Cambridge; Case Western Reserve University; University of Chicago; Drexel University; Fermilab; Institute for Advanced Study; Japan Participation Group; Johns Hopkins University; Joint Institute for Nuclear Astrophysics; Kavli Institute for Particle Astrophysics and Cosmology; Korean Scientist Group; 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 We acknowledge support by NSF grant AST-0807500 to the University of Washington, and NSF grant AST-0551161 to LSST for design and development activity. C. S. K. and S. K. acknowledge support by NSF grant AST-0708082. B. K. acknowledges support by NASA through Hubble Fellowship grant HF-51243.01 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. R. R. G. gratefully acknowledges support from NASA Chandra grants AR9-0015X and AR0-11014X. We thank an anonymous referee for valuable suggestions regarding the analysis in Section 4.4.; Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web site is http://www. sdss.org/.; The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington. NR 79 TC 158 Z9 158 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2010 VL 721 IS 2 BP 1014 EP 1033 DI 10.1088/0004-637X/721/2/1014 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 654TP UT WOS:000282193600008 ER PT J AU Li, ZY Spitler, LR Jones, C Forman, WR Kraft, RP Di Stefano, R Tang, SK Wang, QD Gilfanov, M Revnivtsev, M AF Li, Zhiyuan Spitler, Lee R. Jones, Christine Forman, William R. Kraft, Ralph P. Di Stefano, Rosanne Tang, Shikui Wang, Q. Daniel Gilfanov, Marat Revnivtsev, Mikhail TI X-RAY EMISSION FROM THE SOMBRERO GALAXY: DISCRETE SOURCES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: individual (M104); galaxies: spiral; X-rays: binaries; X-rays: galaxies ID CHANDRA MONITORING OBSERVATIONS; GLOBULAR-CLUSTER SYSTEMS; POINT-SOURCE POPULATION; ELLIPTIC GALAXIES; DEEP CHANDRA; BLACK-HOLES; CENTAURUS-A; MASS; BINARIES; FIELD AB We present a study of discrete X-ray sources in and around the bulge-dominated, massive Sa galaxy, Sombrero (M104), based on new and archival Chandra observations with a total exposure of similar to 200 ks. With a detection limit of L(X) approximate to 10(37) erg s(-1) and a field of view covering a galactocentric radius of similar to 30 kpc (11.'5), 383 sources are detected. Cross-correlation with Spitler et al.'s catalog of Sombrero globular clusters (GCs) identified from HST/ACS observations reveals 41 X-ray sources in GCs, presumably low-mass X-ray binaries (LMXBs). Metal-rich GCs are found to have a higher probability of hosting these LMXBs, a trend similar to that found in elliptical galaxies. On the other hand, the four most luminous GC LMXBs, with apparently super-Eddington luminosities for an accreting neutron star, are found in metal-poor GCs. We quantify the differential luminosity functions (LFs) for both the detected GC and field LMXBs, whose power-law indices (similar to 1.1 for the GC-LF and similar to 1.6 for field-LF) are consistent with previous studies for elliptical galaxies. With precise sky positions of the GCs without a detected X-ray source, we further quantify, through a fluctuation analysis, the GC-LF at fainter luminosities down to 1035 erg s-1. The derived index rules out a faint-end slope flatter than 1.1 at a 2 sigma significance, contrary to recent findings in several elliptical galaxies and the bulge of M31. On the other hand, the 2-6 keV unresolved emission places a tight constraint on the field LF, implying a flattened index of similar to 1.0 below 10(37) erg s(-1). We also detect 101 sources in the halo of Sombrero. The presence of these sources cannot be interpreted as galactic LMXBs whose spatial distribution empirically follows the starlight. Their number is also higher than the expected number of cosmic active galactic nuclei (52 +/- 11 [sigma s]) whose surface density is constrained by deep X-ray surveys. We suggest that either the cosmic X-ray background is unusually high in the direction of Sombrero, or a distinct population of X-ray sources is present in the halo of Sombrero. C1 [Li, Zhiyuan; Jones, Christine; Forman, William R.; Kraft, Ralph P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Spitler, Lee R.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Tang, Shikui; Wang, Q. Daniel] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Gilfanov, Marat] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Revnivtsev, Mikhail] Tech Univ Munich, Excellence Cluster Univ, D-85748 Garching, Germany. [Revnivtsev, Mikhail] Russian Acad Sci, Inst Space Res, Moscow 117997, Russia. RP Li, ZY (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM zyli@cfa.harvard.edu RI Tang, Shikui/D-9798-2012; Spitler, Lee/A-9867-2013 OI Spitler, Lee/0000-0001-5185-9876 FU SAO [G08-9088] FX We are grateful to Ryan Hickox for his advice on the fluctuation analysis. This work is supported by the SAO grant G08-9088. NR 50 TC 9 Z9 9 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2010 VL 721 IS 2 BP 1368 EP 1382 DI 10.1088/0004-637X/721/2/1368 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 654TP UT WOS:000282193600035 ER PT J AU Buemi, CS Umana, G Trigilio, C Leto, P Hora, JL AF Buemi, C. S. Umana, G. Trigilio, C. Leto, P. Hora, J. L. TI VISIR/VLT AND VLA JOINT IMAGING ANALYSIS OF THE CIRCUMSTELLAR NEBULA AROUND IRAS 18576+0341 SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; infrared: stars; stars: early-type; stars: individual (IRAS 18576+0341); stars: winds, outflows ID LUMINOUS-BLUE-VARIABLES; GALACTIC-CENTER QUINTUPLET; SPITZER-SPACE-TELESCOPE; PLANETARY-NEBULAE; STELLAR WINDS; MASSIVE STARS; IRAS-18576+0341; POPULATION; EMISSION; CARINAE AB High spatial and sensitivity images of the Luminous Blue Variable IRAS 18576+0341 were obtained using the mid-infrared imager VISIR at the Very Large Telescope and the Very Large Array interferometer. The resulting mid-infrared continuum maps show a similar clumpy and approximately circular symmetric nebula, which contrasts sharply with the asymmetry that characterizes the ionized component of the envelope, as evidenced from the radio and [Ne II] line images obtained with comparable spatial resolution. In particular, there is excellent overall agreement between the 12.8 mu m map and the radio images, consistent with free-free emission from circumstellar ionized material surrounding a central stellar wind. The color temperature and optical depth maps obtained from mid-infrared images show only slight fluctuations, suggesting quite uniform dust characteristics over the dust shell. We explore various possibilities to understand the cause of the different morphology of the dusty and gaseous component of the circumstellar envelope which are compatible with the observations. C1 [Buemi, C. S.; Umana, G.; Trigilio, C.; Leto, P.] INAF Osservatorio Astrofis Catania, I-95123 Catania, Italy. [Hora, J. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Buemi, CS (reprint author), INAF Osservatorio Astrofis Catania, Via S Sofia 75, I-95123 Catania, Italy. OI Buemi, Carla Simona/0000-0002-7288-4613; Leto, Paolo/0000-0003-4864-2806; Hora, Joseph/0000-0002-5599-4650 FU ASI [I/038/08/0]; PRIN-INAF FX We acknowledge partial financial support from the ASI contract I/038/08/0 "HI-GAL" and from PRIN-INAF 2007. NR 32 TC 7 Z9 7 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2010 VL 721 IS 2 BP 1404 EP 1411 DI 10.1088/0004-637X/721/2/1404 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 654TP UT WOS:000282193600038 ER PT J AU Abdo, AA Ackermann, M Agudo, I Ajello, M Allafort, A Aller, HD Aller, MF Antolini, E Arkharov, AA Axelsson, M Bach, U Baldini, L Ballet, J Barbiellini, G Bastieri, D Bechtol, K Bellazzini, R Berdyugin, A Berenji, B Blandford, RD Blinov, DA Bloom, ED Boettcher, M Bonamente, E Borgland, AW Bouvier, A Bregeon, J Brez, A Brigida, M Bruel, P Buehler, R Buemi, CS Burnett, TH Buson, S Caliandro, GA Cameron, RA Caraveo, PA Carosati, D Carrigan, S Casandjian, JM Cavazzuti, E Cecchi, C Celik, O Chekhtman, A Chen, WP Cheung, CC Chiang, J Ciprini, S Claus, R Cohen-Tanugi, J Conrad, J Corbel, S Costamante, L Dermer, CD de Angelis, A de Palma, F Donato, D Silva, EDE Drell, PS Dubois, R Dumora, D Farnier, C Favuzzi, C Fegan, SJ Ferrara, EC Focke, WB Forne, E Fortin, P Fukazawa, Y Funk, S Fusco, P Gargano, F Gasparrini, D Gehrels, N Germani, S Giebels, B Giglietto, N Giordano, F Giroletti, M Glanzman, T Godfrey, G Grenier, IA Grove, JE Guiriec, S Gurwell, MA Gusbar, C Gomez, JL Hadasch, D Hagen-Thorn, VA Hayashida, M Hays, E Horan, D Hughes, RE Johannesson, G Johnson, AS Johnson, WN Kamae, T Katagiri, H Kataoka, J Kawai, N Kimeridze, G Knodlseder, J Konstantinova, TS Kopatskaya, EN Koptelova, E Kovalev, YY Kurtanidze, OM Kuss, M Lahteenmaki, A Lande, J Larionov, VM Larionova, EG Larionova, LV Larsson, S Latronico, L Lee, SH Leto, P Lister, ML Longo, F Loparco, F Lott, B Lovellette, MN Lubrano, P Madejski, GM Makeev, A Massaro, E Mazziotta, MN McConville, W McEnery, JE McHardy, IM Michelson, PF Mitthumsiri, W Mizuno, T Moiseev, AA Monte, C Monzani, ME Morozova, DA Morselli, A Moskalenko, IV Murgia, S Naumann-Godo, M Nikolashvili, MG Nolan, PL Norris, JP Nuss, E Ohno, M Ohsugi, T Okumura, A Omodei, N Orlando, E Ormes, JF Ozaki, M Paneque, D Panetta, JH Parent, D Pasanen, M Pelassa, V Pepe, M Pesce-Rollins, M Piron, F Porter, TA Pushkarev, AB Raino, S Raiteri, CM Rando, R Razzano, M Reimer, A Reimer, O Reinthal, R Ripken, J Ritz, S Roca-Sogorb, M Rodriguez, AY Roth, M Roustazadeh, P Ryde, F Sadrozinski, HFW Sander, A Scargle, JD Sgro, C Sigua, LA Smith, PD Sokolovsky, K Spandre, G Spinelli, P Starck, JL Strickman, MS Suson, DJ Takahashi, H Takahashi, T Takalo, LO Tanaka, T Taylor, B Thayer, JB Thayer, JG Thompson, DJ Tibaldo, L Tornikoski, M Torres, DF Tosti, G Tramacere, A Trigilio, C Troitsky, IS Umana, G Usher, TL Vandenbroucke, J Vasileiou, V Vilchez, N Villata, M Vitale, V Waite, AP Wang, P Winer, BL Wood, KS Yang, Z Ylinen, T Ziegler, M AF Abdo, A. A. Ackermann, M. Agudo, I. Ajello, M. Allafort, A. Aller, H. D. Aller, M. F. Antolini, E. Arkharov, A. A. Axelsson, M. Bach, U. Baldini, L. Ballet, J. Barbiellini, G. Bastieri, D. Bechtol, K. Bellazzini, R. Berdyugin, A. Berenji, B. Blandford, R. D. Blinov, D. A. Bloom, E. D. Boettcher, M. Bonamente, E. Borgland, A. W. Bouvier, A. Bregeon, J. Brez, A. Brigida, M. Bruel, P. Buehler, R. Buemi, C. S. Burnett, T. H. Buson, S. Caliandro, G. A. Cameron, R. A. Caraveo, P. A. Carosati, D. Carrigan, S. Casandjian, J. M. Cavazzuti, E. Cecchi, C. Celik, Oe Chekhtman, A. Chen, W. P. Cheung, C. C. Chiang, J. Ciprini, S. Claus, R. Cohen-Tanugi, J. Conrad, J. Corbel, S. Costamante, L. Dermer, C. D. de Angelis, A. de Palma, F. Donato, D. do Couto e Silva, E. Drell, P. S. Dubois, R. Dumora, D. Farnier, C. Favuzzi, C. Fegan, S. J. Ferrara, E. C. Focke, W. B. Forne, E. Fortin, P. Fukazawa, Y. Funk, S. Fusco, P. Gargano, F. Gasparrini, D. Gehrels, N. Germani, S. Giebels, B. Giglietto, N. Giordano, F. Giroletti, M. Glanzman, T. Godfrey, G. Grenier, I. A. Grove, J. E. Guiriec, S. Gurwell, M. A. Gusbar, C. Gomez, J. L. Hadasch, D. Hagen-Thorn, V. A. Hayashida, M. Hays, E. Horan, D. Hughes, R. E. Johannesson, G. Johnson, A. S. Johnson, W. N. Kamae, T. Katagiri, H. Kataoka, J. Kawai, N. Kimeridze, G. Knoedlseder, J. Konstantinova, T. S. Kopatskaya, E. N. Koptelova, E. Kovalev, Y. Y. Kurtanidze, O. M. Kuss, M. Lahteenmaki, A. Lande, J. Larionov, V. M. Larionova, E. G. Larionova, L. V. Larsson, S. Latronico, L. Lee, S. -H. Leto, P. Lister, M. L. Longo, F. Loparco, F. Lott, B. Lovellette, M. N. Lubrano, P. Madejski, G. M. Makeev, A. Massaro, E. Mazziotta, M. N. McConville, W. McEnery, J. E. McHardy, I. M. Michelson, P. F. Mitthumsiri, W. Mizuno, T. Moiseev, A. A. Monte, C. Monzani, M. E. Morozova, D. A. Morselli, A. Moskalenko, I. V. Murgia, S. Naumann-Godo, M. Nikolashvili, M. G. Nolan, P. L. Norris, J. P. Nuss, E. Ohno, M. Ohsugi, T. Okumura, A. Omodei, N. Orlando, E. Ormes, J. F. Ozaki, M. Paneque, D. Panetta, J. H. Parent, D. Pasanen, M. Pelassa, V. Pepe, M. Pesce-Rollins, M. Piron, F. Porter, T. A. Pushkarev, A. B. Raino, S. Raiteri, C. M. Rando, R. Razzano, M. Reimer, A. Reimer, O. Reinthal, R. Ripken, J. Ritz, S. Roca-Sogorb, M. Rodriguez, A. Y. Roth, M. Roustazadeh, P. Ryde, F. Sadrozinski, H. F. -W. Sander, A. Scargle, J. D. Sgro, C. Sigua, L. A. Smith, P. D. Sokolovsky, K. Spandre, G. Spinelli, P. Starck, J. -L. Strickman, M. S. Suson, D. J. Takahashi, H. Takahashi, T. Takalo, L. O. Tanaka, T. Taylor, B. Thayer, J. B. Thayer, J. G. Thompson, D. J. Tibaldo, L. Tornikoski, M. Torres, D. F. Tosti, G. Tramacere, A. Trigilio, C. Troitsky, I. S. Umana, G. Usher, T. L. Vandenbroucke, J. Vasileiou, V. Vilchez, N. Villata, M. Vitale, V. Waite, A. P. Wang, P. Winer, B. L. Wood, K. S. Yang, Z. Ylinen, T. Ziegler, M. TI FERMI LARGE AREA TELESCOPE AND MULTI-WAVELENGTH OBSERVATIONS OF THE FLARING ACTIVITY OF PKS 1510-089 BETWEEN 2008 SEPTEMBER AND 2009 JUNE SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: jets; gamma rays: galaxies; quasars: individual (PKS 1510-089) ID GAMMA-RAY EMISSION; GALACTIC NUCLEI; X-RAY; SPECTRAL PROPERTIES; RELATIVISTIC JET; COMPLETE SAMPLE; RADIO-SOURCES; EGRET DATA; 3C 454.3; BLAZAR AB We report on the multi-wavelength observations of PKS 1510-089 (a flat spectrum radio quasar (FSRQ) at z = 0.361) during its high activity period between 2008 September and 2009 June. During this 11 month period, the source was characterized by a complex variability at optical, UV, and gamma-ray bands, on timescales down to 6-12 hr. The brightest gamma-ray isotropic luminosity, recorded on 2009 March 26, was similar or equal to 2 x 1048 erg s-1. The spectrum in the Fermi Large Area Telescope energy range shows a mild curvature described well by a log-parabolic law, and can be understood as due to the Klein-Nishina effect. The. -ray flux has a complex correlation with the other wavelengths. There is no correlation at all with the X-ray band, a weak correlation with the UV, and a significant correlation with the optical flux. The. -ray flux seems to lead the optical one by about 13 days. From the UV photometry, we estimated a black hole mass of similar or equal to 5.4 x 10(8)M(circle dot) and an accretion rate of similar or equal to 0.5M(circle dot) yr(-1). Although the power in the thermal and non-thermal outputs is smaller compared to the very luminous and distant FSRQs, PKS 1510-089 exhibits a quite large Compton dominance and a prominent big blue bump (BBB) as observed in the most powerful gamma-ray quasars. The BBB was still prominent during the historical maximum optical state in 2009 May, but the optical/ UV spectral index was softer than in the quiescent state. This seems to indicate that the BBB was not completely dominated by the synchrotron emission during the highest optical state. We model the broadband spectrum assuming a leptonic scenario in which the inverse Compton emission is dominated by the scattering of soft photons produced externally to the jet. The resulting model-dependent jet energetic content is compatible with a scenario in which the jet is powered by the accretion disk, with a total efficiency within the Kerr black hole limit. C1 [Abdo, A. A.; Chekhtman, A.; Cheung, C. C.; Dermer, C. D.; Grove, J. E.; Johnson, W. N.; Lovellette, M. N.; Makeev, A.; Parent, D.; Strickman, M. S.; Wood, K. S.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. [Abdo, A. A.; Cheung, C. C.] Natl Acad Sci, Washington, DC 20001 USA. [Ackermann, M.; Ajello, M.; Allafort, A.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Bouvier, A.; Buehler, R.; Cameron, R. A.; Chiang, J.; Claus, R.; Costamante, L.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Focke, W. B.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Johannesson, G.; Johnson, A. S.; Kamae, T.; Lande, J.; Lee, S. -H.; Madejski, G. M.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Omodei, N.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Usher, T. L.; Vandenbroucke, J.; Waite, A. P.; Wang, P.] Stanford Univ, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA. [Ackermann, M.; Ajello, M.; Allafort, A.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Bouvier, A.; Buehler, R.; Cameron, R. 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[Tramacere, A.] Consorzio Interuniversitario Fis Spaziale CIFS, I-10133 Turin, Italy. [Tramacere, A.] INTEGRAL Sci Data Ctr, CH-1290 Versoix, Switzerland. [Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. [Ylinen, T.] Univ Kalmar, Sch Pure & Appl Nat Sci, SE-39182 Kalmar, Sweden. RP Abdo, AA (reprint author), USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. EM enrico.massaro@uniroma1.it RI Grishina, Tatiana/H-6873-2013; Hagen-Thorn, Vladimir/H-3983-2013; Johannesson, Gudlaugur/O-8741-2015; Loparco, Francesco/O-8847-2015; Gargano, Fabio/O-8934-2015; Pushkarev, Alexander/M-9997-2015; Moskalenko, Igor/A-1301-2007; Mazziotta, Mario /O-8867-2015; Sgro, Carmelo/K-3395-2016; Torres, Diego/O-9422-2016; Orlando, E/R-5594-2016; Blinov, Dmitry/G-9925-2013; Ozaki, Masanobu/K-1165-2013; Rando, Riccardo/M-7179-2013; Kovalev, Yuri/J-5671-2013; Lahteenmaki, Anne/L-5987-2013; Hays, Elizabeth/D-3257-2012; Johnson, Neil/G-3309-2014; Kurtanidze, Omar/J-6237-2014; Funk, Stefan/B-7629-2015; Sokolovsky, Kirill/D-2246-2015; Agudo, Ivan/G-1701-2015; Morozova, Daria/H-1298-2013; Troitskiy, Ivan/K-7979-2013; Starck, Jean-Luc/D-9467-2011; Thompson, David/D-2939-2012; Gehrels, Neil/D-2971-2012; McEnery, Julie/D-6612-2012; Baldini, Luca/E-5396-2012; lubrano, pasquale/F-7269-2012; Morselli, Aldo/G-6769-2011; Kuss, Michael/H-8959-2012; giglietto, nicola/I-8951-2012; Reimer, Olaf/A-3117-2013; Tosti, Gino/E-9976-2013; Larionov, Valeri/H-1349-2013; Kopatskaya, Evgenia/H-4720-2013; Larionova, Elena/H-7287-2013 OI Berenji, Bijan/0000-0002-4551-772X; Gasparrini, Dario/0000-0002-5064-9495; Tramacere, Andrea/0000-0002-8186-3793; Baldini, Luca/0000-0002-9785-7726; Bastieri, Denis/0000-0002-6954-8862; Omodei, Nicola/0000-0002-5448-7577; Pesce-Rollins, Melissa/0000-0003-1790-8018; Axelsson, Magnus/0000-0003-4378-8785; Giroletti, Marcello/0000-0002-8657-8852; Villata, Massimo/0000-0003-1743-6946; Giordano, Francesco/0000-0002-8651-2394; Larionova, Liudmila/0000-0002-0274-1481; De Angelis, Alessandro/0000-0002-3288-2517; Caraveo, Patrizia/0000-0003-2478-8018; Leto, Paolo/0000-0003-4864-2806; Sgro', Carmelo/0000-0001-5676-6214; Rando, Riccardo/0000-0001-6992-818X; Raiteri, Claudia Maria/0000-0003-1784-2784; Grishina, Tatiana/0000-0002-3953-6676; Hagen-Thorn, Vladimir/0000-0002-6431-8590; Johannesson, Gudlaugur/0000-0003-1458-7036; Loparco, Francesco/0000-0002-1173-5673; Gargano, Fabio/0000-0002-5055-6395; Moskalenko, Igor/0000-0001-6141-458X; Mazziotta, Mario /0000-0001-9325-4672; Torres, Diego/0000-0002-1522-9065; Buemi, Carla Simona/0000-0002-7288-4613; Blinov, Dmitry/0000-0003-0611-5784; Kovalev, Yuri/0000-0001-9303-3263; Funk, Stefan/0000-0002-2012-0080; Sokolovsky, Kirill/0000-0001-5991-6863; Agudo, Ivan/0000-0002-3777-6182; Morozova, Daria/0000-0002-9407-7804; Troitskiy, Ivan/0000-0002-4218-0148; Starck, Jean-Luc/0000-0003-2177-7794; Thompson, David/0000-0001-5217-9135; lubrano, pasquale/0000-0003-0221-4806; Morselli, Aldo/0000-0002-7704-9553; giglietto, nicola/0000-0002-9021-2888; Reimer, Olaf/0000-0001-6953-1385; Larionov, Valeri/0000-0002-4640-4356; Kopatskaya, Evgenia/0000-0001-9518-337X; Larionova, Elena/0000-0002-2471-6500 FU Russian Foundation for Basic Research [08- 0200545] FX The Lebedev Physical Institute team was partly supported by the Russian Foundation for Basic Research (project 08- 0200545). K. S. was supported by stipend from the IMPRS for Astronomy and Astrophysics. We thank A. P. Marscher and S. Jorstad for providing multi- wavelength data. NR 78 TC 57 Z9 57 U1 1 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2010 VL 721 IS 2 BP 1425 EP 1447 DI 10.1088/0004-637X/721/2/1425 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 654TP UT WOS:000282193600041 ER PT J AU Kim, DW Fabbiano, G AF Kim, Dong-Woo Fabbiano, Giuseppina TI X-RAY PROPERTIES OF YOUNG EARLY-TYPE GALAXIES. I. X-RAY LUMINOSITY FUNCTION OF LOW-MASS X-RAY BINARIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: elliptical and lenticular, cD; X-rays: binaries; X-rays: galaxies ID CHANDRA MULTIWAVELENGTH PROJECT; GLOBULAR-CLUSTER CONNECTION; NGC-1316 FORNAX-A; ELLIPTIC GALAXIES; POINT-SOURCE; VIRGO CLUSTER; DEEP CHANDRA; MONITORING OBSERVATIONS; STELLAR POPULATIONS; SAURON PROJECT AB We have compared the combined X-ray luminosity function (XLF) of low-mass X-ray binaries (LMXBs) detected in Chandra observations of young, post-merger elliptical galaxies with that of typical old elliptical galaxies. We find that the XLF of the "young" sample does not present the prominent high-luminosity break at L(X) > 5 x 10(38) erg s(-1) found in the old elliptical galaxy XLF. The "young" and "old" XLFs differ with a 3 sigma statistical significance (with a probability less than 0.2% that they derive from the same underlying parent distribution). Young elliptical galaxies host a larger fraction of luminous LMXBs (L(X) > 5 x 10(38) erg s(-1)) than old elliptical galaxies and the XLF of the young galaxy sample is intermediate between that of typical old elliptical galaxies and that of star-forming galaxies. This observational evidence may be related to the last major/minor mergers and the associated star formation. C1 [Kim, Dong-Woo; Fabbiano, Giuseppina] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Kim, DW (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. FU Chandra GO [G08-9133X] FX The data analysis was supported by the CXC CIAO software and CALDB. We have used the NASA NED and ADS facilities and extracted archival data from the Chandra archives. This work was supported by the Chandra GO grant G08-9133X (PI: Kim). We thank Tassos Fragos and Vicky Kalogera for interesting conversations. NR 64 TC 33 Z9 33 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2010 VL 721 IS 2 BP 1523 EP 1530 DI 10.1088/0004-637X/721/2/1523 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 654TP UT WOS:000282193600048 ER PT J AU Reeves, KK Linker, JA Mikic, Z Forbes, TG AF Reeves, Katharine K. Linker, Jon A. Mikic, Zoran Forbes, Terry G. TI CURRENT SHEET ENERGETICS, FLARE EMISSIONS, AND ENERGY PARTITION IN A SIMULATED SOLAR ERUPTION SO ASTROPHYSICAL JOURNAL LA English DT Article DE magnetic reconnection; magnetohydrodynamics (MHD); Sun: coronal mass ejections (CMEs) Sun: flares ID CORONAL MASS EJECTIONS; X-RAY TELESCOPE; FIELD LINE SHRINKAGE; WHOLE SUN MONTH; MAGNETIC RECONNECTION; HELMET STREAMER; 3 DIMENSIONS; FLUX ROPES; MODEL; DISRUPTION AB We investigate coronal energy flow during a simulated coronal mass ejection (CME). We model the CME in the context of the global corona using a 2.5D numerical MHD code in spherical coordinates that includes coronal heating, thermal conduction, and radiative cooling in the energy equation. The simulation domain extends from 1 to 20 Rs. To our knowledge, this is the first attempt to apply detailed energy diagnostics in a flare/ CMEsimulationwhen these important terms are considered in the context of the MHD equations. We find that the energy conservation properties of the code are quite good, conserving energy to within 4% for the entire simulation (more than 6 days of real time). We examine the energy release in the current sheet as the eruption takes place, and find, as expected, that the Poynting flux is the dominant carrier of energy into the current sheet. However, there is a significant flow of energy out of the sides of the current sheet into the upstream region due to thermal conduction along field lines and viscous drag. This energy outflow is spatially partitioned into three separate components, namely, the energy flux flowing out the sides of the current sheet, the energy flowing out the lower tip of the current sheet, and the energy flowing out the upper tip of the current sheet. The energy flow through the lower tip of the current sheet is the energy available for heating of the flare loops. We examine the simulated flare emissions and energetics due to the modeled CME and find reasonable agreement with flare loop morphologies and energy partitioning in observed solar eruptions. The simulation also provides an explanation for coronal dimming during eruptions and predicts that the structures surrounding the current sheet are visible in X-ray observations. C1 [Reeves, Katharine K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Linker, Jon A.; Mikic, Zoran] Predict Sci Inc PSI, San Diego, CA 92121 USA. [Forbes, Terry G.] Univ New Hampshire, Inst Study Earth Oceans & Space EOS, Durham, NH 03824 USA. RP Reeves, KK (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM kreeves@cfa.harvard.edu; linkerj@predsci.com; mikicz@predsci.com; terry.forbes@unh.edu RI Reeves, Katharine/P-9163-2014 FU NSF-SHINE [ATM0752257] FX K. K. Reeves thanks E. E. DeLuca and H. D. Winter for useful conversations about the numerical simulations. K. R. and T. F. are supported under the NSF-SHINE program, grant number ATM0752257. Additional support for K. R. is provided by NASA grant NNM07AA02C to the Smithsonian Astrophysical Observatory. The work of J. L. and Z. M. is supported by NASA's Heliophysics Theory, LWS, and SR& T Programs, the LWS Strategic Capabilities Program (NASA, NSF, and AFOSR), and the Center for Integrated Space Weather Modeling (an NSF Science and Technology Center). NR 50 TC 48 Z9 48 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2010 VL 721 IS 2 BP 1547 EP 1558 DI 10.1088/0004-637X/721/2/1547 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 654TP UT WOS:000282193600050 ER PT J AU Brown, PJ Roming, PWA Milne, P Bufano, F Ciardullo, R Elias-Rosa, N Filippenko, AV Foley, RJ Gehrels, N Gronwall, C Hicken, M Holland, ST Hoversten, EA Immler, S Kirshner, RP Li, WD Mazzali, P Phillips, MM Pritchard, T Still, M Turatto, M Vanden Berk, D AF Brown, Peter J. Roming, Peter W. A. Milne, Peter Bufano, Filomena Ciardullo, Robin Elias-Rosa, Nancy Filippenko, Alexei V. Foley, Ryan J. Gehrels, Neil Gronwall, Caryl Hicken, Malcolm Holland, Stephen T. Hoversten, Erik A. Immler, Stefan Kirshner, Robert P. Li, Weidong Mazzali, Paolo Phillips, Mark M. Pritchard, Tyler Still, Martin Turatto, Massimo Vanden Berk, Daniel TI THE ABSOLUTE MAGNITUDES OF TYPE Ia SUPERNOVAE IN THE ULTRAVIOLET SO ASTROPHYSICAL JOURNAL LA English DT Article DE distance scale; dust, extinction; galaxies: distances and redshifts; supernovae: general; ultraviolet: general ID HUBBLE-SPACE-TELESCOPE; SURFACE BRIGHTNESS FLUCTUATIONS; HIGH-REDSHIFT SUPERNOVAE; EARLY-TYPE GALAXIES; LIGHT-CURVE SHAPES; DIGITAL SKY SURVEY; K-CORRECTIONS; DARK ENERGY; DECLINE-RATE; LUMINOSITY INDICATORS AB We examine the absolute magnitudes and light-curve shapes of 14 nearby (redshift z = 0.004-0.027) Type Ia supernovae (SNe Ia) observed in the ultraviolet (UV) with the Swift Ultraviolet/Optical Telescope. Colors and absolute magnitudes are calculated using both a standard Milky Way extinction law and one for the Large Magellanic Cloud that has been modified by circumstellar scattering. We find very different behavior in the near-UV filters (uvw1(rc) covering similar to 2600-3300 (A) over circle after removing optical light, and u approximate to 3000-4000 (A) over circle) compared to a mid-UV filter (uvm2 approximate to 2000-2400 (A) over circle). The uvw1(rc) - b colors show a scatter of similar to 0.3 mag while uvm2-b scatters by nearly 0.9 mag. Similarly, while the scatter in colors between neighboring filters is small in the optical and somewhat larger in the near-UV, the large scatter in the uvm2 - uvw1 colors implies significantly larger spectral variability below 2600 (A) over circle. We find that in the near-UV the absolute magnitudes at peak brightness of normal SNe Ia in our sample are correlated with the optical decay rate with a scatter of 0.4 mag, comparable to that found for the optical in our sample. However, in the mid-UV the scatter is larger, similar to 1 mag, possibly indicating differences in metallicity. We find no strong correlation between either the UV light-curve shapes or the UV colors and the UV absolute magnitudes. With larger samples, the UV luminosity might be useful as an additional constraint to help determine distance, extinction, and metallicity in order to improve the utility of SNe Ia as standardized candles. C1 [Brown, Peter J.; Roming, Peter W. A.; Ciardullo, Robin; Gronwall, Caryl; Hoversten, Erik A.; Pritchard, Tyler] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Milne, Peter] Univ Arizona, Steward Observ, Tucson, AZ 85719 USA. [Bufano, Filomena; Mazzali, Paolo] INAF Osservatorio Astron Padova, I-35122 Padua, Italy. [Elias-Rosa, Nancy] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Filippenko, Alexei V.; Li, Weidong] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Foley, Ryan J.; Hicken, Malcolm; Kirshner, Robert P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gehrels, Neil; Holland, Stephen T.; Immler, Stefan] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Holland, Stephen T.] Univ Space Res Assoc, Columbia, MD 21044 USA. [Holland, Stephen T.; Immler, Stefan] NASA GFC, Ctr Res & Explorat Space Sci & Technol, Greenbelt, MD 20771 USA. [Immler, Stefan] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Mazzali, Paolo] Max Planck Inst Astrophys, D-85748 Garching, Germany. [Mazzali, Paolo] Scuola Normale Super Pisa, I-56126 Pisa, Italy. [Phillips, Mark M.] Las Campanas Observ, La Serena, Chile. [Still, Martin] Univ Coll London, Dept Space & Climate Phys, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Still, Martin] NASA, Ames Res Ctr, Moffett Field, CA 93045 USA. [Turatto, Massimo] Osserv Astrofis Catania, I-95123 Catania, Italy. [Vanden Berk, Daniel] St Vincent Coll, Latrobe, PA 15650 USA. RP Brown, PJ (reprint author), Univ Utah, Dept Phys & Astron, 115 South 1400 East 201, Salt Lake City, UT 84112 USA. EM pbrown@physics.utah.edu RI Gehrels, Neil/D-2971-2012; Elias-Rosa, Nancy/D-3759-2014; OI Elias-Rosa, Nancy/0000-0002-1381-9125; Turatto, Massimo/0000-0002-9719-3157 FU NASA [NAS5-00136, NNH06ZDA001N]; NSF [AST-0908886, NNX09AG54G, AST-0907903]; PRIN of Italian Ministry of University and Science Research [2006022731] FX We are grateful to A. Goobar for extending his circumstellar extinction model into the UV for us. This work is supported at Penn State University by NASA contract NAS5-00136 and Swift Guest Investigator grant NNH06ZDA001N. A.V.F. is grateful for the support of NSF grant AST-0908886 and Swift Guest Investigator grant NNX09AG54G. This work made use of public data in the Swift data archive and the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. The CfA Supernova Program at Harvard University is supported by NSF grant AST-0907903. The work of M.T. is supported by grant no.. 2006022731 of the PRIN of Italian Ministry of University and Science Research. NR 116 TC 53 Z9 53 U1 2 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2010 VL 721 IS 2 BP 1608 EP 1626 DI 10.1088/0004-637X/721/2/1608 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 654TP UT WOS:000282193600057 ER PT J AU Milne, PA Brown, PJ Roming, PWA Holland, ST Immler, S Filippenko, AV Ganeshalingam, M Li, WD Stritzinger, M Phillips, MM Hicken, M Kirshner, RP Challis, PJ Mazzali, P Schmidt, BP Bufano, F Gehrels, N Vanden Berk, D AF Milne, Peter A. Brown, Peter J. Roming, Peter W. A. Holland, Stephen T. Immler, Stefan Filippenko, Alexei V. Ganeshalingam, Mohan Li, Weidong Stritzinger, Maximilian Phillips, Mark M. Hicken, Malcolm Kirshner, Robert P. Challis, Peter J. Mazzali, Paolo Schmidt, Brian P. Bufano, Filomena Gehrels, Neil Vanden Berk, Daniel TI NEAR-ULTRAVIOLET PROPERTIES OF A LARGE SAMPLE OF TYPE Ia SUPERNOVAE AS OBSERVED WITH THE Swift UVOT SO ASTROPHYSICAL JOURNAL LA English DT Article DE distance scale; dust, extinction; galaxies: distances and redshifts; supernovae: general; ultraviolet: general ID HUBBLE-SPACE-TELESCOPE; ULTRA-VIOLET/OPTICAL TELESCOPE; LIGHT-CURVE SHAPES; X-RAY OBSERVATIONS; II-P SUPERNOVAE; DECLINE-RATE; INFRARED OBSERVATIONS; OPTICAL PHOTOMETRY; IMPROVED DISTANCES; SYNTHETIC SPECTRA AB We present ultraviolet (UV) and optical photometry of 26 Type Ia supernovae (SNe Ia) observed from 2005 March to 2008 March with the NASA Swift Ultraviolet and Optical Telescope (UVOT). The dataset consists of 2133 individual observations, making it by far the most complete study of the UV emission from SNe Ia to date. Grouping the SNe into three subclasses as derived from optical observations, we investigate the evolution of the colors of these SNe, finding a high degree of homogeneity within the normal subclass, but dramatic differences between that group and the subluminous and SN 2002cx-like groups. For the normal events, the redder UV filters on UVOT (u, uvw1) show more homogeneity than do the bluer UV filters (uvm2, uvw2). Searching for purely UV characteristics to determine existing optically based groupings, we find the peak width to be a poor discriminant, but we do see a variation in the time delay between peak emission and the late, flat phase of the light curves. The UV light curves peak a few days before the B band for most subclasses (as was previously reported by Jha et al.), although the SN 2002cx-like objects peak at a very early epoch in the UV. That group also features the bluest emission observed among SNe Ia. As the observational campaign is ongoing, we discuss the critical times to observe, as determined by this study, in order to maximize the scientific output of future observations. C1 [Milne, Peter A.] Univ Arizona, Steward Observ, Tucson, AZ 85719 USA. [Brown, Peter J.; Roming, Peter W. A.; Vanden Berk, Daniel] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Holland, Stephen T.; Immler, Stefan; Bufano, Filomena; Gehrels, Neil] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Holland, Stephen T.; Immler, Stefan] Univ Space Res Assoc, Columbia, MD 21044 USA. [Filippenko, Alexei V.; Ganeshalingam, Mohan; Li, Weidong] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Stritzinger, Maximilian; Phillips, Mark M.] Carnegie Observ, Las Campanas Observ, La Serena, Chile. [Stritzinger, Maximilian] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen O, Denmark. [Hicken, Malcolm; Kirshner, Robert P.; Challis, Peter J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Mazzali, Paolo] Astron Observ Padova, INAF, I-35122 Padua, Italy. [Mazzali, Paolo] Max Planck Inst Astrophys, D-85748 Garching, Germany. [Schmidt, Brian P.] Australian Natl Univ, Res Sch Astron & Astrophys, Mt Stromlo Observ, Weston, ACT 2611, Australia. [Bufano, Filomena] Univ Padua, Dipartmento Astron, I-35122 Padua, Italy. [Vanden Berk, Daniel] St Vincent Coll, Latrobe, PA USA. RP Milne, PA (reprint author), Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85719 USA. RI Gehrels, Neil/D-2971-2012; OI Schmidt, Brian/0000-0001-6589-1287; stritzinger, maximilian/0000-0002-5571-1833 FU National Science Foundation (NSF) [AST-0607485, AST-0908886, AST-0606772, AST-0907903]; TABASGO Foundation; US Department of Energy [DE-FC02-06ER41453, DE-FG02-08ER41563, NNX09AG54G]; NASA [NAS5-00136]; Sun Microsystems, Inc.; Hewlett-Packard Company; AutoScope Corporation; Lick Observatory; University of California; Sylvia & Jim Katzman Foundation FX We thank the Mission Operations team at Penn State University for scheduling so many UVOT SN Ia observations on short notice. We are grateful to Stephane Blondin for his efforts on behalf of the CfA Supernova Program, and X. Wang for categorization of NHV and NNN SNe Ia. P.A.M. thanks K. Krisciunas for assistance in obtaining information on specific supernovae. The research of A.V.F.'s supernova group at UC Berkeley is supported by National Science Foundation (NSF) grants AST-0607485 and AST-0908886, the TABASGO Foundation, US Department of Energy SciDAC grant DE-FC02-06ER41453, US Department of Energy grant DE-FG02-08ER41563, and Swift Guest Investigator grant NNX09AG54G. The work at PSU is sponsored by NASA contract NAS5-00136. KAIT and its ongoing operations were made possible by donations from Sun Microsystems, Inc., the Hewlett-Packard Company, AutoScope Corporation, Lick Observatory, the NSF, the University of California, the Sylvia & Jim Katzman Foundation, and the TABASGO Foundation. Supernova research at the Harvard College Observatory is supported in part by the NSF through grants AST-0606772 and AST-0907903. NR 96 TC 41 Z9 41 U1 1 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2010 VL 721 IS 2 BP 1627 EP 1655 DI 10.1088/0004-637X/721/2/1627 PG 29 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 654TP UT WOS:000282193600058 ER PT J AU Lanz, L Jones, C Forman, WR Ashby, MLN Kraft, R Hickox, RC AF Lanz, Lauranne Jones, Christine Forman, William R. Ashby, Matthew L. N. Kraft, Ralph Hickox, Ryan C. TI CONSTRAINING THE OUTBURST PROPERTIES OF THE SMBH IN FORNAX A THROUGH X-RAY, INFRARED, AND RADIO OBSERVATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: individual (NGC 1316); galaxies: structure; infrared: galaxies; radio continuum: galaxies; X-rays: galaxies ID SPITZER-SPACE-TELESCOPE; GALAXY NGC-1316 FORNAX; MULTIBAND IMAGING PHOTOMETER; SUPERMASSIVE BLACK-HOLE; ACTIVE GALACTIC NUCLEI; NEARBY GALAXIES; CENTAURUS-A; ABSOLUTE CALIBRATION; CHANDRA OBSERVATION; ELLIPTIC GALAXIES AB Combined Spitzer, Chandra, XMM-Newton, and VLA observations of the giant radio galaxy NGC 1316 (Fornax A) show a radio jet and X-ray cavities from active galactic nucleus (AGN) outbursts most likely triggered by a merger with a late-type galaxy at least 0.4 Gyr ago. We detect a weak nucleus with a spectral energy distribution typical of a low-luminosity AGN with a bolometric luminosity of 2.4 x 10(42) erg s(-1). We examine the Spitzer IRAC and MIPS images of NGC 1316. We find that the dust emission is strongest in regions with little or no radio emission and that the particularly large infrared luminosity relative to the galaxy's K-band luminosity implies an external origin for the dust. The inferred dust mass implies that the merger spiral galaxy had a stellar mass of (1-6) x 10(10) M(circle dot) and a gas mass of (2-4) x 10(9) M(circle dot). X-ray cavities in the Chandra and XMM-Newton images likely result from the expansion of relativistic plasma ejected by the AGN. The soft (0.5-2.0 keV) Chandra images show a small similar to 15 '' (1.6 kpc) cavity coincident with the radio jet, while the XMM-Newton image shows two large X-ray cavities lying 320 '' (34.8 kpc) east and west of the nucleus, each approximately 230 '' (25 kpc) in radius. Current radio observations do not show emission within these cavities. The radio lobes lie at radii of 14'.3 (93.3 kpc) and 15'.6 (101 kpc), more distant from the nucleus than the detected X-ray cavities. The relative morphology of the large scale 1.4 GHz and X-ray emission suggests they were products of two distinct outbursts, an earlier one creating the radio lobes and a later one producing the X-ray cavities. Alternatively, if a single outburst created both the X-ray cavities and the radio lobes, this would require that the radio morphology is not fully defined by the 1.4 GHz emission. For the more likely two outbursts scenarios, we use the buoyancy rise times to estimate an age for the more recent outburst that created the X-ray cavities of 0.1 Gyr and the PV work done by the expanding plasma that created the X-ray cavities to estimate the outburst's energy to be 10(58) erg. The present size and location of the radio lobes imply that the outburst that created them happened similar to 0.4 Gyr ago and released similar to 5 x 10(58) erg. C1 [Lanz, Lauranne; Jones, Christine; Forman, William R.; Ashby, Matthew L. N.; Kraft, Ralph; Hickox, Ryan C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hickox, Ryan C.] Univ Durham, Dept Phys, Durham DH1 3LE, England. RP Lanz, L (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM llanz@head.cfa.harvard.edu OI Lanz, Lauranne/0000-0002-3249-8224 FU Smithsonian Institution; Chandra X-ray Center; NASA [NNX07AQ18G] FX We are grateful to C. Horellou and J. H. Black for providing us with CO(2-1) intensities and for their comments regarding the molecular gas kinematics, Zhiyuan Li for his useful discussion on calculating masses, Dharam Lal for his assistance in creating the 4.89 GHz map, and to Ramesh Narayan for his comments. We thank the anonymous referee for the many comments that improved this work. This work was based on archival data obtained from the Spitzer Science Archive, the Chandra Data Archive, and the XMM-Newton Science Data Archive. Archived images were also obtained from the Hubble Legacy Archive, the NASA/IPAC Extragalactic Database, and the National Radio Astronomy Observatory Archive. We thank Z. Levay of the Space Telescope Science Institute for his assistance in obtaining the Hubble ACS image. This work was supported by the Smithsonian Institution, the Chandra X-ray Center, and NASA contract NNX07AQ18G. NR 69 TC 16 Z9 16 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2010 VL 721 IS 2 BP 1702 EP 1713 DI 10.1088/0004-637X/721/2/1702 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 654TP UT WOS:000282193600063 ER PT J AU Kafka, S Tappert, C Ribeiro, T Honeycutt, RK Hoard, DW Saar, S AF Kafka, S. Tappert, C. Ribeiro, T. Honeycutt, R. K. Hoard, D. W. Saar, S. TI LOW-STATE MAGNETIC STRUCTURES IN POLARS: NATURE OR NURTURE? SO ASTROPHYSICAL JOURNAL LA English DT Article DE novae, cataclysmic variables; stars: individual (BL Hyi, AM Her, ST LMi, VV Pup, EF Eri); stars: magnetic field ID EMISSION-LINE REGIONS; VARIABLE ST-LMI; AM-HERCULIS; CATACLYSMIC VARIABLES; X-RAY; VV-PUPPIS; BL HYI; SLINGSHOT PROMINENCES; ROCHE TOMOGRAPHY; PERIOD GAP AB We present an orbit-resolved study of the magnetic cataclysmic variable (MCV) BL Hyi in its low state, and we explore the origin of its H alpha emission line components, their properties, and their possible formation mechanism. We tentatively associate one of the line components with a high-velocity component also seen in the high state. We propose a scenario in which streaming prominence- like magnetic loops (super-prominences) are kept in place by magnetic field interactions between the white dwarf and the donor star and are responsible for the high-velocity line components in the Balmer lines. We also discuss how this is in accord with the standard scenario of the secular evolution for MCVs. Finally, we offer an observational test of our ideas and present challenges for future theoretical studies. C1 [Kafka, S.] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA. [Kafka, S.; Hoard, D. W.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Tappert, C.] Univ Valparaiso, Dept Fis & Astrofis, Valparaiso, Chile. [Ribeiro, T.] Univ Fed Santa Catarina, Dept Fis, BR-88040900 Florianopolis, SC, Brazil. [Honeycutt, R. K.] Indiana Univ, Dept Astron, Bloomington, IN 47405 USA. [Saar, S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kafka, S (reprint author), Carnegie Inst Washington, Dept Terr Magnetism, 5241 Broad Branch Rd NW, Washington, DC 20015 USA. EM skafka@dtm.ciw.edu OI Hoard, Donald W./0000-0002-6800-6519 NR 54 TC 5 Z9 5 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2010 VL 721 IS 2 BP 1714 EP 1724 DI 10.1088/0004-637X/721/2/1714 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 654TP UT WOS:000282193600064 ER PT J AU Agol, E Cowan, NB Knutson, HA Deming, D Steffen, JH Henry, GW Charbonneau, D AF Agol, Eric Cowan, Nicolas B. Knutson, Heather A. Deming, Drake Steffen, Jason H. Henry, Gregory W. Charbonneau, David TI THE CLIMATE OF HD 189733b FROM FOURTEEN TRANSITS AND ECLIPSES MEASURED BY SPITZER SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems ID HUBBLE-SPACE-TELESCOPE; HOT SUPER-EARTHS; EXTRASOLAR PLANET; ATMOSPHERIC CIRCULATION; TRANSMISSION SPECTRUM; INFRARED-EMISSION; TIMING VARIATIONS; SYSTEM HD-189733; ROTATION PERIOD; LIGHT CURVES AB We present observations of six transits and six eclipses of the transiting planet system HD 189733 taken with the Spitzer Space Telescope's Infrared Array Camera (IRAC) at 8 mu m, as well as a re-analysis of previously published data. We use several novel techniques in our data analysis, the most important of which is a new correction for the detector "ramp" variation with a double-exponential function, which performs better and is a better physical model for this detector variation. Our main scientific findings are (1) an upper limit on the variability of the dayside planet flux of 2.7% (68% confidence); (2) the most precise set of transit times measured for a transiting planet, with an average accuracy of 3 s; (3) a lack of transit-timing variations, excluding the presence of second planets in this system above 20% of the mass of Mars in low-order mean-motion resonance at 95% confidence; (4) a confirmation of the planet's phase variation, finding the night side is 64% as bright as the day side, as well as an upper limit on the nightside variability of 17% (68% confidence); (5) a better correction for stellar variability at 8 mu m causing the phase function to peak 3.5 hr before secondary eclipse, confirming that the advection and radiation timescales are comparable at the 8 mu m photosphere; (6) variation in the depth of transit, which possibly implies variations in the surface brightness of the portion of the star occulted by the planet, posing a fundamental limit on non-simultaneous multi-wavelength transit absorption measurements of planet atmospheres; (7) a measurement of the infrared limb darkening of the star, which is in good agreement with stellar atmosphere models; (8) an offset in the times of secondary eclipse of 69 s, which is mostly accounted for by a 31 s light-travel time delay and 33 s delay due to the shift of ingress and egress by the planet hot spot; this confirms that the phase variation is due to an offset hot spot on the planet; (9) a retraction of the claimed eccentricity of this system due to the offset of secondary eclipse, which is now just an upper limit; and (10) high-precision measurements of the parameters of this system. These results were enabled by the exquisite photometric precision of Spitzer IRAC; for repeat observations the scatter is less than 0.35 mmag over the 590 day timescale of our observations after decorrelating with detector parameters. C1 [Agol, Eric; Cowan, Nicolas B.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Agol, Eric] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93110 USA. [Agol, Eric] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93110 USA. [Knutson, Heather A.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Deming, Drake] NASA, Goddard Space Flight Ctr, Planetary Syst Lab, Greenbelt, MD 20771 USA. [Steffen, Jason H.] Fermilab Ctr Particle Astrophys, Batavia, IL 60510 USA. [Henry, Gregory W.] Tennessee State Univ, Ctr Excellence Informat Syst, Nashville, TN 37209 USA. [Charbonneau, David] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Agol, E (reprint author), Univ Washington, Dept Astron, Box 351580, Seattle, WA 98195 USA. RI Steffen, Jason/A-4320-2013; Agol, Eric/B-8775-2013; OI Agol, Eric/0000-0002-0802-9145; Charbonneau, David/0000-0002-9003-484X FU NASA; Miller Institute for Basic Research in Science; National Science Foundation [NSF PHY05-51164, 0645416] FX This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory (JPL), California Institute of Technology under contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. E.A. acknowledges the hospitality of the Institute for Theory and Computation at the Harvard-Smithsonian Center for Astrophysics, the Michigan Center for Theoretical Physics, and the Kavli Institute for Theoretical Physics where portions of this work were completed. H.A.K. is supported by a fellowship from the Miller Institute for Basic Research in Science. This research was supported in part by the National Science Foundation under grant No. NSF PHY05-51164 and CAREER grant No. 0645416. NR 70 TC 125 Z9 125 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2010 VL 721 IS 2 BP 1861 EP 1877 DI 10.1088/0004-637X/721/2/1861 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 654TP UT WOS:000282193600076 ER PT J AU Acciari, VA Aliu, E Arlen, T Beilicke, M Benbow, W Bottcher, M Bradbury, SM Buckley, JH Bugaev, V Butt, Y Byrum, K Cannon, A Celik, O Cesarini, A Chow, YC Ciupik, L Cogan, P Cui, W Daniel, MK Dickherber, R Ergin, T Falcone, A Fegan, SJ Finley, JP Fortin, P Fortson, L Furniss, A Gall, D Gibbs, K Gillanders, GH Godambe, S Grube, J Guenette, R Gyuk, G Hanna, D Hays, E Holder, J Horan, D Hui, CM Humensky, TB Imran, A Kaaret, P Karlsson, N Kertzman, M Kieda, D Kildea, J Konopelko, A Krawczynski, H Krennrich, F Lang, MJ LeBohec, S Maier, G McCann, A McCutcheon, M Millis, J Moriarty, P Mukherjee, R Nagai, T Ong, RA Otte, AN Pandel, D Perkins, JS Petry, D Pizlo, F Pohl, M Quinn, J Ragan, K Reyes, LC Reynolds, PT Roache, E Rose, HJ Schroedter, M Sembroski, GH Smith, AW Steele, D Swordy, SP Theiling, M Toner, JA Varlotta, A Vassiliev, VV Wagner, RG Wakely, SP Ward, JE Weekes, TC Weinstein, A Williams, DA Wissel, S Wood, M Zitzer, B AF Acciari, V. A. Aliu, E. Arlen, T. Beilicke, M. Benbow, W. Boettcher, M. Bradbury, S. M. Buckley, J. H. Bugaev, V. Butt, Y. Byrum, K. Cannon, A. Celik, O. Cesarini, A. Chow, Y. C. Ciupik, L. Cogan, P. Cui, W. Daniel, M. K. Dickherber, R. Ergin, T. Falcone, A. Fegan, S. J. Finley, J. P. Fortin, P. Fortson, L. Furniss, A. Gall, D. Gibbs, K. Gillanders, G. H. Godambe, S. Grube, J. Guenette, R. Gyuk, G. Hanna, D. Hays, E. Holder, J. Horan, D. Hui, C. M. Humensky, T. B. Imran, A. Kaaret, P. Karlsson, N. Kertzman, M. Kieda, D. Kildea, J. Konopelko, A. Krawczynski, H. Krennrich, F. Lang, M. J. LeBohec, S. Maier, G. McCann, A. McCutcheon, M. Millis, J. Moriarty, P. Mukherjee, R. Nagai, T. Ong, R. A. Otte, A. N. Pandel, D. Perkins, J. S. Petry, D. Pizlo, F. Pohl, M. Quinn, J. Ragan, K. Reyes, L. C. Reynolds, P. T. Roache, E. Rose, H. J. Schroedter, M. Sembroski, G. H. Smith, A. W. Steele, D. Swordy, S. P. Theiling, M. Toner, J. A. Varlotta, A. Vassiliev, V. V. Wagner, R. G. Wakely, S. P. Ward, J. E. Weekes, T. C. Weinstein, A. Williams, D. A. Wissel, S. Wood, M. Zitzer, B. TI VERITAS OBSERVATIONS OF A VERY HIGH ENERGY gamma-RAY FLARE FROM THE BLAZAR 3C 66A (vol 693, pg L104, 2009) SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Correction C1 [Acciari, V. A.; Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland. [Aliu, E.; Holder, J.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Aliu, E.; Holder, J.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Arlen, T.; Celik, O.; Chow, Y. C.; Fegan, S. J.; Ong, R. A.; Vassiliev, V. V.; Weinstein, A.; Wood, M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Beilicke, M.; Buckley, J. H.; Bugaev, V.; Dickherber, R.; Krawczynski, H.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Benbow, W.; Gibbs, K.; Kildea, J.; Roache, E.; Theiling, M.; Weekes, T. C.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Boettcher, M.] Ohio Univ, Inst Astrophys, Dept Phys & Astron, Athens, OH 45701 USA. [Bradbury, S. M.; Daniel, M. K.; Rose, H. J.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Butt, Y.; Ergin, T.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Byrum, K.; Smith, A. W.; Wagner, R. G.] Argonne Natl Lab, Argonne, IL 60439 USA. [Cannon, A.; Grube, J.; Quinn, J.; Ward, J. E.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Cesarini, A.; Gillanders, G. H.; Lang, M. J.; Toner, J. A.] Natl Univ Ireland, Sch Phys, Galway, Ireland. [Ciupik, L.; Fortson, L.; Gyuk, G.; Karlsson, N.; Steele, D.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA. [Cogan, P.; Guenette, R.; Hanna, D.; Maier, G.; McCann, A.; McCutcheon, M.; Ragan, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Cui, W.; Finley, J. P.; Gall, D.; Pizlo, F.; Sembroski, G. H.; Varlotta, A.; Zitzer, B.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Falcone, A.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Fortin, P.; Mukherjee, R.] Columbia Univ, Dept Phys & Astron, Barnard Coll, New York, NY 10027 USA. [Furniss, A.; Otte, A. N.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Furniss, A.; Otte, A. N.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Godambe, S.; Hui, C. M.; Kieda, D.; LeBohec, S.] Univ Utah, Dept Phys, Salt Lake City, UT 84112 USA. [Hays, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Horan, D.] Ecole Polytech, CNRS, Lab Leprince Ringuet, IN2P3, F-91128 Palaiseau, France. [Humensky, T. B.; Swordy, S. P.; Wakely, S. P.; Wissel, S.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Imran, A.; Krennrich, F.; Nagai, T.; Pohl, M.; Schroedter, M.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Kaaret, P.; Pandel, D.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. [Konopelko, A.] Pittsburg State Univ, Dept Phys, Pittsburg, KS 66762 USA. [Millis, J.] Anderson Univ, Dept Phys, Anderson, IN 46012 USA. [Petry, D.] European So Observ, D-85748 Garching, Germany. [Reyes, L. C.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland. RP Acciari, VA (reprint author), Galway Mayo Inst Technol, Dept Life & Phys Sci, Dublin Rd, Galway, Ireland. EM jperkins@cfa.harvard.edu RI Hays, Elizabeth/D-3257-2012; Daniel, Michael/A-2903-2010 OI Daniel, Michael/0000-0002-8053-7910 NR 3 TC 2 Z9 2 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD OCT 1 PY 2010 VL 721 IS 2 BP L203 EP L204 DI 10.1088/2041-8205/721/2/L203 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 654TB UT WOS:000282192200027 ER PT J AU Besla, G Kallivayalil, N Hernquist, L van der Marel, RP Cox, TJ Keres, D AF Besla, G. Kallivayalil, N. Hernquist, L. van der Marel, R. P. Cox, T. J. Keres, D. TI SIMULATIONS OF THE MAGELLANIC STREAM IN A FIRST INFALL SCENARIO SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: halos; galaxies: individual (Magellanic Clouds); galaxies: kinematics and dynamics ID HIGH-VELOCITY CLOUDS; N-BODY SIMULATIONS; PROPER MOTION; MILKY-WAY; HI SURVEY; GALAXIES; ORIGIN; HALO; KINEMATICS; SYSTEM AB Recent high-precision proper motions from the Hubble Space Telescope suggest that the Large and Small Magellanic Clouds (LMC and SMC, respectively) are either on their first passage or on an eccentric long period (>6 Gyr) orbit about the Milky Way (MW). This differs markedly from the canonical picture in which the Clouds travel on a quasi-periodic orbit about the MW (period of similar to 2 Gyr). Without a short-period orbit about the MW, the origin of the Magellanic Stream, a young (1-2 Gyr old) coherent stream of H I gas that trails the Clouds similar to 150 degrees across the sky, can no longer be attributed to stripping by MW tides and/or ram pressure stripping by MW halo gas. We propose an alternative formation mechanism in which material is removed by LMC tides acting on the SMC before the system is accreted by the MW. We demonstrate the feasibility and generality of this scenario using an N-body/smoothed particle hydrodynamics simulation with cosmologically motivated initial conditions constrained by the observations. Under these conditions, we demonstrate that it is possible to explain the origin of the Magellanic Stream in a first infall scenario. This picture is generically applicable to any gas-rich dwarf galaxy pair infalling toward a massive host or interacting in isolation. C1 [Besla, G.; Hernquist, L.; Keres, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kallivayalil, N.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [van der Marel, R. P.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Cox, T. J.] Carnegie Observ, Pasadena, CA 91101 USA. RP Besla, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM gbesla@cfa.harvard.edu NR 49 TC 90 Z9 90 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD OCT 1 PY 2010 VL 721 IS 2 BP L97 EP L101 DI 10.1088/2041-8205/721/2/L97 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 654TB UT WOS:000282192200005 ER PT J AU Cassano, R Ettori, S Giacintucci, S Brunetti, G Markevitch, M Venturi, T Gitti, M AF Cassano, R. Ettori, S. Giacintucci, S. Brunetti, G. Markevitch, M. Venturi, T. Gitti, M. TI ON THE CONNECTION BETWEEN GIANT RADIO HALOS AND CLUSTER MERGERS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: clusters: general; radiation mechanisms: non-thermal; radio continuum: general; X-rays: galaxies: clusters ID GALAXY CLUSTERS; REACCELERATION MODEL; SAMPLE; SUBSTRUCTURE; EVOLUTION; EMISSION; PERSEUS AB The frequently observed association between giant radio halos (RHs) and merging galaxy clusters has driven present theoretical models of non-thermal emission from galaxy clusters, which are based on the idea that the energy dissipated during cluster-cluster mergers could power the formation of RHs. To quantitatively test the merger-halo connection, we present the first statistical study based on deep radio data and X-ray observations of a complete X-ray-selected sample of galaxy clusters with X-ray luminosity >= 5 x 10(44) erg s(-1) and redshift 0.2 <= z <= 0.32. Using several methods to characterize cluster substructures, namely, the power ratios, centroid shift, and X-ray brightness concentration parameter, we show that clusters with and without RH can be quantitatively differentiated in terms of their dynamical properties. In particular, we confirm that RHs are associated with dynamically disturbed clusters and clusters without RH are more "relaxed," with only a couple of exceptions where a disturbed cluster does not exhibit a halo. C1 [Cassano, R.; Giacintucci, S.; Brunetti, G.; Venturi, T.] IRA, INAF, I-40129 Bologna, Italy. [Cassano, R.; Giacintucci, S.; Markevitch, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ettori, S.; Gitti, M.] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy. [Ettori, S.] Ist Nazl Fis Nucl, Sez Bologna, I-40127 Bologna, Italy. RP Cassano, R (reprint author), IRA, INAF, Via Gobetti 101, I-40129 Bologna, Italy. RI Ettori, Stefano/N-5004-2015; OI Ettori, Stefano/0000-0003-4117-8617; Venturi, Tiziana/0000-0002-8476-6307; Brunetti, Gianfranco/0000-0003-4195-8613; Gitti, Myriam/0000-0002-0843-3009; Cassano, Rossella/0000-0003-4046-0637 FU INAF [PRIN-INAF2007, PRIN-INAF2008]; ASI-INAF [I/088/06/0]; NASA [ARO-11017X, G09-0133X] FX We thank the referee for useful comments. This work was partially supported by INAF under grants PRIN-INAF2007 and PRIN-INAF2008, and by ASI-INAF under grant I/088/06/0. Support was also provided by NASA via Chandra grants ARO-11017X and G09-0133X. R.C. and G.B. thank the Harvard-Smithsonian Center for Astrophysics for its hospitality. NR 28 TC 117 Z9 117 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD OCT 1 PY 2010 VL 721 IS 2 BP L82 EP L85 DI 10.1088/2041-8205/721/2/L82 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 654TB UT WOS:000282192200002 ER PT J AU Currie, T Bailey, V Fabrycky, D Murray-Clay, R Rodigas, T Hinz, P AF Currie, Thayne Bailey, Vanessa Fabrycky, Daniel Murray-Clay, Ruth Rodigas, Timothy Hinz, Phil TI HIGH-CONTRAST 3.8 mu m IMAGING OF THE BROWN DWARF/PLANET-MASS COMPANION TO GJ 758 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE brown dwarfs ID YOUNG SUBSTELLAR COMPANION; EXTRASOLAR GIANT PLANETS; HR 8799; BINARY-SYSTEM; DWARFS; DISCOVERY; STARS; DISK; SUN; AGE AB We present L'-band (3.8 mu m) MMT/Clio high-contrast imaging data for the nearby star GJ 758, which was recently reported by Thalmann et al. to have one-possibly two-faint comoving companions (GJ 758B and "C," respectively). GJ 758B is detected in two distinct data sets. Additionally, we report a possible detection of the object identified by Thalmann et al. as " GJ 758C" in our more sensitive data set, though it is likely a residual speckle. However, if it is the same object as that reported by Thalmann et al. it cannot be a companion in a bound orbit. GJ 758B has an H - L' color redder than nearly all known L-T8 dwarfs. Based on comparisons with the COND evolutionary models, GJ 758B has T(e) similar to 560 K(-90K)(+150K) and a mass ranging from similar to 10-20 M(J) if it is similar to 1 Gyr old to similar to 25-40 M(J) if it is 8.7 Gyr old. GJ 758B is likely in a highly eccentric orbit, e similar to 0.73(-0.21)(+ 0.12), with a semimajor axis of similar to 44AU(-14AU)(+32AU). Though GJ 758B is sometimes discussed within the context of exoplanet direct imaging, its mass is likely greater than the deuterium-burning limit and its formation may resemble that of binary stars rather than that of Jovian-mass planets. C1 [Currie, Thayne] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Bailey, Vanessa; Rodigas, Timothy; Hinz, Phil] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Fabrycky, Daniel; Murray-Clay, Ruth] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Currie, T (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. FU NASA; Michelson Fellowship; Institute for Theory and Computation Fellowship FX We thank the anonymous referee and Adam Kraus for suggestions that strengthened this Letter and Adam Burgasser, Marc Kuchner, Scott Kenyon, and Jonathan Irwin for other useful discussions. T.C. is supported by a NASA Postdoctoral Fellowship, D.F. is supported by a Michelson Fellowship, and R.M.-C. is supported by an Institute for Theory and Computation Fellowship. NR 40 TC 15 Z9 15 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD OCT 1 PY 2010 VL 721 IS 2 BP L177 EP L181 DI 10.1088/2041-8205/721/2/L177 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 654TB UT WOS:000282192200022 ER PT J AU Kilic, M Prieto, CA Brown, WR Agueros, MA Kenyon, SJ Camilo, F AF Kilic, Mukremin Prieto, Carlos Allende Brown, Warren R. Agueeros, M. A. Kenyon, S. J. Camilo, Fernando TI ACCURATE MASSES FOR THE PRIMARY AND SECONDARY IN THE ECLIPSING WHITE DWARF BINARY NLTT 11748 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE stars: individual (NLTT 11748); stars: low-mass; white dwarfs ID STARS; DISCOVERY; EVOLUTION; COMPANION; HELIUM AB We measure the radial velocity curve of the eclipsing detached white dwarf binary NLTT 11748. The primary exhibits velocity variations with a semi-amplitude of 273 km s(-1) and an orbital period of 5.641 hr. We do not detect any spectral features from the secondary star or any spectral changes during the secondary eclipse. We use our composite spectrum to constrain the temperature and surface gravity of the primary to be T(eff) = 8690 +/- 140 K and log g = 6.54 +/- 0.05, which correspond to a mass of 0.18 M(circle dot). For an inclination angle of 89 degrees.9 derived from the eclipse modeling, the mass function requires a 0.76 M(circle dot) companion. The merger time for the system is 7.2 Gyr. However, due to the extreme mass ratio of 0.24, the binary will most likely create an AM CVn system instead of a merger. C1 [Kilic, Mukremin; Brown, Warren R.; Kenyon, S. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Prieto, Carlos Allende] Inst Astrofis Canarias, Tenerife 38205, Spain. [Agueeros, M. A.; Camilo, Fernando] Columbia Univ, Dept Astron, New York, NY 10027 USA. RP Kilic, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mkilic@cfa.harvard.edu RI Agueros, Marcel/K-7998-2014; OI Agueros, Marcel/0000-0001-7077-3664; Kenyon, Scott/0000-0003-0214-609X FU NASA; NSF [AST-0602099]; US National Science Foundation; Caltech FX We thank the referee S. Vennes for helpful suggestions, D. Koester for kindly providing WD model spectra, and S. Ransom for his help with the GBT observations. Support for this work was provided by NASA through the Spitzer Space Telescope Fellowship Program, under an award from Caltech. M.A.A. is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-0602099. The Robert C. Byrd Green Bank Telescope is operated by the National Radio Astronomy Observatory, which is a facility of the US National Science Foundation operated under cooperative agreement by Associated Universities, Inc. NR 27 TC 18 Z9 18 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD OCT 1 PY 2010 VL 721 IS 2 BP L158 EP L162 DI 10.1088/2041-8205/721/2/L158 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 654TB UT WOS:000282192200018 ER PT J AU Sanchez-Monge, A Palau, A Estalella, R Kurtz, S Zhang, QZ Di Francesco, J Shepherd, D AF Sanchez-Monge, Alvaro Palau, Aina Estalella, Robert Kurtz, Stan Zhang, Qizhou Di Francesco, James Shepherd, Debra TI IRAS 22198+6336: DISCOVERY OF AN INTERMEDIATE-MASS HOT CORE SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE ISM: individual objects (IRAS 22198+6336); ISM: lines and bands; radio continuum: ISM; stars: formation ID STAR-FORMING REGIONS; BIPOLAR OUTFLOWS; JET HH-211; H2O MASERS; EMISSION; OBJECTS; PROTOSTARS; POPULATION; RESOLUTION; SAMPLE AB We present new Submillimeter Array and Plateau de Bure Interferometer observations of the intermediate-mass object IRAS 22198+6336 in the millimeter continuum and in several molecular line transitions. The millimeter continuum emission reveals a strong and compact source with a mass of similar to 5M(circle dot) and with properties of Class 0 objects. CO emission shows an outflow with a quadrupolar morphology centered on the position of the dust condensation. The CO outflow emission seems to come from two distinct outflows, one of them associated with SiO outflow emission. A large set of molecular lines has been detected toward a compact dense core clearly coincident with the compact millimeter source, and showing a velocity gradient perpendicular to the outflow traced by CO and SiO. The chemically rich spectrum and the rotational temperatures derived from CH(3)CN and CH(3)OH (100-150 K) indicate that IRAS 22198+6336 is harboring one of the few intermediate-mass hot cores known at present. C1 [Sanchez-Monge, Alvaro; Estalella, Robert] Univ Barcelona, Inst Ciencies Cosmos, Dept Astron & Meteorol, IEEC UB, E-08028 Barcelona, Spain. [Palau, Aina] Fac Ciencies, Inst Ciencies Espai, CSIC IEEC, E-08193 Barcelona, Spain. [Kurtz, Stan] Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Morelia 58090, Michoacan, Mexico. [Zhang, Qizhou] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Di Francesco, James] Herzberg Inst Astrophys, Conseil Natl Rech Canada, Victoria, BC, Canada. [Shepherd, Debra] Natl Radio Astron Observ, Socorro, NM 87801 USA. RP Sanchez-Monge, A (reprint author), Univ Barcelona, Inst Ciencies Cosmos, Dept Astron & Meteorol, IEEC UB, Marti & Franques 1, E-08028 Barcelona, Spain. EM asanchez@am.ub.es OI Zhang, Qizhou/0000-0003-2384-6589 FU Spanish MICINN [AYA2008-06189-C03, ESP2007-65475-C02-02, Consolider-CSD2006-00070]; JAE-Doc CSIC; DGAPA-UNAM [IN101310]; European Social Fund FX We thank the anonymous referee for his/her useful comments. A.S-M. and A.P. are grateful to Esteban Araya for his help in analyzing the data, to Francesco Fontani and Asuncion Fuente for kindly providing complementary data, and also to Rob Gutermuth for his help with Spitzer data. A.S-M., A.P., and R.E. are supported by the Spanish MICINN grant AYA2008-06189-C03 (co-funded with FEDER funds). A.P. is supported by a JAE-Doc CSIC fellowship co-funded with the European Social Fund. This research has been partially funded by Spanish MICINN under the ESP2007-65475-C02-02 and Consolider-CSD2006-00070 grants. S.K. is partially supported by the DGAPA-UNAM grant IN101310. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. NR 36 TC 17 Z9 17 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD OCT 1 PY 2010 VL 721 IS 2 BP L107 EP L111 DI 10.1088/2041-8205/721/2/L107 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 654TB UT WOS:000282192200007 ER PT J AU Wiersema, K Farrell, SA Webb, NA Servillat, M Maccarone, TJ Barret, D Godet, O AF Wiersema, K. Farrell, S. A. Webb, N. A. Servillat, M. Maccarone, T. J. Barret, D. Godet, O. TI A REDSHIFT FOR THE INTERMEDIATE-MASS BLACK HOLE CANDIDATE HLX-1: CONFIRMATION OF ITS ASSOCIATION WITH THE GALAXY ESO 243-49 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE accretion, accretion disks; X-rays: binaries; X-rays: individual (ESO 243-49 HLX-1) ID X-RAY SOURCES; XMM-NEWTON OBSERVATIONS; STATE AB In this Letter, we report a spectroscopic confirmation of the association of HLX-1, the brightest ultra-luminous X-ray (ULX) source, with the galaxy ESO 243-49. At the host galaxy distance of 95 Mpc, the maximum observed 0.2-10 keV luminosity is 1.2 x 10(42) erg s(-1). This luminosity is similar to 400 times above the Eddington limit for a 20 M(circle dot) black hole and has been interpreted as implying an accreting intermediate-mass black hole with a mass in excess of 500 M(circle dot) (assuming that the luminosity is a factor of 10 above the Eddington value). However, a number of other ULX sources have been later identified as background active galaxies or foreground sources. It has recently been claimed that HLX-1 could be a quiescent neutron star X-ray binary at a Galactic distance of only 2.5 kpc, so a definitive association with the host galaxy is crucial in order to confirm the nature of the object. Here, we report the detection of the Ha emission line for the recently identified optical counterpart at a redshift consistent with that of ESO 243-49. This finding definitively places HLX-1 inside ESO 243-49, confirming the extreme maximum luminosity and strengthening the case for it containing an accreting intermediate-mass black hole of more than 500 M(circle dot). C1 [Wiersema, K.; Farrell, S. A.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Webb, N. A.; Barret, D.; Godet, O.] Univ Toulouse, UPS, CESR, F-31028 Toulouse 9, France. [Webb, N. A.; Barret, D.; Godet, O.] CNRS, UMR 5187, F-31028 Toulouse, France. [Servillat, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Maccarone, T. J.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. RP Wiersema, K (reprint author), Univ Leicester, Dept Phys & Astron, Univ Rd, Leicester LE1 7RH, Leics, England. FU National Science Foundation; STFC; European Union [215212]; [AR9-0013X]; [GO9-0102X] FX We thank M. C. Miller and the anonymous referees for their comments that helped to improve this Letter. We thank Tim de Zeeuw for granting us the VLT DDT observations. Based on observations made with ESO Telescopes at the Paranal Observatory under program ID 284.D-5008. IRAF is distributed by the National Optical Astronomy Observatories, which are operated by the Association of Universities for Research in Astronomy, Inc., under cooperative agreement with the National Science Foundation. S.A.F., K.W., and T.J.M. acknowledge STFC funding. T.J.M. thanks the European Union FP7 for support through grant 215212 Black Hole Universe. M.S. is supported in part by Chandra grants AR9-0013X and GO9-0102X. NR 19 TC 45 Z9 45 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD OCT 1 PY 2010 VL 721 IS 2 BP L102 EP L106 DI 10.1088/2041-8205/721/2/L102 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 654TB UT WOS:000282192200006 ER PT J AU Xu, X Narayanan, D Walker, C AF Xu, X. Narayanan, D. Walker, C. TI MOLECULAR DISK PROPERTIES IN EARLY-TYPE GALAXIES SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: elliptical and lenticular, cD; galaxies: evolution; galaxies: kinematics and dynamics; ISM: molecules ID PARTICLE HYDRODYNAMICS SIMULATIONS; CO-TO-H-2 CONVERSION FACTOR; ELLIPTIC GALAXIES; CO OBSERVATIONS; GALACTIC WINDS; STAR-FORMATION; BLACK-HOLES; H-I; GAS; MERGERS AB We study the simulated CO emission from elliptical galaxies formed in the mergers of gas-rich disk galaxies. The cold gas not consumed in the merger-driven starburst quickly resettles into a disk-like configuration. By analyzing a variety of arbitrary merger orbits that produce a range of fast-to slow-rotating remnants, we find that molecular disk formation is a fairly common consequence of gas-rich galaxy mergers. Hence, if a molecular disk is observed in an early-type merger remnant, it is likely the result of a "wet merger" rather than a "dry merger." We compare the physical properties from our simulated disks (e. g., size and mass) and find reasonably good agreement with recent observations. Finally, we discuss the detectability of these disks as an aid to future observations. C1 [Xu, X.; Walker, C.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Narayanan, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Xu, X (reprint author), Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA. EM xxu@as.arizona.edu NR 50 TC 6 Z9 6 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD OCT 1 PY 2010 VL 721 IS 2 BP L112 EP L116 DI 10.1088/2041-8205/721/2/L112 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 654TB UT WOS:000282192200008 ER PT J AU Li, S Wang, DJ Gu, XD McShea, WJ AF Li, Sheng Wang, Dajun Gu, Xiaodong McShea, William J. TI Beyond pandas, the need for a standardized monitoring protocol for large mammals in Chinese nature reserves SO BIODIVERSITY AND CONSERVATION LA English DT Article DE Giant panda; Monitoring; Camera-trapping; Large mammals; China ID ESTIMATING SITE OCCUPANCY; PHOTOGRAPHIC RATES; ESTIMATE DENSITIES; CRYPTIC MAMMALS; CAMERA TRAPS; WILDLIFE; TIGERS; CONSERVATION; POPULATIONS; LANDSCAPE AB Monitoring programs are important for effective conservation and management programs. However, most of these programs rely on indirect sign surveys of elusive animals that often leave cryptic signs of their presence. In Sichuan Province, China, sign surveys are oriented mainly toward giant panda (Ailuropoda melanoleuca) populations but also are used to track other nationally listed species. We have developed and tested a monitoring system based on camera-trapping that can detect a wide range of large, terrestrial mammal and bird species within the reserves of Sichuan. This system is embedded within current protected area patrolling activities and relies on a partnership of management agencies, universities and international organizations. The international organizations and national universities primarily provide the training and assist with study design and data analysis. Data management and access is controlled at the regional level by the appropriate state agencies. Limitations to this system include the need for additional training and support to less developed reserves and the long-term availability of funds to support field staff. However, the potential return on investment is a consistent tracking of multiple species across diverse set of reserves, facilitating comparative analysis of results that will assist in adaptive management throughout the region. C1 [Li, Sheng; McShea, William J.] Smithsonian Conservat Biol Inst, Ctr Conservat Ecol, Front Royal, VA 22630 USA. [Li, Sheng; Wang, Dajun] Peking Univ, Coll Life Sci, Ctr Nat & Soc, Beijing 100871, Peoples R China. [Gu, Xiaodong] Sichuan Wildlife Conservat Management & Survey St, Sichuan Forestry Dept, Chengdu 610081, Peoples R China. RP Li, S (reprint author), Smithsonian Conservat Biol Inst, Ctr Conservat Ecol, 1500 Remount Rd, Front Royal, VA 22630 USA. EM lis@si.edu FU Smithsonian's National Zoological Park; Friends of the National Zoo; Peking University; Sichuan Forestry Department; China Wildlife Conservation Association; World Wildlife Fund China FX This project was supported by Smithsonian's National Zoological Park, Friends of the National Zoo, Peking University, Sichuan Forestry Department, China Wildlife Conservation Association, and World Wildlife Fund China. We thank Tangjiahe NR and Wolong NR for hosting the training courses and workshops, and all the reserve staffs that assisted with program management, data collection and logistic support. We also thank George B. Schaller and Colby Loucks for reviewing our manuscript and providing valuable comments. We had fruitful discussions with Lu Zhi, Wang Hongjia, Gu Haijun and Dai Bo on this project and the manuscript. NR 45 TC 9 Z9 22 U1 5 U2 35 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0960-3115 J9 BIODIVERS CONSERV JI Biodivers. Conserv. PD OCT PY 2010 VL 19 IS 11 BP 3195 EP 3206 DI 10.1007/s10531-010-9886-x PG 12 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 663GG UT WOS:000282870700011 ER PT J AU Boyer, AG James, HF Olson, SL Grand-Mackie, JA AF Boyer, Alison G. James, Helen F. Olson, Storrs L. Grand-Mackie, Jack A. TI Long-term ecological change in a conservation hotspot: the fossil avifauna of Me Aure Cave, New Caledonia SO BIODIVERSITY AND CONSERVATION LA English DT Article DE Birds; Deforestation; Extinction; Owl pellet; Pacific islands; Radiocarbon; Sclerophyll forest; Subfossil; Turnix ID CERVUS-TIMORENSIS-RUSSA; NATIVE SCLEROPHYLL FOREST; SPECIES RICHNESS; EXTINCTION; ISLANDS; AREAS; BP AB Through the continuing accumulation of fossil evidence, it is clear that first human arrival on islands around the world was linked to a rise in the extinction rate for vertebrates. Bones in human-era fossil sites can also reveal changes in the composition and structure of ecological communities due to human environmental impacts. New Caledonia is a large and biogeographically distinct island in the southwest Pacific and is considered a critical priority for biodiversity conservation. We examined fossil birds from the Me Aure Cave site (WMD007), located in lowland dry forest on the west coast of New Caledonia. Accumulation of bird skeletal material in the cave was primarily through deposition in barn owl (Tyto alba) pellets. The site recorded the island-wide extinction of two species and extirpation of at least two other species from the lowlands in the past 1200 years. Species richness of birds in the stratigraphic deposit was quite high, reflecting the catholic diet of barn owls on islands, and many species have continued to persist near the site despite loss and degradation of the dry forest. However, we found substantial turnover in relative abundance of species in the cave deposit, with edge and open country birds becoming more common through time. These changes may reflect the severe reduction of dry forest habitat during the colonial period. This work provides a temporal record of avifaunal and environmental change in the threatened dry forest habitat that should be particularly informative for ongoing conservation and restoration efforts. C1 [Boyer, Alison G.] Yale Univ, Dept Ecol & Evolutionary Biol, New Haven, CT 06520 USA. [Boyer, Alison G.; James, Helen F.; Olson, Storrs L.] Smithsonian Inst, Natl Museum Nat Hist, Div Birds, MRC 116, Washington, DC 20013 USA. [Grand-Mackie, Jack A.] Univ Auckland, Sch Geog & Environm, Auckland 1, New Zealand. RP Boyer, AG (reprint author), Yale Univ, Dept Ecol & Evolutionary Biol, 165 Prospect St, New Haven, CT 06520 USA. EM alison.boyer@yale.edu OI Boyer, Alison/0000-0002-4252-9725 FU Smithsonian Institution; NMNH; National Science Foundation [DBI-0805669] FX We are grateful to F. Desmoulins and the Programme de Conservation des Forets Seches for providing bird survey data from the Deux Freres forest and to Mr. G. SantaCroce for access to the Me Aure Cave site. P. Maurizot and C. Sand provided valuable advice that enabled our fieldwork in New Caledonia. We thank A. Wiley for pretreatment of the barn owl bones for radiocarbon dating. We thank D. Steadman and curatorial staff at the Florida Museum of Natural History and the National Museum of Natural History (NMNH) for their assistance. Funding was provided by a Smithsonian Institution Postdoctoral Fellowship to AGB and a NMNH grant to HFJ and AGB. The project was also partially supported by a National Science Foundation Postdoctoral Research Fellowship in Biological Informatics (DBI-0805669) to AGB. NR 61 TC 7 Z9 7 U1 1 U2 16 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0960-3115 J9 BIODIVERS CONSERV JI Biodivers. Conserv. PD OCT PY 2010 VL 19 IS 11 BP 3207 EP 3224 DI 10.1007/s10531-010-9887-9 PG 18 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 663GG UT WOS:000282870700012 ER PT J AU Baeza, JA Piantoni, C AF Baeza, J. A. Piantoni, C. TI Sexual System, Sex Ratio, and Group Living in the Shrimp Thor amboinensis (De Man): Relevance to Resource-Monopolization and Sex-Allocation Theories SO BIOLOGICAL BULLETIN LA English DT Article ID LYSMATA-WURDEMANNI CARIDEA; LIFE-HISTORY; HERMAPHRODITIC SHRIMP; MATING TACTICS; DECAPODA; ANEMONE; HIPPOLYTIDAE; EVOLUTION; ANIMALS; CRUSTACEANS AB The sexual system of the symbiotic shrimp Thor amboinensis is described, along with observations on sex ratio and host-use pattern of different populations. We used a comprehensive approach to elucidate the previously unknown sexual system of this shrimp. Dissections, scanning electron microscopy, size-frequency distribution analysis, and laboratory observations demonstrated that T amboinensis is a protandric hermaphrodite: shrimp first mature as males and change into females later in life. Thor amboinensis inhabited the large and structurally heterogeneous sea anemone Stichoclactyla helianthus in large groups (up to 11 individuals) more frequently than expected by chance alone. Groups exhibited no particularly complex social structure and showed male-biased sex ratios more frequently than expected by chance alone. The adult sex ratio was male-biased in the four separate populations studied, one of them being thousands of kilometers apart from the others. This study supports predictions central to theories of resource monopolization and sex allocation. Dissections demonstrated that unusually large males were parasitized by an undescribed species of isopod (family Entoniscidae). Infestation rates were similarly low in both sexes (approximate to 11%-12%). The available information suggests that T. amboinensis uses pure search promiscuity as a mating system. This hypothesis needs to be formally tested with mating behavior observations and field measurements on the movement pattern of both sexes of the species. Further detailed studies on the lifestyle and sexual system of all the species within this genus and the development of a molecular phylogeny are necessary to elucidate the evolutionary history of gender expression in the genus Thor. C1 [Baeza, J. A.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Baeza, J. A.] Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. [Baeza, J. A.] Univ Catolica Norte, Fac Ciencias Mar, Dept Biol Marina, Larrondo 1281, Coquimbo, Chile. [Piantoni, C.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. [Piantoni, C.] Univ Sao Paulo, Inst Biociencias, Dept Fisiol, BR-05508900 Sao Paulo, Brazil. RP Baeza, JA (reprint author), Smithsonian Trop Res Inst, Apartado Postal 0843-03092, Balboa, Ancon, Panama. EM baezaa@si.edu OI Piantoni, Carla/0000-0002-1201-0041; Baeza, Juan Antonio/0000-0002-2573-6773 FU Marine Science Network; Smithsonian Institution through the Johnson and Hunterdon Oceanographic Research Endowment; National Geographic Society; Smithsonian Marine Station; Smithsonian Tropical Research Institute (STRI, Panama) FX We thank Sherry Reed and Narrisa Bax for their help during tedious hours of diving under harsh conditions while sampling sea anemones. We are also grateful to Mike Carpenter for his patience and help with the scheduling of diving trips and experimental work at CBC. Special thanks to Klaus Ruetzler, Tuck Hines, and Valerie Paul for their continuous support and funding for traveling to Belize. Jeff Shields and CRUST-L members were most helpful with identification of the parasite. Logistical support from Diane and Mark Littler and Barrett Brooks at Carrie Bow Cay, and James D. Reimer, Yoshikatsu Nakano, Yoshihisa Fujita, Obushi Masami, and Takuma Fujii at Okinawa, is deeply appreciated. We greatly appreciate Scott Whittaker's help with the SEM work. This research was funded by a Marine Science Network Grant from the Smithsonian Institution through the Johnson and Hunterdon Oceanographic Research Endowment (to JAB and Candy Feller) and by a Committee for Research and Exploration Grant of the National Geographic Society. Support from the Smithsonian Marine Station (Fort Pierce, Florida) Fellowship and Smithsonian Tropical Research Institute (STRI, Panama) Marine Fellowship is appreciated. Dr. Raymond T. Bauer and two anonymous referees critically reviewed the English as well as the content and provided very helpful comments. This article is CCRE and SMSFP contribution numbers 887 and 831, respectively. NR 62 TC 17 Z9 21 U1 2 U2 9 PU MARINE BIOLOGICAL LABORATORY PI WOODS HOLE PA 7 MBL ST, WOODS HOLE, MA 02543 USA SN 0006-3185 EI 1939-8697 J9 BIOL BULL-US JI Biol. Bull. PD OCT PY 2010 VL 219 IS 2 BP 151 EP 165 PG 15 WC Biology; Marine & Freshwater Biology SC Life Sciences & Biomedicine - Other Topics; Marine & Freshwater Biology GA 672YU UT WOS:000283625000008 PM 20972260 ER PT J AU Malo, AF Martinez-Pastor, F Alaks, G Dubach, J Lacy, RC AF Malo, Aurelio F. Martinez-Pastor, Felipe Alaks, Glen Dubach, Jean Lacy, Robert C. TI Effects of Genetic Captive-Breeding Protocols on Sperm Quality and Fertility in the White-Footed Mouse SO BIOLOGY OF REPRODUCTION LA English DT Article DE conservation breeding; docility; genetic adaptation to captivity; inbreeding depression; mean kinship; Peromyscus leucopus; reproductive success; testosterone ID G-DORCAS-NEGLECTA; INBREEDING DEPRESSION; OSMOTIC TOLERANCE; FLUCTUATING ASYMMETRY; CONSERVATION PROGRAMS; NATURAL-POPULATIONS; MEMBRANE INTEGRITY; EJACULATE QUALITY; GAZELLA-CUVIERI; DOMESTIC CAT AB Mice (Peromyscus leucopus noveboracensis) from a captive-breeding program were used to test the effects of three genetic breeding protocols (minimizing mean kinship [MK], random breeding, and selection for docility [DOC]) and inbreeding levels on sperm traits and fertility. Earlier, in generation 8, one DOC replicate went extinct because of poor reproductive success. By generation 10, spermatozoa from DOC mice had more acrosome and midpiece abnormalities, which were shown to be strong determinants of fertility, as well as lower sperm production and resistance to osmotic stress. In addition, determinants of fertility, including male and female components, were assessed in a comprehensive manner. Results showed that the probability (P) of siring litters is determined by sperm number, sperm viability, and midpiece and acrosome abnormalities; that the P of siring one versus two litters is determined by tail abnormalities; and that the total number of offspring is influenced by female size and proportion of normal sperm, showing the relative importance of different sperm traits on fertility. On average, males with 20% normal sperm sired one pup per litter, and males with 70% normal sperm sired eight pups per litter. Interestingly, the proportion of normal sperm was affected by docility but not by relatively low inbreeding. However, inbreeding depression in sperm motility was detected. In the MK group, inbreeding depression not only affected sperm motility but also fertility: An increase in the coefficient of inbreeding (f) of 0.03 reduced sperm motility by 30% and translated into an offspring reduction of three pups in second litters. A genetic load of 48 fecundity equivalents was calculated. C1 [Malo, Aurelio F.] Smithsonian Inst, Natl Zool Pk, Ctr Conservat & Evolutionary Genet, Washington, DC 20008 USA. [Malo, Aurelio F.; Martinez-Pastor, Felipe; Alaks, Glen; Dubach, Jean; Lacy, Robert C.] Chicago Zool Soc, Dept Conservat Sci, Brookfield, IL USA. [Malo, Aurelio F.] Univ London Imperial Coll Sci Technol & Med, Sect Ecol & Evolut, Ascot, Berks, England. [Martinez-Pastor, Felipe] Univ Leon, ITRA ULE, INDEGSAL, E-24071 Leon, Spain. [Martinez-Pastor, Felipe] UCLM CSIC JCCM, IREC, Natl Wildlife Res Inst, Biol Reprod Grp, Albacete, Spain. RP Malo, AF (reprint author), Smithsonian Inst, Natl Zool Pk, Ctr Conservat & Evolutionary Genet, Washington, DC 20008 USA. EM a.malo@imperial.ac.uk RI Malo, Aurelio/D-3973-2011; Martinez-Pastor, Felipe/B-4277-2008 OI Malo, Aurelio/0000-0002-0846-2096; Martinez-Pastor, Felipe/0000-0003-2987-4302 FU IMLS [IC-03-02-0186-02]; Spanish Ministry of Education and Science [FU2005-0893]; European Union [PIEF-GA-2008-220322]; Spanish Ministry of Science and Innovation; University of Castilla-La Mancha FX Supported by the IMLS Conservation Project Support Grant IC-03-02-0186-02. A.F.M. was a recipient of an MEC/Fulbright fellowship from the Spanish Ministry of Education and Science (FU2005-0893) and a Marie Curie fellowship from the European Union (PIEF-GA-2008-220322). F.M.-P. was supported by the Juan de la Cierva and Ramon y Cajal programs from the Spanish Ministry of Science and Innovation and by a travel grant from the University of Castilla-La Mancha. NR 76 TC 11 Z9 11 U1 2 U2 31 PU SOC STUDY REPRODUCTION PI MADISON PA 1691 MONROE ST,SUITE # 3, MADISON, WI 53711-2021 USA SN 0006-3363 EI 1529-7268 J9 BIOL REPROD JI Biol. Reprod. PD OCT PY 2010 VL 83 IS 4 BP 540 EP 548 DI 10.1095/biolreprod.110.085316 PG 9 WC Reproductive Biology SC Reproductive Biology GA 654JI UT WOS:000282163900006 PM 20519695 ER PT J AU Pelican, KM Spindler, RE Pukazhenthi, BS Wildt, DE Ottinger, MA Howard, J AF Pelican, Katharine M. Spindler, Rebecca E. Pukazhenthi, Budhan S. Wildt, David E. Ottinger, Mary A. Howard, JoGayle TI Progestin Exposure Before Gonadotropin Stimulation Improves Embryo Development after In Vitro Fertilization in the Domestic Cat SO BIOLOGY OF REPRODUCTION LA English DT Article DE embryo; gonadotropin-releasing hormone; oocyte metabolism; ovary; progesterone ID SUBSEQUENT LUTEAL FUNCTION; TIGER PANTHERA-TIGRIS; INVITRO FERTILIZATION; ARTIFICIAL-INSEMINATION; CHORIONIC-GONADOTROPIN; FOLLICLE DEVELOPMENT; OVARIAN ACTIVITY; LUTEINIZING-HORMONE; SEXUAL-BEHAVIOR; GNRH ANTAGONIST AB This study investigated the influence of progestin priming and ovarian quiescence on response to exogenous gonadotropin stimulation in the cat. Because a subpopulation of cats routinely ovulated spontaneously, there also was the opportunity to examine the ovary's reaction to the added impact of endogenously secreted progestagen. Queens were given 1) equine chorionic gonadotropin (eCG) plus human chorionic gonadotropin (hCG) only (control; n = 9 cats), 2) GnRH antagonist (antide) injections followed by eCG and hCG (n = 9), and 3) a progestin implant (levonorgestrel) followed by eCG and hCG (n = 9). Laparoscopy was used to assess ovarian activity and aspirate follicular oocytes that were graded on the basis of morphology. In five cats per treatment, half of the high-quality oocytes were assessed for glucose, pyruvate, and lactate metabolism as well as nuclear maturation. Remaining oocytes were inseminated in vitro, cultured, and examined at 72 h after insemination for cleavage. In the remaining four cats per treatment, all oocytes were inseminated in vitro and assessed at 72, 120, and 168 h after insemination for embryo developmental stage. Cats pretreated with progestin had more follicles and produced more embryos per donor (including at the combined morula/blastocyst stage) than controls or females treated with GnRH antagonist (P < 0.05). There were no differences among groups (P > 0.05) in oocyte carbohydrate metabolism, nuclear maturation metrics, or fertilization success, although there was a tendency toward improvements in all three (P < 0.2) in progestin-treated females. Interestingly, cats that spontaneously ovulated within 60 days of treatment onset also produced more embryos per cat than induced-ovulation counterparts (P < 0.05). Results indicate that prior exposure to exogenous progestin (via implant) or endogenous progestagen (via spontaneous ovulation) improves ovarian responsiveness to gonadotropins in the cat through a mechanism that is independent of the induction of ovarian quiescence. C1 [Pelican, Katharine M.; Spindler, Rebecca E.; Pukazhenthi, Budhan S.; Wildt, David E.; Howard, JoGayle] Natl Zool Pk, Smithsonian Conservat Biol Inst, Ctr Species Survival, Front Royal, VA USA. [Pelican, Katharine M.; Ottinger, Mary A.] Univ Maryland, Dept Anim & Avian Sci, College Pk, MD 20742 USA. RP Pelican, KM (reprint author), Univ Minnesota, Dept Vet Populat Med, 385F Anim Sci Vet Med Bldg,1365 Gortner Ave, St Paul, MN 55108 USA. EM pelicank@umn.edu FU Smithsonian Institution; National Institutes of Health [K01-RR017310-05, KO1-RR00135]; Friends of the National Zoo; University of Maryland FX Supported by the Smithsonian Institution's Scholarly Studies Program, the National Institutes of Health (K01-RR017310-05), Friends of the National Zoo, and a Graduate Fellowship awarded to K.M.P. by the University of Maryland. B.S.P. was supported by funds from the National Institutes of Health (KO1-RR00135). Research conducted in partial fulfillment of requirements for the Ph.D. for K.M.P. at the University of Maryland. NR 70 TC 9 Z9 9 U1 0 U2 5 PU SOC STUDY REPRODUCTION PI MADISON PA 1691 MONROE ST,SUITE # 3, MADISON, WI 53711-2021 USA SN 0006-3363 EI 1529-7268 J9 BIOL REPROD JI Biol. Reprod. PD OCT PY 2010 VL 83 IS 4 BP 558 EP 567 DI 10.1095/biolreprod.109.083360 PG 10 WC Reproductive Biology SC Reproductive Biology GA 654JI UT WOS:000282163900008 PM 20463355 ER PT J AU Fontoura, T Cazetta, E do Nascimento, W Catenacci, L De Vleeschouwer, K Raboy, B AF Fontoura, Talita Cazetta, Eliana do Nascimento, Wander Catenacci, Lilian De Vleeschouwer, Kristel Raboy, Becky TI Diurnal frugivores on the Bromeliaceae Aechmea depressa LB Sm. from Northeastern Brazil: the prominent role taken by a small forest primate SO BIOTA NEOTROPICA LA English DT Article DE Atlantic Rainforest; epiphyte; golden-headed-lion tamarin; Leontopithecus chlysomelas AB Little is lcnown about frugivory of epiphytes. We investigated diurnal frugivores consuming Aechmea depressa, an endemic species from Southern Bahia, Brazil, through 67 hours of observation on three fruiting individuals. Infructescences were visited for 2% of the time and only by golden-headed lion tamarins (GHLTs; Leontopithecus chrysomelas). Aechmea depressa invests on physical defense to retain fruits for prolonged periods, however, GIALTs used their small size and dexterity to remove rigid bracts and extract fruits from the infructescence. Prior studies indicate GHLTs disperseAechmea seeds. Given the low visitation rates and probability that few frugivores successfully manipulate A. depressa fruits, we suggest that GHLTs are extremely important to maintaining the populations of this bromeliad species. C1 [Fontoura, Talita; Cazetta, Eliana; do Nascimento, Wander] Univ Estadual Santa Cruz UESC, Dept Ciencias Biol, BR-45650000 Ilheus, BA, Brazil. [Catenacci, Lilian] Univ Estadual Santa Cruz UESC, Dept Ciencias Biol, Programa Posgrad Zool, BR-45650000 Ilheus, BA, Brazil. [Catenacci, Lilian; De Vleeschouwer, Kristel; Raboy, Becky] Inst Estudos Socio Ambientais Sul Bahia, BR-45653145 Ilheus, BA, Brazil. [De Vleeschouwer, Kristel] Royal Zool Soc Antwerp, Ctr Res & Conservat, B-2018 Antwerp, Belgium. [Raboy, Becky] Smithsonian Conservat Biol Inst, Washington, DC 20008 USA. RP Fontoura, T (reprint author), Univ Estadual Santa Cruz UESC, Dept Ciencias Biol, Rod Ilheus Itabuna,Km 16, BR-45650000 Ilheus, BA, Brazil. EM talita_fontoura@uol.com.br RI Cazetta, Eliana/F-3296-2010 OI Cazetta, Eliana/0000-0002-2209-2554 FU Universidade Estadual de Santa Cruz (UESC) FX The Universidade Estadual de Santa Cruz (UESC) provided funding for this project with additional infrastructure support from Projeto Mico Ledo-da-Cara-Dourada. Talita Fontoura, Wander do Nascimento and Becky Raboy had permission to conduct field work under the IBAMA licenses N 178/2006, 12714-1 and with additional approval from the owners of Fazenda Cabana da Serra/Incon. We are grateful to field assistants Gilvan Gomes Mota and Romano dos Santos Souza for helping us locate the focal clusters of A. depressa under observation in this study. NR 32 TC 4 Z9 4 U1 1 U2 3 PU REVISTA BIOTA NEOTROPICA PI CAMPINAS PA AV. DR. ROMEU TORTIMA, 388 - BARAO GERALDO, CEP 13084-520, CAMPINAS, SP, BRAZIL SN 1676-0603 J9 BIOTA NEOTROP JI Biota Neotrop. PD OCT-DEC PY 2010 VL 10 IS 4 SI SI BP 351 EP 354 PG 4 WC Biodiversity Conservation SC Biodiversity & Conservation GA V28BD UT WOS:000208655400042 ER PT J AU Frick, MG Zardus, JD Lazo-Wasem, EA AF Frick, Michael G. Zardus, John D. Lazo-Wasem, Eric A. TI A New Coronuloid Barnacle Subfamily, Genus and Species from Cheloniid Sea Turtles SO BULLETIN OF THE PEABODY MUSEUM OF NATURAL HISTORY LA English DT Article DE Caretta caretta; Chelonia mydas; sea turtles; epibiont; barnacle; new genus and species; Coronuloidea ID EPIBIONTS AB During a survey of the commensal barnacles of nesting and foraging sea turtles from the coastal waters of Florida and Georgia, USA, an undescribed species of platylepadid coronuloid barnacle was encountered, embedded within the carapace and plastron regions of host turtles. This new genus and species is described herein as Calyptolepas bjorndalae gen. et sp. nov. and is compared with other members of the family Platylepadidae. While similar in some respects to members of currently recognized platylepadid subfamilies, particularly Cylindrolepas darwiniana Pilsbry (Cylindrolepadinae Ross and Frick) and Platylepas decorata Darwin (Platylepadidae Newman and Ross), this new species bears an amalgamation of characters from these two subfamilies that require it to be placed into a new subfamily, Calyptolepadinae subfam. nov., also described herein. C1 [Frick, Michael G.] Smithsonian Natl Zool Pk, Friends Natl Zoo, Washington, DC 20013 USA. [Zardus, John D.] The Citadel, Dept Biol, Charleston, SC 29404 USA. [Lazo-Wasem, Eric A.] Yale Univ, Peabody Museum Nat Hist, Div Invertebrate Zool, New Haven, CT 06520 USA. RP Frick, MG (reprint author), Smithsonian Natl Zool Pk, Friends Natl Zoo, POB 37012,MRC-5516, Washington, DC 20013 USA. EM caretta05@aol.com; zardusjl@citadel.edu; eric.lazo-wasem@yale.edu NR 22 TC 8 Z9 8 U1 2 U2 4 PU PEABODY MUSEUM NATURAL HISTORY-YALE UNIV PI NEW HAVEN PA 170 WHITNEY AVE, PO BOX 208118, NEW HAVEN, CT 06520-8118 USA SN 0079-032X EI 2162-4135 J9 B PEABODY MUS NAT HI JI Bull. Peabody Mus. Natl. Hist. PD OCT PY 2010 VL 51 IS 2 BP 169 EP 177 DI 10.3374/014.051.0203 PG 9 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 673CQ UT WOS:000283636600003 ER PT J AU Cole, DG AF Cole, Daniel G. TI Archaeology and Landscape in the Mongolian Altai: An Atlas SO CARTOGRAPHY AND GEOGRAPHIC INFORMATION SCIENCE LA English DT Book Review C1 [Cole, Daniel G.] Smithsonian Inst, Washington, DC 20560 USA. RP Cole, DG (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 6 PU CARTOGRAPHY & GEOGRAPHIC INFOR SOC PI GAITHERSBURG PA 6 MONTGOMERY VILLAGE AVE, STE 403, GAITHERSBURG, MD 20879 USA SN 1523-0406 J9 CARTOGR GEOGR INF SC JI Cartogr. Geogr. Inf. Sci. PD OCT PY 2010 VL 37 IS 4 BP 319 EP 320 DI 10.1559/152304010793454345 PG 2 WC Geography SC Geography GA 686CW UT WOS:000284675400005 ER PT J AU Edgar, RG Clark, MA Dale, K Mitchell, DA Ord, SM Wayth, RB Pfister, H Greenhill, LJ AF Edgar, R. G. Clark, M. A. Dale, K. Mitchell, D. A. Ord, S. M. Wayth, R. B. Pfister, H. Greenhill, L. J. TI Enabling a high throughput real time data pipeline for a large radio telescope array with GPUs SO COMPUTER PHYSICS COMMUNICATIONS LA English DT Article DE Radio telescopes and instrumentation; Heterodyne receivers; Mathematical procedures and computer techniques; Computer science and technology ID MURCHISON WIDEFIELD ARRAY AB The Murchison Widefield Array (MWA) is a next-generation radio telescope currently under construction in the remote Western Australia Outback. Raw data will be generated continuously at 5 GiBs(-1), grouped into 8 s cadences. This high throughput motivates the development of on-site, real time processing and reduction in preference to archiving, transport and off-line processing. Each batch of 8 s data must be completely reduced before the next batch arrives. Maintaining real time operation will require a sustained performance of around 2.5 TFLOPs(-1) (including convolutions, FFTs, interpolations and matrix multiplications). We describe a scalable heterogeneous computing pipeline implementation, exploiting both the high computing density and FLOP-per-Watt ratio of modern GPUs. The architecture is highly parallel within and across nodes, with all major processing elements performed by GPUs. Necessary scatter-gather operations along the pipeline are loosely synchronized between the nodes hosting the GPUs. The MWA will be a frontier scientific instrument and a pathfinder for planned peta- and exa-scale facilities. (c) 2010 Elsevier B.V. All rights reserved. C1 [Edgar, R. G.; Clark, M. A.] Initiat Innovat Comp, Cambridge, MA 02138 USA. [Clark, M. A.; Mitchell, D. A.; Ord, S. M.; Wayth, R. B.; Greenhill, L. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Dale, K.; Pfister, H.] Sch Engn & Appl Sci, Cambridge, MA 02138 USA. RP Edgar, RG (reprint author), Initiat Innovat Comp, 29 Oxford St, Cambridge, MA 02138 USA. EM rge21@seas.harvard.edu; mikec@seas.harvard.edu; dale@eecs.harvard.edu; dmitchell@cfa.harvard.edu; sord@cfa.harvard.edu; rwayth@cfa.harvard.edu; pfister@seas.harvard.edu; greenhill@cfa.harvard.edu RI Wayth, Randall/B-2444-2013; Ord, Stephen/C-6138-2013 OI Wayth, Randall/0000-0002-6995-4131; FU Smithsonian Astrophysical Observatory; National Science Foundation [AST-0457585, PHY-0835713]; NVIDIA via the Harvard CUDA Center of Excellence FX We would like to thank NVIDIA for support via the Harvard CUDA Center of Excellence. Funding support was provided in part by the Smithsonian Astrophysical Observatory. This work was supported in part by the National Science Foundation through grants AST-0457585 and PHY-0835713. NR 27 TC 3 Z9 3 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0010-4655 J9 COMPUT PHYS COMMUN JI Comput. Phys. Commun. PD OCT PY 2010 VL 181 IS 10 BP 1707 EP 1714 DI 10.1016/j.cpc.2010.06.019 PG 8 WC Computer Science, Interdisciplinary Applications; Physics, Mathematical SC Computer Science; Physics GA 651RU UT WOS:000281945600007 ER PT J AU Gaillou, E Post, JE Bassim, ND Zaitsev, AM Rose, T Fries, MD Stroud, RM Steele, A Butler, JE AF Gaillou, E. Post, J. E. Bassim, N. D. Zaitsev, A. M. Rose, T. Fries, M. D. Stroud, R. M. Steele, A. Butler, J. E. TI Spectroscopic and microscopic characterizations of color lamellae in natural pink diamonds SO DIAMOND AND RELATED MATERIALS LA English DT Article DE Natural pink diamond; Graining; Deformation twin; Plastic deformation; 405.5 nm center ID PLASTIC-DEFORMATION; RAMAN-SPECTROSCOPY; OPTICAL-CENTERS; CVD DIAMOND; CRYSTALS; GROWTH; PHOTOLUMINESCENCE; TEMPERATURE; PRESSURE; STRESS AB Nineteen natural, untreated, type laAB pink diamonds from various localities were studied. They display microscopic (similar to 1 mu m thick) pink lamellae along {111} in an otherwise colorless diamond. This coloration concentrated in lamellae is commonly referred to as "graining". The diamonds were examined using high spatial resolution spectroscopic methods and transmission electron microscopy. TEM revealed that a pink lamella consists of a cluster of paired microtwins created under stress by plastic deformation. Raman line shift and broadening associated with the twinned pink lamellae indicate the presence of residual stress. Ultraviolet-visible absorption spectra from each of the samples showed a broad absorption band centered at similar to 550 nm, the source of the pink color. Cathodoluminescence spectra of the pink lamellae are different from those of the bulk, colorless diamond matrix. Within the lamellae only, the H3 center is observed along with a less intense N3 center. In some samples, instead of the N3 center a new center with a zero phonon line at 405.5 nm is observed. This previously unreported 405.5 nm center has phonon sidebands qualitatively identical to the N3 center, and may be an N3 center modified by a specific environment. These results suggest that lattice vacancies were created during twinning resulting from plastic deformation, and that impurity centers (such as those containing nitrogen) trap some of the diffusing vacancies. Since the pink lamellae are still under residual stress, new or modified defect centers are created, e.g. H3 and N3. The color center(s) responsible for the pink color (550 nm absorption) was not identified, but likely is only present in diamonds that experienced plastic deformation. Reported annealing of plastically deformed brown diamonds, which results in a residual pink color, suggests that the pink color is stable under these high pressure, high temperature conditions. The reported observations that annealing plastically deformed brown diamonds results in a residual pink color and that the pink color does not anneal out under similar high pressure, high temperature conditions, suggests that the deformation inducing pink color occurs inside the Earth's mantle, whereas brown coloration might be induced during a more recent event such as the ascent of the diamond to the surface in a kimberlitic/lamproitic eruption. Published by Elsevier BM. C1 [Gaillou, E.; Post, J. E.; Rose, T.] Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. [Gaillou, E.; Bassim, N. D.; Stroud, R. M.; Butler, J. E.] USN, Res Lab, Washington, DC 20375 USA. [Zaitsev, A. M.] CUNY Coll Staten Isl, Staten Isl, NY 10314 USA. [Fries, M. D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Steele, A.] Carnegie Inst Washington, Geophys Lab, Washington, DC 20015 USA. RP Gaillou, E (reprint author), Smithsonian Inst, Natl Museum Nat Hist, MRC 0119,Natl Hist Bldg W,Loading Dock 10th & Con, Washington, DC 20560 USA. EM gailloue@si.edu RI Butler, James/B-7965-2008; Gaillou, Eloise/D-1753-2009; Stroud, Rhonda/C-5503-2008 OI Butler, James/0000-0002-4794-7176; Gaillou, Eloise/0000-0002-7949-268X; Stroud, Rhonda/0000-0001-5242-8015 FU Apollo Diamond; JCK Industry Fund; Coralyn Whitney Endowment Fund (Smithsonian Institution) FX The authors wish to thank Alan Collins for constructive discussion of the some spectroscopic results, as well as Fischione and Yoosuff Piccard for assistance with the Nanomilling of the FIB sections. We gratefully acknowledge grants from Apollo Diamond, the JCK Industry Fund, and the Coralyn Whitney Endowment Fund (Smithsonian Institution). We also thank Dr. Benjamin Rondeau and the anonymous person who reviewed this paper, and who improved the quality of this manuscript. NR 60 TC 25 Z9 25 U1 2 U2 20 PU ELSEVIER SCIENCE SA PI LAUSANNE PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND SN 0925-9635 J9 DIAM RELAT MATER JI Diam. Relat. Mat. PD OCT PY 2010 VL 19 IS 10 BP 1207 EP 1220 DI 10.1016/j.diamond.2010.06.015 PG 14 WC Materials Science, Multidisciplinary SC Materials Science GA 654XB UT WOS:000282203300014 ER PT J AU Kaspari, M Chang, C Weaver, J AF Kaspari, Michael Chang, Charlotte Weaver, Johanna TI Salted roads and sodium limitation in a northern forest ant community SO ECOLOGICAL ENTOMOLOGY LA English DT Article DE Biogeochemistry; foraging; pollution; landscape; nutrition; soil ID SIZE-GRAIN HYPOTHESIS; BODY-SIZE; FRESH-WATER; FOOD; TEMPERATURE; POPULATION AB 1. Road salt is a common, anthropogenic source of NaCl in many temperate ecosystems. Sodium is also an essential and potentially limiting element for inland animal populations. This suggests that Na limitation in inland ecosystems, and hence attraction to Na sources, should increase with distance from salted roads. 2. In a North Temperate forest, we tested the prediction that Na recruitment would increase, as soil [Na] decreased, with distance from a salted two-lane highway. We presented ants with three concentrations of NaCl and sucrose solution along four pairs of transects ca 1, 10, 100, and 1000 m from the road. 3. Consistent with the Na-limitation hypothesis, the ratio of NaCl to sucrose use increased with distance from the road from 1:13 vials at 1 m to 1:5 vials at 1 km. Genera characterised by high Na use did not accumulate farther from the road. For the common and widespread Tapinoma sessile (Say), a 10-fold increase in distance from the road resulted in ants doubling their use of NaCl relative to sucrose. 4. Road salt is a well-known pollutant, especially of freshwater ecosystems. However, by suppressing plants and potentially promoting consumers, road salt may have more complex effects on terrestrial ecosystems, especially those far inland from oceanic aerosols. C1 [Kaspari, Michael] Univ Oklahoma, Dept Zool, Norman, OK 73019 USA. [Kaspari, Michael] Smithsonian Trop Res Inst, Balboa, Panama. [Chang, Charlotte] Pomona Coll, Dept Biol, Claremont, CA 91711 USA. [Weaver, Johanna] Oberlin Coll, OCMR, Oberlin, OH 44074 USA. RP Kaspari, M (reprint author), Univ Oklahoma, Dept Zool, Norman, OK 73019 USA. EM mkaspari@ou.edu OI Kaspari, Michael/0000-0002-9717-5768 FU NSF; Bullard Fellowship FX An NSF Research Experience for Undergraduates grant (to Harvard Forest), and a Bullard Fellowship (to MK) funded this research. A. Ellison and A. Smith were instrumental in providing logistical support; S. Cover was a continual source of insight into the New England ant community. NR 34 TC 13 Z9 13 U1 9 U2 40 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0307-6946 J9 ECOL ENTOMOL JI Ecol. Entomol. PD OCT PY 2010 VL 35 IS 5 BP 543 EP 548 DI 10.1111/j.1365-2311.2010.01209.x PG 6 WC Entomology SC Entomology GA 647TJ UT WOS:000281641900001 ER PT J AU Smith, JAM Reitsma, LR Marra, PP AF Smith, Joseph A. M. Reitsma, Leonard R. Marra, Peter P. TI Moisture as a determinant of habitat quality for a nonbreeding Neotropical migratory songbird SO ECOLOGY LA English DT Article DE body condition; body mass; habitat quality; migratory birds; nonbreeding winter habitat; Northern Waterthrush; Roosevelt Roads Naval Station, Puerto Rico; Seiurus noveboracensis ID WINTER SITE FIDELITY; NON-BREEDING SEASON; VENEZUELAN MANGROVES; NEARCTIC MIGRANTS; SAMPLING BLOOD; BODY CONDITION; STABLE-CARBON; TASSELED CAP; DRY SEASON; BIRDS AB Identifying the determinants of habitat quality for a species is essential for understanding how populations are limited and regulated. Spatiotemporal variation in moisture and its influence on food availability may drive patterns of habitat occupancy and demographic outcomes. Nonbreeding migratory birds in the neotropics occupy a range of habitat types that vary with respect to moisture. Using carbon isotopes and a satellite-derived measure of habitat moisture, we identified a moisture gradient across home ranges of radio-tracked Northern Waterthrush (Seiurus noveboracensis). We used this gradient to classify habitat types and to examine whether habitat moisture correlates with overwinter mass change and spring departure schedules of Northern Waterthrush over the late-winter dry season in the tropics. The two independent indicators of moisture revealed similar gradients that were directly proportional to body mass change as the dry season progressed. Birds occupying drier habitats declined in body mass over the study period, while those occupying wetter habitats increased in body mass. Regardless of habitat, birds lost an average of 7.6% of their mass at night, and mass recovery during the day trended lower in dry compared with wet habitats. This suggests that daily incremental shortfalls in mass recovery can lead to considerable season-long declines in body mass. These patterns resulted in consequences for the premigratory period, with birds occupying drier habitats having a delayed rate of fat deposition compared with those in wet habitats. Taken together with the finding that males, which are significantly larger than females, are also in better condition than females regardless of habitat suggests that high-quality habitats may be limited and that there may be competition for them. The habitat-linked variation in performance we observed suggests that habitat limitation could impact individual and population-level processes both during and in subsequent periods of the annual cycle. The linkage between moisture and habitat quality for a migratory bird indicates that the availability of high-quality habitats is dynamic due to variation in precipitation among seasons and years. Understanding this link is critical for ascertaining the impact of future climate change, particularly in the Caribbean basin, where a much drier future is predicted. C1 [Smith, Joseph A. M.; Marra, Peter P.] Smithsonian Migratory Bird Ctr, Natl Zool Pk, Washington, DC 20008 USA. [Reitsma, Leonard R.] Plymouth State Univ, Dept Biol Sci, Plymouth, NH 03264 USA. RP Smith, JAM (reprint author), Nature Conservancy, Delaware Bayshores Off, 2350 Route 47, Delmont, NJ 08314 USA. EM Joseph_Smith@tnc.org FU DoD FX This research was supported by a grant from the DoD Legacy Resources Management Program. We thank Daniel Brown, Ram Papish, Ryan Peters, Mark Pollock, T. J. Robinson, Jared Woodcock, Alicia Byrd, Sara Campbell, Bill Deluca, Brian Gibbons, and Karin Roux for their excellent and dedicated work in the field. We thank Winston Martinez and Oscar Diaz for facilitating our work at Roosevelt Roads Naval Station and the U. S. Forest Service Sabana Field Station and its staff for providing lodging and laboratory space. Thanks to William Gould and Gary Potts for help with acquiring imagery. Lee Weight at the Smithsonian Museum Support Center provided laboratory space and indispensable guidance during analysis of blood samples. We thank two anonymous reviewers for their thoughtful comments on the manuscript. Finally we thank Jean Lodge and Joe Wunderle for all of the assistance and hospitality they extended during our stay in Puerto Rico. NR 66 TC 35 Z9 35 U1 3 U2 32 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 0012-9658 J9 ECOLOGY JI Ecology PD OCT PY 2010 VL 91 IS 10 BP 2874 EP 2882 DI 10.1890/09-2212.1 PG 9 WC Ecology SC Environmental Sciences & Ecology GA 660PE UT WOS:000282654700007 PM 21058548 ER PT J AU Voigt, CC Sorgel, K Dechmann, DKN AF Voigt, Christian C. Soergel, Karin Dechmann, Dina K. N. TI Refueling while flying: Foraging bats combust food rapidly and directly to power flight SO ECOLOGY LA English DT Article DE Chiroptera; diet; energetics; flight metabolism; foraging; lesser bulldog bat; Neotropics; Noctilio albiventris; Smithsonian Tropical Research Institute, Gamboa, Panama; substrate ID STABLE CARBON ISOTOPES; NECTAR-FEEDING BATS; SUBSTRATE PATHWAYS; ENERGY-EXPENDITURE; HOVERING FLIGHT; EXHALED BREATH; MIXING MODELS; WIND-TUNNEL; BIRDS; FUEL AB Flying vertebrates, such as bats, face exceptionally high energy costs during active flapping flight. Once airborne, energy turnover may exceed basal metabolic rate by a factor of up to 15. Here, we asked whether fuel that powers flight originates from exogenous (dietary nutrients), endogenous sources (mostly body lipids or glycogen), or a combination of both. Since most insectivorous bats fly continuously over relatively long time periods during foraging, we assumed that slowly mobilized glycogen, although suitable for supporting brief sallying flights, is inadequate to power aerial insect-hunting of bats. We hypothesized that the insect-feeding Noctilio albiventris rapidly mobilizes and combusts nutrients from insects it has just eaten instead of utilizing endogenous lipids. We used the stable carbon isotope ratio in the bats' exhaled breath (delta(13)C(brth)) to assess the origin of metabolized substrates of resting and flying N. albiventris in two nutritional conditions: fasted and recently fed. The breath of fasted resting bats was depleted in (13)C in relation to their insect diet (delta(13)C(diet)), indicating the combustion of (13)C depleted body lipids. In contrast to this, delta(13)C(brth) of bats that had recently fed closely matched delta(13)C(diet) in both resting and flying bats, suggesting a quick mobilization of ingested nutrients for metabolism. In contrast to most non-volant mammals, bats have evolved the ability to fuel their high energy expenditure rates through the rapid combustion of exogenous nutrients, enabling them to conquer the nocturnal niche of aerial insectivory. C1 [Voigt, Christian C.; Soergel, Karin; Dechmann, Dina K. N.] Leibniz Inst Zoo & Wildlife Res, Evolutionary Ecol Res Grp, D-10315 Berlin, Germany. [Dechmann, Dina K. N.] Univ Konstanz, Dept Biol, D-78457 Constance, Germany. [Dechmann, Dina K. N.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Voigt, CC (reprint author), Leibniz Inst Zoo & Wildlife Res, Evolutionary Ecol Res Grp, Alfred Kowalke Str 17, D-10315 Berlin, Germany. EM voigt@izw-berlin.de FU Deutsche Forschungsgemeinschaft [Vo890/11] FX We thank Antje S. Kretzschmar, Silke L. Voitgt-Heucke, Megan Lupek, Shai Pilosoph, and Apanie Wood for help during fieldwork, and Egbert Leigh and two anonymous reviewers for comments on the manuscript. We acknowledge the generous support of the Smithsonian Tropical Research Institute (STRI) and the Panamanian authorities. The experiments were carried out under permits from the Autoridad National del Ambiente (ANAM) of Panama and STRI IUCAC protocols. This work was financed by a grant from the Deutsche Forschungsgemeinschaft to C. C. Voigt and D. K. N. Dechmann (Vo890/11). NR 56 TC 26 Z9 26 U1 4 U2 42 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 0012-9658 J9 ECOLOGY JI Ecology PD OCT PY 2010 VL 91 IS 10 BP 2908 EP 2917 DI 10.1890/09-2232.1 PG 10 WC Ecology SC Environmental Sciences & Ecology GA 660PE UT WOS:000282654700010 PM 21058551 ER PT J AU Reef, R Ball, MC Feller, IC Lovelock, CE AF Reef, Ruth Ball, Marilyn C. Feller, Ilka C. Lovelock, Catherine E. TI Relationships among RNA : DNA ratio, growth and elemental stoichiometry in mangrove trees SO FUNCTIONAL ECOLOGY LA English DT Article DE C : N : P; ecostoichiometry; growth rate hypothesis; nutrients; plant; shoot elongation ID C-N-P; BIOLOGICAL STOICHIOMETRY; CERIOPS-TAGAL; NUTRITIONAL CONDITION; NUTRIENT DYNAMICS; RNA/DNA RATIOS; LIFE-HISTORY; ATLANTIC COD; ACID; FOREST AB P>1. Growth rate is a fundamental property of organisms. In trees, growth is indeterminate and varies in space and time depending on resource availability, genetic constraints, competition and stress from biotic and abiotic environmental factors. 2. The ratio between the abundance of RNA and DNA in the tissue has been used to indicate recent growth rates in many systems, but not for trees. We assessed the applicability of using RNA : DNA ratios for assessing intraspecific and interspecific differences in growth rates in two species of mangrove trees under field conditions. We manipulated growth by fertilizing mangrove trees over a period of 4 years and measured tree growth as increments in linear extension of tagged shoots. The C, N and P contents per unit biomass were measured to test the hypothesis that faster growing organisms require more P per unit biomass (the Growth Rate Hypothesis). 3. We found that interspecific differences in the RNA : DNA ratio clearly reflected the difference in shoot elongation rates between the species. Intraspecific differences in RNA : DNA were significantly correlated with growth rates only for Avicennia marina and not for Ceriops australis. C : N and C : P ratios were lower in trees with higher growth rates and exhibited a negative correlation with RNA : DNA ratios. 4. Our results indicate that RNA : DNA ratios can reliably predict interspecific differences in growth rates between the two mangrove species and that RNA : DNA ratios can be used as an indication of variation in growth rate for Avicennia marina. The interaction between C : N : P ratios, RNA : DNA ratios and growth rates supported the Growth Rate Hypothesis on an interspecific level, but not on an intraspecific level. C1 [Reef, Ruth; Lovelock, Catherine E.] Univ Queensland, Ctr Marine Studies, St Lucia, Qld 4072, Australia. [Reef, Ruth; Lovelock, Catherine E.] Univ Queensland, Sch Biol Sci, St Lucia, Qld 4072, Australia. [Ball, Marilyn C.] Australian Natl Univ, Res Sch Biol, Div Plant Sci, Canberra, ACT 0200, Australia. [Feller, Ilka C.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Reef, R (reprint author), Univ Queensland, Ctr Marine Studies, St Lucia, Qld 4072, Australia. EM r.reef@uq.edu.au RI Ball, Marilyn/D-1180-2009; Lovelock, Catherine/G-7370-2012; OI Lovelock, Catherine/0000-0002-2219-6855; Feller, Ilka/0000-0002-6391-1608 FU Australian Research Council [DP0774491, DP0986170]; Smithsonian Marine Science Network FX We thank N. Stromsoe and A. Main for their help with sample analysis and V. Benion, A. Grinham, A. Chamberlain and B. Clegg for assistance with fieldwork. U. Motro helped with statistical analysis. We thank M. Motro and the anonymous reviewers for their useful comments on this manuscript. Australian Research Council Discovery Projects DP0774491 and DP0986170 and the Smithsonian Marine Science Network funded this work. NR 62 TC 20 Z9 25 U1 4 U2 27 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0269-8463 J9 FUNCT ECOL JI Funct. Ecol. PD OCT PY 2010 VL 24 IS 5 BP 1064 EP 1072 DI 10.1111/j.1365-2435.2010.01722.x PG 9 WC Ecology SC Environmental Sciences & Ecology GA 651AA UT WOS:000281895800014 ER PT J AU den Tex, RJ Maldonado, JE Thorington, R Leonard, JA AF den Tex, Robert-Jan Maldonado, Jesus E. Thorington, Richard Leonard, Jennifer A. TI Nuclear copies of mitochondrial genes: another problem for ancient DNA SO GENETICA LA English DT Article DE Numt; aDNA; Sundasciurus; Mitochondria; Universal primers ID PSEUDOGENES; GENOME; NUMTS; SYSTEMATICS; RODENTIA; HISTORY AB The application of ancient DNA techniques is subject to many problems caused primarily by low quality and by low quantity of DNA. For these reasons most studies employing ancient DNA rely on the characterization of mitochondrial DNA, which is present in many more copies per cell than nuclear DNA and hence more copies are likely to survive. We used universal and taxon specific mitochondrial primers to amplify DNA from museum specimens, and found many instances where the amplification of nuclear copies of the mitochondrial gene (numts) instead of the targeted mitochondrial fragment had occurred. Furthermore, the likelihood of amplifying numts increased dramatically when universal primers were utilized. Here we suggest that ancient DNA practitioners must consider the possibility that numts can be amplified at higher rates than previously thought. This is another complication for ancient DNA studies, but it also suggests that more extensive inclusion of nuclear markers in ancient DNA studies should be feasible. C1 [den Tex, Robert-Jan; Leonard, Jennifer A.] Uppsala Univ, Dept Evolutionary Biol, S-75236 Uppsala, Sweden. [Maldonado, Jesus E.; Thorington, Richard] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA. [Maldonado, Jesus E.; Leonard, Jennifer A.] Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, Washington, DC 20008 USA. [Leonard, Jennifer A.] CSIC, Estn Biol Donana, Seville 41092, Spain. RP Leonard, JA (reprint author), Uppsala Univ, Dept Evolutionary Biol, Norbyvagen 18D, S-75236 Uppsala, Sweden. EM JLeonard@ebd.csic.es RI CSIC, EBD Donana/C-4157-2011; Leonard, Jennifer/A-7894-2010 OI CSIC, EBD Donana/0000-0003-4318-6602; Leonard, Jennifer/0000-0003-0291-7819 FU Smithsonian Restricted Endowment Walcott Fund; Swedish Research Council FX Samples were kindly provided by the National Museum of Natural History 'Naturalis' (formerly Rijksmuseum van Natuurlijke Historie), Leiden, The Netherlands; the Natural History Museum, London; and the United States National Museum of Natural History, Smithsonian Institution. This project was funded by the Smithsonian Restricted Endowment Walcott Fund and the Swedish Research Council. Logistical support was provided by the Center for Conservation and Evolutionary Genetics, National Zoological Park, Smithsonian Institution, USA. NR 22 TC 20 Z9 22 U1 1 U2 12 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0016-6707 J9 GENETICA JI Genetica PD OCT PY 2010 VL 138 IS 9-10 BP 979 EP 984 DI 10.1007/s10709-010-9481-9 PG 6 WC Genetics & Heredity SC Genetics & Heredity GA 657SG UT WOS:000282432000007 PM 20700629 ER PT J AU Goto, K Fukuda, K Senda, A Saito, T Kimura, K Glander, KE Hinde, K Dittus, W Milligan, LA Power, ML Oftedal, OT Urashima, T AF Goto, Kohta Fukuda, Kenji Senda, Akitsugu Saito, Tadao Kimura, Kazumasa Glander, Kenneth E. Hinde, Katie Dittus, Wolfgang Milligan, Lauren A. Power, Michael L. Oftedal, Olav T. Urashima, Tadasu TI Chemical characterization of oligosaccharides in the milk of six species of New and Old world monkeys SO GLYCOCONJUGATE JOURNAL LA English DT Article DE Old world monkey; New world monkey; Milk oligosaccharide; Rhesus macaque; Toque macaque; Baboon; Capuchin; Mantled howler; Squirrel monkey; N-glycolylneuraminic acid ID BIFIDOBACTERIUM-BIFIDUM; MASS-SPECTROMETRY; DIVERGENCE TIMES; COLOSTRUM; CHROMATOGRAPHY; COMBINATION; CHIMPANZEE; PRIMATES; GORILLA AB Human and great ape milks contain a diverse array of milk oligosaccharides, but little is known about the milk oligosaccharides of other primates, and how they differ among taxa. Neutral and acidic oligosaccharides were isolated from the milk of three species of Old World or catarrhine monkeys (Cercopithecidae: rhesus macaque (Macaca mulatta), toque macaque (Macaca sinica) and Hamadryas baboon (Papio hamadryas)) and three of New World or platyrrhine monkeys (Cebidae: tufted capuchin (Cebus apella) and Bolivian squirrel monkey (Saimiri boliviensis); Atelidae: mantled howler (Alouatta palliata)). The milks of these species contained 6-8% total sugar, most of which was lactose: the estimated ratio of oligosaccharides to lactose in Old World monkeys (1:4 to 1:6) was greater than in New World monkeys (1:12 to 1:23). The chemical structures of the oligosaccharides were determined mainly by H-1-NMR spectroscopy. Oligosaccharides containing the type II unit (Gal(beta 1-4)GlcNAc) were found in the milk of the rhesus macaque, toque macaque, Hamadryas baboon and tufted capuchin, but oligosaccharides containing the type I unit (Gal(beta 1-3)GlcNAc), which have been found in human and many great ape milks, were absent from the milk of all species studied. Oligosaccharides containing Lewis x (Gal(beta 1-4)[Fuc(alpha 1-3)]GlcNAc) and 3-fucosyl lactose (3-FL, Gal(beta 1-4)[Fuc(alpha 1-3)]Glc) were found in the milk of the three cercopithecid monkey species, while 2-fucosyl lactose (5'-FL, Fuc(alpha 1-2)Gal(beta 1-4)Glc) was absent from all species studied. All of these milks contained acidic oligosaccharides that had N-acetylneuraminic acid as part of their structures, but did not contain oligosaccharides that had N-glycolylneuraminic acid, in contrast to the milk or colostrum of great apes which contain both types of acidic oligosaccharides. Two GalNAc-containing oligosaccharides, lactose 3'-O-sulfate and lacto-N-novopentaose I (Gal(beta 1-3)[Gal(beta 1-4)GlcNAc(beta 1-6)]Gal(beta 1-4)Glc) were found only in the milk of rhesus macaque, hamadryas baboon and tufted capuchin, respectively. Further research is needed to determine the extent to which the milk oligosaccharide patterns observed among these taxa represent wider phylogenetic trends among primates and how much variation occurs among individuals or species. C1 [Goto, Kohta; Fukuda, Kenji; Senda, Akitsugu; Urashima, Tadasu] Obihiro Univ Agr & Vet Med, Grad Sch Food Hyg, Obihiro, Hokkaido 0808555, Japan. [Saito, Tadao] Tohoku Univ, Grad Sch Agr, Sendai, Miyagi 980, Japan. [Kimura, Kazumasa] Yakult Cent Inst, Kunitachi, Tokyo, Japan. [Glander, Kenneth E.] Duke Univ, Dept Evolutionary Anthropol, Durham, NC USA. [Hinde, Katie] Univ Calif Davis, Calif Natl Primate Res Ctr, Brain Mind & Behav Unit, Davis, CA 95616 USA. [Dittus, Wolfgang] Inst Fundamental Studies, Smithsonian Primate Biol Program, Kandy, Sri Lanka. [Milligan, Lauren A.] Univ Calif Santa Cruz, Dept Anthropol, Santa Cruz, CA 95064 USA. [Dittus, Wolfgang; Power, Michael L.] Smithsonian Conservat Biol Inst, Natl Zool Pk, Nutr Lab, Washington, DC USA. [Oftedal, Olav T.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Urashima, T (reprint author), Obihiro Univ Agr & Vet Med, Grad Sch Food Hyg, Obihiro, Hokkaido 0808555, Japan. EM urashima@obihiro.ac.jp OI Power, Michael/0000-0002-6120-3528; Hinde, Katie/0000-0002-0528-866X FU National Institutes of Health [RR019970, RR000169]; US National Science Foundation [BNS-9510894]; Earthwatch Institute, Boston, MA; LSB Leakey Foundation [1965]; National Center for Research Resources (NCRR) [P40 RR01254]; National Institutes of Health (NIH) FX We thank Michael Jakubasz and Regina Eisert for assistance in selecting and preparing samples at the Nutrition Laboratory of the Smithsonian National Zoological Park. Collection of rhesus macaque milk was supported in part by National Institutes of Health grants RR019970 to John Capitanio and RR000169 to the California National Primate Research Center. Toque macaque field research was supported by grants to W. Dittus from the US National Science Foundation (BNS-9510894) and the Earthwatch Institute, Boston, MA, and Sunil Gunathilake assisted with the collection of milk samples. Collection of capuchin milk was supported by a grant to LA Milligan from the LSB Leakey Foundation 1965. Squirrel monkey research was made possible by Grant Number P40 RR01254 from the National Center for Research Resources (NCRR), a component of the National Institutes of Health (NIH). Mantled howler research was supported by a grant to K. Glander from the Earthwatch Institute, Boston, MA and Kay Izard assisted with collection of milks. The contents of this paper are solely the responsibility of the authors and do not necessarily reflect the official views of the funding agencies. Samples obtained from primate research institutes were collected under Animal Care and Use authorizations of these organizations and/or the universities of the coauthors. NR 50 TC 20 Z9 21 U1 1 U2 11 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0282-0080 J9 GLYCOCONJUGATE J JI Glycoconjugate J. PD OCT PY 2010 VL 27 IS 7-9 BP 703 EP 715 DI 10.1007/s10719-010-9315-0 PG 13 WC Biochemistry & Molecular Biology SC Biochemistry & Molecular Biology GA 695HO UT WOS:000285361400007 PM 21127965 ER PT J AU Ousley, SD Jones, EB AF Ousley, Stephen D. Jones, Erica B. TI Craniometric Variation in the Aleutians: Integrating Morphological, Molecular, Spatial, and Temporal Data SO HUMAN BIOLOGY LA English DT Article DE CEPHALIC INDEX; CRANIAL INDEX; ALEUT PREHISTORY; ALEUTIAN ISLANDS; CRANIOMETRIC VARIATION; TYPOLOGY ID REPLACEMENT; ESKIMOS AB Several hypotheses have been put forward about the origins and evolution of the inhabitants of the Aleutian Islands. Both Hrdlicka [The Aleutian and Commander Islands and Their Inhabitants ( Philadelphia: Wistar Institute of Anatomy and Biology, 1945)] and Laughlin ["The Alaska gateway viewed from the Aleutian Islands," in Papers on the Physical Anthropology of the American Indian, W. S. Laughlin, ed. ( New York: Viking Fund, 1951), 98-126] analyzed cranial morphology and came to somewhat different conclusions using a typological approach and limited analytical methods. Subsequent investigations using morphological data have not significantly improved our understanding of Aleut prehistory. More recently, radiocarbon dating and mitochondrial DNA analyses have shed light on Aleut genetic variation and changes over time, but better morphological methods using multivariate statistical analysis have not yet been used. We analyzed craniometric data using multivariate procedures and found that Aleuts demonstrate significant changes in cranial morphology over time, and these changes correspond to Hrdlicka's observations but may not necessarily reflect in-migration. The morphological changes were concentrated in the very aspects of morphology that are easily observable and that Hrdlicka most often measured, namely, cranial length, breadth, and height, but they were obscured when craniometric variation as a whole was analyzed. Also, we found that the morphological changes over time were not related to the changes in haplogroup frequencies over time, suggesting that migration into the Aleutians did not play a significant role in producing the morphological changes. However, craniometric variability apparently increases over time, suggesting in-migration, localized selection, and/or greater environmental heterogeneity. Our results contradict Laughlin's observations but may be more in line with his hypothesis of in situ evolutionary changes absent gene flow. In addition to selection, gene flow, and gene drift, however, sociocultural changes must also be considered as a factor in why morphology changed over time. C1 [Ousley, Stephen D.] Mercyhurst Coll, Dept Anthropol Archaeol, Erie, PA 16546 USA. [Jones, Erica B.] Smithsonian Inst, Dept Anthropol, Washington, DC 20560 USA. RP Ousley, SD (reprint author), Mercyhurst Coll, Dept Anthropol Archaeol, Erie, PA 16546 USA. NR 28 TC 4 Z9 4 U1 1 U2 8 PU WAYNE STATE UNIV PRESS PI DETROIT PA 4809 WOODWARD AVE, DETROIT, MI 48201-1309 USA SN 0018-7143 J9 HUM BIOL JI Hum. Biol. PD OCT-DEC PY 2010 VL 82 IS 5-6 SI SI BP 629 EP 651 PG 23 WC Anthropology; Biology; Genetics & Heredity SC Anthropology; Life Sciences & Biomedicine - Other Topics; Genetics & Heredity GA 734MW UT WOS:000288339200008 PM 21417887 ER PT J AU Ghent, RR Gupta, V Campbell, BA Ferguson, SA Brown, JCW Fergason, RL Carter, LM AF Ghent, Rebecca R. Gupta, V. Campbell, B. A. Ferguson, S. A. Brown, J. C. W. Fergason, R. L. Carter, L. M. TI Generation and emplacement of fine-grained ejecta in planetary impacts SO ICARUS LA English DT Article DE Moon; Mars; Venus; Cratering; Radar observations ID CRATER EJECTA; VENUS; MOON; MAGELLAN; DEPOSITS; BASIN AB We report here on a survey of distal fine-grained ejecta deposits on the Moon, Mars, and Venus. On all three planets, fine-grained ejecta form circular haloes that extend beyond the continuous ejects and other types of distal deposits such as run-out lobes or ramparts. Using Earth-based radar images, we find that lunar fine-grained ejecta haloes represent meters-thick deposits with abrupt margins, and are depleted in rocks >= 1 cm in diameter. Martian haloes show low nighttime thermal IR temperatures and thermal inertia, indicating the presence of fine particles estimated to range from similar to 10 mu m to 10 mm. Using the large sample sizes afforded by global datasets for Venus and Mars, and a complete nearside radar map for the Moon, we establish statistically robust scaling relationships between crater radius R and fine-grained ejects run-out r* for all three planets. On the Moon, r* similar to R(-0.18) for craters 5-640 km in diameter. For Venus, radar-dark haloes are larger than those on the Moon, but scale as r* similar to R(-0.49), consistent with ejecta entrainment in Venus' dense atmosphere. On Mars, fine-ejecta haloes are larger than lunar haloes for a given crater size, indicating entrainment of ejects by the atmosphere or vaporized subsurface volatiles, but scale as R(-0.13), similar to the ballistic lunar scaling. Ejecta suspension in vortices generated by passage of the ejecta curtain is predicted to result in ejecta run-out that scales with crater size as R(1/2), and the wind speeds so generated may be insufficient to transport particles at the larger end of the calculated range. The observed scaling and morphology of the low-temperature haloes leads us rather to favor winds generated by early-stage vapor plume expansion as the emplacement mechanism for low-temperature halo materials. (C) 2010 Elsevier Inc. All rights reserved. C1 [Ghent, Rebecca R.; Gupta, V.; Ferguson, S. A.; Brown, J. C. W.] Univ Toronto, Dept Geol, Toronto, ON M5S 3B1, Canada. [Campbell, B. A.; Carter, L. M.] Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. [Fergason, R. L.] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA. RP Ghent, RR (reprint author), Univ Toronto, Dept Geol, 22 Russell St, Toronto, ON M5S 3B1, Canada. EM ghentr@geology.utoronto.ca RI Carter, Lynn/D-2937-2012 FU Natural Sciences and Engineering Research Council of Canada; NASA; PGG FX We thank Nadine Barlow and Goro Komatsu for constructive reviews, which greatly improved the quality of this paper. Taronish Pithawala and John Koziar assisted with halo identification. This work was supported by a grant from the Natural Sciences and Engineering Research Council of Canada to R.R.G., and by the NASA Planetary Astronomy and PGG Programs. Arecibo Observatory is part of the National Astronomy and Ionosphere Center, operated by Cornell University under a cooperative agreement with the NSF. The Green Bank Telescope is part of the National Radio Astronomy Observatory, an NSF facility operated under cooperative agreement by Associated Universities, Inc. NR 37 TC 17 Z9 17 U1 1 U2 8 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD OCT PY 2010 VL 209 IS 2 BP 818 EP 835 DI 10.1016/j.icarus.2010.05.005 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 654VL UT WOS:000282199000047 ER PT J AU Judkins, HL Vecchione, M Roper, CFE Torres, J AF Judkins, Heather L. Vecchione, Michael Roper, Clyde F. E. Torres, Joseph TI Cephalopod species richness in the wider Caribbean region SO ICES JOURNAL OF MARINE SCIENCE LA English DT Article; Proceedings Paper CT Symposium of the Cephalopod-International-Advisory-Council CY SEP, 2009 CL Spanish Natl Res Council, Vigo, SPAIN SP Cephalopod Int Advisory Council HO Spanish Natl Res Council DE cephalopod distribution; species richness; wider Caribbean region ID LATITUDINAL DIVERSITY GRADIENTS; ATLANTIC-OCEAN; DEEP-SEA; MARINE MOLLUSKS; RAPOPORTS RULE; NORTH-ATLANTIC; PATTERNS; NEMATODES; RANGE; SIZE AB The cephalopods of the wider Caribbean region (western central Atlantic) were examined in terms of distribution and ecological importance. In all, 4190 preserved cephalopod specimens were identified and catalogued to produce regional maps of cephalopod distribution within the wider Caribbean. Regional species richness was examined with respect to Rapoport's rule (RR) and to determine possible cephalopod hotspots in the region. Rarefaction curves were used to normalize the samples of various size collected throughout the wider Caribbean. Cephalopods of the wider Caribbean within latitudinal bands from 8 to 308N do not support RR because they exhibit increasing species richness with increasing latitude. Eight subareas were chosen to compare species richness. Regionally, species richness appears to be patchy, with cephalopods concentrated more off the eastern Florida coast. There is a need for increased sampling throughout the wider Caribbean. Areas were lacking in samples, especially the central and southeastern parts of the region. There is a need to explore the systematics, life histories, and distribution patterns for this group of organisms in future. C1 [Judkins, Heather L.; Torres, Joseph] Univ S Florida, Coll Marine Sci, St Petersburg, FL 33701 USA. [Vecchione, Michael] Smithsonian Inst, Natl Museum Nat Hist, NMFS Natl Systemat Lab, Washington, DC 20013 USA. RP Judkins, HL (reprint author), Univ S Florida, Coll Marine Sci, St Petersburg, FL 33701 USA. EM judkins@mail.usf.edu NR 48 TC 0 Z9 0 U1 4 U2 15 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 1054-3139 J9 ICES J MAR SCI JI ICES J. Mar. Sci. PD OCT PY 2010 VL 67 IS 7 BP 1392 EP 1400 DI 10.1093/icesjms/fsq092 PG 9 WC Fisheries; Marine & Freshwater Biology; Oceanography SC Fisheries; Marine & Freshwater Biology; Oceanography GA 648UH UT WOS:000281719300010 ER PT J AU McDonald, KA Grunbaum, D AF McDonald, Kathryn A. Gruenbaum, Daniel TI Swimming Performance in Early Development and the "Other" Consequences of Egg Size for Ciliated Planktonic Larvae SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Article; Proceedings Paper CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY JAN 03-07, 2010 CL Seattle, WA SP Soc Integrat & Comparat Biol ID MARINE BENTHIC INVERTEBRATES; TO-ZYGOTIC TRANSITION; SEA-URCHIN EMBRYOS; CELL LINEAGE; REPRODUCTIVE STRATEGIES; CREPIDULA-FORNICATA; ECHINODERM LARVAE; NONFEEDING LARVAE; PATELLA-VULGATA; EVOLUTION AB The evolutionary significance of egg size in marine invertebrates is commonly perceived in energetic terms. Embryonic size should also have direct effects upon the forces that govern swimming, a behavior common to early larval development in the plankton. If swimming is ecologically important, early larvae may need to perform to a certain "standard", or threshold of speed and/or stability. The existence of performance standards in early development could therefore act to constrain the evolution of egg size and the evolution of development. Here we present the key parameters that characterize the upward swimming speed of ciliated spheroidal larvae moving at very low Reynolds numbers. The dependence of maximum supported mass upon larval size, and the independence of neutral-weight swimming speed from size, lead to hypotheses about scaling of swimming speed with size. Experimental studies with thirteen broadcast-spawning planktotrophs demonstrate that free-living embryonic swimmers in all of these species conform to a strong negative scaling of density with size that offsets increases in mass with increasing size. This trend suggests that swimming ability is broadly under selection in early development. In experimental studies and in a hydrodynamic model of larval swimming, the performance of trochophore larvae provides support for our hypothesized scaling relationships, and also for the concept of a standard in swimming speed. Echinoid blastulae, however, show relationships between speed and size that are not predicted by our scaling arguments. Results for echinoids suggest that differences in ciliary tip speed, or possibly in spatial density of cilia over the blastula's surface, result in significant differences in species' performance. Strong phyletic differences in the initial patterning and growth of structures used for swimming thus appear to cause significant differences in the relationship of swimming ability with embryo size. C1 [McDonald, Kathryn A.] Univ Washington, Friday Harbor Labs, Friday Harbor, WA 98250 USA. [McDonald, Kathryn A.] Smithsonian Trop Res Inst, DPO, AA 34002 USA. [Gruenbaum, Daniel] Univ Washington, Sch Oceanog, Seattle, WA 98195 USA. RP McDonald, KA (reprint author), Univ Washington, Friday Harbor Labs, Friday Harbor, WA 98250 USA. EM mcdonaldk2@si.edu FU National Science Foundation [OCE-0217304]; National Oceanic and Atmospheric Administration Washington [NA040AR170032]; Friday Harbor FX Friday Harbor-Achievement Rewards for College Scientists Fellowship (to K.A.M.); National Science Foundation support for K. A. M. came from grant (OCE-0217304 to R. R. S.); National Oceanic and Atmospheric Administration Washington Sea Grant (# NA040AR170032 to D.G.). NR 61 TC 10 Z9 10 U1 2 U2 14 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 EI 1557-7023 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD OCT PY 2010 VL 50 IS 4 BP 589 EP 605 DI 10.1093/icb/icq090 PG 17 WC Zoology SC Zoology GA 657TU UT WOS:000282437700010 PM 21558226 ER PT J AU Jud, NA Rothwell, GW Stockey, RA AF Jud, Nathan A. Rothwell, Gar W. Stockey, Ruth A. TI PALEOECOLOGICAL AND PHYLOGENETIC IMPLICATIONS OF SAXICAULIS MECKERTII GEN. ET SP. NOV.: A BENNETTITALEAN STEM FROM THE UPPER CRETACEOUS OF WESTERN NORTH AMERICA SO INTERNATIONAL JOURNAL OF PLANT SCIENCES LA English DT Article DE Bennettitales; borer; Cretaceous; oribatid mites; plant-animal interactions ID SEED-PLANT PHYLOGENY; CHIBA PREFECTURE; PETRIFIED PLANTS; ANGIOSPERMS; ORIGIN; TRUNK; CYCADEOIDEA; GNETALES; JAPAN; REEVALUATION AB A new anatomically preserved bennettitalean stem has been recovered from the Upper Cretaceous (Coniacian) Eden Main locality on Vancouver Island, British Columbia, Canada. The fossil, described as Saxicaulis meckertii gen. et sp. nov., is permineralized and consists of a eustelic stem with diverging non-girdling leaf traces, a narrow zone of dense wood, primary cortex, and adventitious roots. Important vegetative characters that differentiate bennettitalean stems from cycad stems are reviewed, and while the anatomy of the stem conforms to Bennettitales, it is not consistent with either the Williamsoniaceae or the Cycadeoidaceae as they are currently understood. This fossil documents greater structural diversity among Cretaceous bennettitaleans than previously known and tentatively documents an additional growth habit (underground stem). Co-occurring fossils and plant structure suggest this plant may have inhabited an environment prone to fires. Additionally, there is evidence for two forms of plant-animal interaction in the fossil. The first is a large gallery in the pith lined with wound reaction tissue and accessed through a 3-mm hole on the surface of the stem that represents a new type of herbivore damage for Bennettitales. Reaction tissue occurs in rings and plates throughout the plant body. Smaller galleries containing coprolites of oribatid mites and lacking wound reaction tissue are present in the cortex. The complexity of Upper Cretaceous bennettitalean plant-animal interactions through herbivory and detritivory is evaluated. C1 [Jud, Nathan A.] Smithsonian Inst, Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. [Jud, Nathan A.] Univ Maryland Coll Pk, Program Behav Ecol Evolut & Systemat, College Pk, MD 20742 USA. [Rothwell, Gar W.] Ohio Univ, Dept Environm & Plant Biol, Athens, OH 45701 USA. [Stockey, Ruth A.] Univ Alberta, Dept Biol Sci, Edmonton, AB T6G 2E9, Canada. RP Jud, NA (reprint author), Smithsonian Inst, Museum Nat Hist, Dept Paleobiol, POB 37012, Washington, DC 20560 USA. EM njud@umd.edu FU NSF [EF-0629819]; NSERC [A-6908] FX We are indebted to Dirk Meckert and Rick Ross on Vancouver Island and Steve Karafit, Hendrix College, for collecting assistance and to Steve Karafit for making the specimen available for detailed study. This work was supported in part by the NSF (grant EF-0629819 to G. W. Rothwell and R. A. Stockey) and the NSERC (grant A-6908 to R. A. Stockey). NR 85 TC 5 Z9 5 U1 2 U2 7 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 1058-5893 J9 INT J PLANT SCI JI Int. J. Plant Sci. PD OCT PY 2010 VL 171 IS 8 BP 915 EP 925 DI 10.1086/655963 PG 11 WC Plant Sciences SC Plant Sciences GA 650UA UT WOS:000281876900010 ER PT J AU Lambert, AM Dudley, TL Saltonstall, K AF Lambert, Adam M. Dudley, Tom L. Saltonstall, Kristin TI Ecology and Impacts of the Large-Statured Invasive Grasses Arundo donax and Phragmites australis in North America SO INVASIVE PLANT SCIENCE AND MANAGEMENT LA English DT Article DE Biological invasions; ruderal; life form; functional group; invasive species ID GIANT REED; COMMON REED; BIOLOGICAL-CONTROL; SOUTHERN CALIFORNIA; TETRAMESA-ROMANA; TIDAL MARSHES; ALIEN PLANTS; REPRODUCTION; ARUNDINOIDEAE; EXPANSION AB Large-statured invasive grasses (LSIGs) constitute a distinct functional group with characteristic life history traits that facilitate colonization and aggressive growth in aquatic ecosystems, particularly those modified by human activities. These species typically form monocultures in the systems they invade and have wide-ranging and negative impacts on biodiversity and ecosystem processes. In March 2008, a special symposium was held as part of the Western Society of Weed Scientists annual meeting to synthesize our current knowledge of the ecological impacts and management of two notorious LSIGs: Arundo donax and Phragmites australis. In this volume of Invasive Plant Science and Management, symposium participants provide articles summarizing existing knowledge, recent research progress, and research needs for these two taxa. Here, we summarize the basic biology of these species and suggest the use of a more holistic approach to deal with the effects and management of LSIG invasions. C1 [Lambert, Adam M.] Univ Calif Santa Barbara, Inst Marine Sci, Santa Barbara, CA 93106 USA. Smithsonian Trop Res Inst, Panama City, Panama. RP Lambert, AM (reprint author), Univ Calif Santa Barbara, Inst Marine Sci, Santa Barbara, CA 93106 USA. EM lambert@msi.ucsb.edu NR 54 TC 21 Z9 21 U1 3 U2 56 PU WEED SCI SOC AMER PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044-8897 USA SN 1939-7291 EI 1939-747X J9 INVAS PLANT SCI MANA JI Invasive Plant Sci. Manag. PD OCT-DEC PY 2010 VL 3 IS 4 BP 489 EP 494 DI 10.1614/IPSM-D-10-00031.1 PG 6 WC Plant Sciences SC Plant Sciences GA 778MG UT WOS:000291707800014 ER PT J AU Saltonstall, K Lambert, A Meyerson, LA AF Saltonstall, Kristin Lambert, Adam Meyerson, Laura A. TI Genetics and Reproduction of Common (Phragmites australis) and Giant Reed (Arundo donax) SO INVASIVE PLANT SCIENCE AND MANAGEMENT LA English DT Article DE Clonal; hybridization; large-statured invasive grass; plant dispersal; rhizome ID TRIN EX STEUDEL; NORTH-AMERICA; SEEDLING GROWTH; SALT MARSHES; ASEXUAL REPRODUCTION; SEXUAL REPRODUCTION; CHROMOSOME-NUMBERS; CRYPTIC INVASION; UNITED-STATES; PLOIDY LEVEL AB Genetic diversity and reproductive characteristics may play an important role in the invasion process. Here, we review the genetic structure and reproductive characteristics of common reed and giant reed, two of the most aggressive, large-statured invasive grasses in North America. Common reed reproduces both sexually and asexually and has a complex population structure, characterized by three subspecies with overlapping distributions; of which, one is introduced, one native, and the third is of unknown origins. These three subspecies show varying levels of genetic diversity, with introduced common reed having high levels of nuclear diversity, indicating that multiple introductions have likely occurred. In contrast, giant reed has low genetic diversity and appears to reproduce solely via asexual fragments yet is highly aggressive in parts of its introduced range. Both species are well-adapted for growth in human-dominated landscapes, which is presumably facilitated by their rhizomatous growth habit. C1 [Saltonstall, Kristin] Smithsonian Trop Res Inst, Panama City, Panama. Eastern Connecticut State Univ, Dept Biol, Willimantic, CT 06226 USA. Univ Rhode Isl, Kingston, RI 02881 USA. RP Saltonstall, K (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Panama City, Panama. EM kristin.saltonstall@aya.yale.edu RI Meyerson, Laura/K-9013-2012; Meyerson, Laura/D-4487-2013 FU Dr. Eldredge Bermingham; Eastern Connecticut State University; Center for Invasive Plant Management, Montana State University; U.S. Department of Agriculture Agricultural Experiment Station [0208537] FX We thank the organizers of the "Arundol Phragmites Symposium" at the Western Society of Weed Science annual meeting in 2008. We thank Tom Dudley for sharing his knowledge of Arundo donax ecology and reproduction and Jacques Brisson, Jane Molofsky, and two anonymous reviewers for their comments on earlier versions of the manuscript. K. S. thanks Dr. Eldredge Bermingham for financial support and use of his laboratory facilities at the Smithsonian Tropical Research Institute. A.M.L. received grant support from Eastern Connecticut State University and from the Center for Invasive Plant Management, Montana State University. L.A.M. received support from the U.S. Department of Agriculture Agricultural Experiment Station grant 0208537. NR 83 TC 28 Z9 28 U1 0 U2 43 PU WEED SCI SOC AMER PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044-8897 USA SN 1939-7291 J9 INVAS PLANT SCI MANA JI Invasive Plant Sci. Manag. PD OCT-DEC PY 2010 VL 3 IS 4 BP 495 EP 505 DI 10.1614/IPSM-09-053.1 PG 11 WC Plant Sciences SC Plant Sciences GA 778MG UT WOS:000291707800015 ER PT J AU Meyerson, LA Lambert, AM Saltonstall, K AF Meyerson, Laura A. Lambert, Adam M. Saltonstall, Kristin TI A Tale of Three Lineages: Expansion of Common Reed (Phragmites australis) in the U.S. Southwest and Gulf Coast SO INVASIVE PLANT SCIENCE AND MANAGEMENT LA English DT Article DE Hybridization; desert vegetation; food web; plant invasion; conservation ID NORTH-AMERICA; POPULATIONS; WETLANDS AB The common reed invasion in North America has spanned two centuries and is still ongoing. This expansion comprises two main forms: an introduced Eurasian lineage (identified here as "Introduced Phragmites") and a Gulf Coast lineage of unknown origin (identified here as "Gulf Coast Phragmites"). Both lineages are spreading beyond their current ranges and are colonizing Southwestern and Gulf Coast ecosystems where they have not previously existed. As a result, the native North American lineage of common reed (hereafter "native Phragmites") has declined in many places. The recent invasion of the U.S. Southwest by Introduced and Gulf Coast Phragmites lineages has made this the only region in the world colonized by all three lineages. Along the central Gulf Coast where Gulf Coast Phragmites remains the dominant form, Introduced Phragmites has also recently invaded the Mississippi River delta. The consequences of these new invasions are uncertain, but a rapid response is needed to protect native species and ecosystems and reduce future control costs. C1 [Meyerson, Laura A.] Univ Rhode Isl, Dept Nat Resources Sci, Kingston, RI 02881 USA. Univ Calif Santa Barbara, Inst Marine Sci, Santa Barbara, CA 93106 USA. Smithsonian Trop Res Inst, Panama City, Panama. RP Meyerson, LA (reprint author), Univ Rhode Isl, Dept Nat Resources Sci, 1 Greenhouse Rd, Kingston, RI 02881 USA. EM Laura_Meyerson@uri.edu RI Meyerson, Laura/K-9013-2012; Meyerson, Laura/D-4487-2013 NR 29 TC 22 Z9 23 U1 1 U2 31 PU WEED SCI SOC AMER PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044-8897 USA SN 1939-7291 J9 INVAS PLANT SCI MANA JI Invasive Plant Sci. Manag. PD OCT-DEC PY 2010 VL 3 IS 4 BP 515 EP 520 DI 10.1614/IPSM-D-09-00052.1 PG 6 WC Plant Sciences SC Plant Sciences GA 778MG UT WOS:000291707800017 ER PT J AU Borojevic, K Steiner, WE Gerisch, R Zazzaro, C Ward, C AF Borojevic, Ksenija Steiner, Warren E., Jr. Gerisch, Rainer Zazzaro, Chiara Ward, Cheryl TI Pests in an ancient Egyptian harbor SO JOURNAL OF ARCHAEOLOGICAL SCIENCE LA English DT Article DE Plants; Pests; Tenebrionidae; Shipworms; Red Sea; Egypt; Punt ID STORED PRODUCTS; PLANTS; RECORDS; INSECT AB Our investigations combine detailed identification and interpretation of plant remains and associated fauna and their mode of arrival in one of the rock-cut galleries, Cave 3, at the site of Mersa/Wadi Gawasis on Egypt's Red Sea coast. The site served as a staging area and harbor from which Middle Kingdom pharaohs launched seafaring expeditions to the land of Punt in the early second millennium BC. Quantities of wood, including ship timbers, fastenings, debris related to ship dismantling and reworking, and charcoal were excavated and analyzed. Evidence of marine mollusk infestation (shipworm) was abundant in Cave 3, as were the remains of insect pests of stored foods. We also report on a unique find of a plaster "spill" that preserved the floor of Cave 3 as it was when people worked in the gallery ca. 3800 years ago. The plaster spill created a sealed deposit of plant and insect remains with a diagnostic ceramic fragment, allowing us to securely associate insect remains and "hollow" spikelets of emmer wheat (Triticum dicoccum) recovered from the gallery. An impression of the beetle Trachyderma hispida and its associated exoskeleton fragments provide new evidence of this species as a potential pest not yet reported from an archaeological grain storage site in Egypt. The finding of Tenebroides mauritanicus from the same deposit is the earliest known association of this pest with stored grains. These unique finds shed new light on the risks associated with preserving food supplies, combating pest infestation, and dealing with marine organisms on land and at sea in the pharaonic harbor. (C) 2010 Elsevier Ltd. All rights reserved. C1 [Borojevic, Ksenija] Boston Univ, Dept Archaeol, Boston, MA 02215 USA. [Steiner, Warren E., Jr.] Natl Museum Nat Hist, Smithsonian Inst, Dept Entomol, Washington, DC 20560 USA. [Gerisch, Rainer] Free Univ Berlin, Inst Biol, D-14195 Berlin, Germany. [Zazzaro, Chiara] Univ Naples Orientale, Dipartemento Studi & Ric Africa & Paesi Arabi, Lab Archeol, I-80134 Naples, Italy. [Ward, Cheryl] Coastal Carolina Univ, Ctr Archaeol & Anthropol, Dept Hist, Conway, SC 29528 USA. RP Borojevic, K (reprint author), Boston Univ, Dept Archaeol, 675 Commonwealth Ave, Boston, MA 02215 USA. EM boro@bu.edu; steinerw@si.edu; Gerisch1@aol.com; c.zazzaro@exeter.ac.uk; cward@coastal.edu FU Ministry for the University and Research, Rome, Italy (FIRB); University of Naples "I'Orientale," Naples, Italy; Italian Institute for Africa; Orient, Rome, Italy; Glen Dash Charitable Foundation, Woodstock; SCIEM; University of Naples "Suor Orsola di Benincasa," Naples, Italy FX Funds for the archaeological expedition at Mersa/Wadi Gawasis were granted by the Ministry for the University and Research, Rome, Italy (FIRB 2003); University of Naples "I'Orientale," Naples, Italy; Italian Institute for Africa and the Orient, Rome, Italy; generous contributions by Mr. Wallace Sellers, Lahaska, PA; and the Glen Dash Charitable Foundation, Woodstock, CT. Prof. Otto Cichocki and Dr. Carla Pepe participated with Research funds from SCIEM 2000, Project 7, and the University of Naples "Suor Orsola di Benincasa," Naples, Italy, respectively. The first author (K.B.) thanks the following colleagues for their help with identification from the photos: Yoel Melamed and Mordai Kislev for the help of some of the ambiguous plant specimens, Rebecca Mountain for the help with the identification of the monocotyledons, and W. Van Neer for confirming the identification of ovicaprine coprolites. Paul Goldberg and Francesco Berna provided useful comments and Trina Arpin helped with editing. All five authors are grateful to Kathryn Bard and Rodolfo Fattovich for providing them with an opportunity to be part of the Mersa/Wadi Gawasis research team. NR 45 TC 3 Z9 3 U1 0 U2 11 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0305-4403 J9 J ARCHAEOL SCI JI J. Archaeol. Sci. PD OCT PY 2010 VL 37 IS 10 BP 2449 EP 2458 DI 10.1016/j.jas.2010.04.013 PG 10 WC Anthropology; Archaeology; Geosciences, Multidisciplinary SC Anthropology; Archaeology; Geology GA 643AX UT WOS:000281265900009 ER PT J AU del Hoyo-Melendez, JM Mecklenburg, MF AF del Hoyo-Melendez, Julio M. Mecklenburg, Marion F. TI A survey on the light-fastness properties of organic-based Alaska Native artifacts SO JOURNAL OF CULTURAL HERITAGE LA English DT Article DE Alaska Native artifacts; Light-fastness; Micro-fading tester; Ethnographic collections AB A series of light-fastness tests were conducted on a group of ethnographic objects that will be on exhibit at the Smithsonian Institution Arctic Studies Center, a recent addition to the Anchorage Museum at Rasmuson Center in Alaska. The objects surveyed belong to the collections of the Smithsonian National Museum of Natural History and the Smithsonian National Museum of the American Indian. This work was designed as a feasibility study on the use of a micro-fading tester as a non-contact and non-destructive technique to evaluate the light-stability of materials present in ethnographic collections. A broad range of objects containing a wide variety of materials were selected for the study. The materials investigated included a variety of dyes applied on silk, cotton, and wool substrates along with some unusual materials such as tanned skin and seal gut skin. The results from this investigation have allowed establishing exhibition recommendations taking into consideration the sensitivity of each object, light levels in the museum building, and estimated light exposures based on the duration of the exhibit. The micro-fading tester has proven to be a very useful tool for determining the light-stability of ethnographic materials without causing any harm to the objects. Objects containing equivalent materials are usually classified under a general category based on their probable sensitivity to light. However, micro-fading test results have permitted the detection of dissimilarities among some of these objects, which could be associated to variations in prior fading histories, the quality of raw materials, and different preparation methods. (C) 2010 Elsevier Masson SAS. All rights reserved. C1 [del Hoyo-Melendez, Julio M.; Mecklenburg, Marion F.] Smithsonian Inst, Museum Conservat Inst, Suitland, MD 20746 USA. RP del Hoyo-Melendez, JM (reprint author), Univ Politecn Valencia, Inst Univ Restaurac Patrimonio, Camino Vera S-N 14,Edificio 9B, Valencia 46022, Spain. EM judeho1@doctor.upv.es; mecklenburgm@si.edu RI del Hoyo-Melendez, Julio/B-1395-2012 OI del Hoyo-Melendez, Julio/0000-0003-2163-2149 FU Smithsonian Institution Office of Research and Training Services FX This research was supported through a Pre-Doctoral Fellowship from the Smithsonian Institution Office of Research and Training Services. The authors would like to thank the staff from the Anthropology Conservation Laboratory of the National Museum of the Natural History and also the staff from the Conservation Laboratory of the National Museum of the American Indian for authorizing the use of artifacts in their collections for this survey. Special thanks to Kim Cullen Cobb, Landis Smith and Michelle Austin-Dennehy for all their support and assistance in coordinating this project. The authors wish to express their gratitude to Magdalena Moskal for providing valuable comments to this work. NR 32 TC 6 Z9 6 U1 1 U2 7 PU ELSEVIER FRANCE-EDITIONS SCIENTIFIQUES MEDICALES ELSEVIER PI PARIS PA 23 RUE LINOIS, 75724 PARIS, FRANCE SN 1296-2074 J9 J CULT HERIT JI J. Cult. Herit. PD OCT-DEC PY 2010 VL 11 IS 4 BP 493 EP 499 DI 10.1016/j.culher.2010.01.004 PG 7 WC Archaeology; Art; Chemistry, Analytical; Geosciences, Multidisciplinary; Materials Science, Multidisciplinary; Spectroscopy SC Archaeology; Art; Chemistry; Geology; Materials Science; Spectroscopy GA 660XO UT WOS:000282680500017 ER PT J AU Pruitt, RJ Culver, SJ Buzas, MA Corbett, DR Horton, BP Mallinson, DJ AF Pruitt, Rebecca J. Culver, Stephen J. Buzas, Martin A. Corbett, D. Reide Horton, Benjamin P. Mallinson, David J. TI MODERN FORAMINIFERAL DISTRIBUTION AND RECENT ENVIRONMENTAL CHANGE IN CORE SOUND, NORTH CAROLINA, USA SO JOURNAL OF FORAMINIFERAL RESEARCH LA English DT Article ID ALBEMARLE-ESTUARINE-SYSTEM; NEUSE RIVER ESTUARY; BENTHIC FORAMINIFERA; OUTER BANKS; PARALIC ENVIRONMENTS; MARSH FORAMINIFERA; CONTINENTAL-SHELF; CHESAPEAKE BAY; PAMLICO-SOUND; SEA-LEVEL AB Core Sound, a shallow, narrow estuarine lagoon located behind North Carolina's southern Outer Banks, was studied to document modern foraminiferal distributions and identify environmental changes during the past ca. 90 years. Seventy-six samples collected in 2004 were analyzed to establish the modern distribution and abundance of foraminifera. Cluster analysis defined four modern biofacies: Marsh (dominated by Trochammina inflata and Haplophragmoides wilberti), Estuarine High Salinity A (dominated by Ammonia parkinsoniana and Elphidium mexicanum), Estuarine High Salinity B (dominated by Ammonia parkinsoniana and Elphidium excavatum), and Estuarine Low Salinity (dominated by Ammotium salsum, Ammonia parkinsoniana and Elphidium gunteri). The four biofacies were also recognized by discriminant analysis. Comparison of the 2004 distributional data with those derived from samples collected in 1959 from central and eastern Core Sound revealed that Elphidium decreased while Ammonia increased in relative abundance. Other researchers have suggested that such a trend reflects increased eutrophication, although there is no independent evidence for this in Core Sound. The temporal comparison also showed that Quinqueloculina has become more widespread immediately adjacent to barrier islands, which might relate to an increase in subaquatic vegetation. Five short cores were taken in mainland bays on the western margin of Core Sound. Analysis of radionuclides ((210)Pb and (137)Cs) provided a chronostratigraphic framework for two of the cores. To aid paleoenvironmental interpretations, foraminiferal data from core sediments dated as ca. 90 yr were entered as unknowns into the modern distribution discriminant analysis. Samples from mainland bay cores were classified with modern biofacies and indicated no significant foraminiferal change in the mainland bays over the last ca. 90 years. C1 [Pruitt, Rebecca J.; Culver, Stephen J.; Corbett, D. Reide; Mallinson, David J.] E Carolina Univ, Dept Geol Sci, Greenville, NC 27858 USA. [Corbett, D. Reide] E Carolina Univ, Inst Coastal Sci & Policy, Greenville, NC 27858 USA. [Buzas, Martin A.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. [Horton, Benjamin P.] Univ Penn, Dept Earth & Environm Sci, Philadelphia, PA 19104 USA. RP Pruitt, RJ (reprint author), E Carolina Univ, Dept Geol Sci, Greenville, NC 27858 USA. FU [02ERAG0044] FX We thank Jim Watson, John Woods, and Dorothea Ames for their technical assistance in the field and laboratory and Drs. P. Buzas-Stephens, E. Leorri, and B. Hayward for their reviews. This research is part of the North Carolina Coastal Geology Cooperative Program. Funding for the USGS cooperative agreement award 02ERAG0044 is gratefully acknowledged. NR 90 TC 11 Z9 11 U1 1 U2 15 PU CUSHMAN FOUNDATION FORAMINIFERAL RES PI CAMBRIDGE PA MUSEUM COMPARATIVE ZOOLOGY, DEPT INVERTEBRATE PALEONTOLOGY 26 OXFORD ST, HARVARD UNIV, CAMBRIDGE, MA 02138 USA SN 0096-1191 J9 J FORAMIN RES JI J. Foraminifer. Res. PD OCT PY 2010 VL 40 IS 4 BP 344 EP 365 PG 22 WC Paleontology SC Paleontology GA 656RG UT WOS:000282353700004 ER PT J AU Chaimanee, V Warrit, N Chantawannakul, P AF Chaimanee, Veeranan Warrit, Natapot Chantawannakul, Panuwan TI Infections of Nosema ceranae in four different honeybee species SO JOURNAL OF INVERTEBRATE PATHOLOGY LA English DT Article DE Apis mellifera; Asian honeybee; Nosema ceranae; Nosema apis; Microsporidia ID APIS-MELLIFERA; MICROSPORIDIAN PARASITE; MOLECULAR CHARACTERIZATION; COLONY COLLAPSE; BEE; EUROPE AB The microsporidium Nosema ceranae is detected in honeybees in Thailand for the first time. This endoparasite has recently been reported to infect most Apis mellifera honeybee colonies in Europe, the US, and parts of Asia, and is suspected to have displaced the endemic endoparasite species, Nosema apis, from the western A. mellifera. We collected and identified species of microsporidia from the European honeybee (A. mellifera), the cavity nesting Asian honeybee (Apis cerana), the dwarf Asian honeybee (Apis florea) and the giant Asian honeybee (Apis dorsata) from colonies in Northern Thailand. We used multiplex PCR technique with two pairs of primers to differentiate N. ceranae from N. apis. From 80 A. mellifera samples, 62 (77.5%) were positively identified for the presence of the N. ceranae. Amongst 46 feral colonies of Asian honeybees (A. cerana, A. florea and A. dorsata) examined for Nosema infections, only N. ceranae could be detected. No N. apis was found in our samples. N. ceranae is found to be the only microsporidium infesting honeybees in Thailand. Moreover, we found the frequencies of N. ceranae infection in native bees to be less than that of A. mellifera. (C) 2010 Elsevier Inc. All rights reserved. C1 [Chaimanee, Veeranan; Chantawannakul, Panuwan] Chiang Mai Univ, Fac Sci, Dept Biol, Chiang Mai 50200, Thailand. [Warrit, Natapot] Chulalongkorn Univ, Fac Sci, Dept Biol, Ctr Excellence Entomol, Bangkok 10330, Thailand. [Warrit, Natapot] Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Chantawannakul, P (reprint author), Chiang Mai Univ, Fac Sci, Dept Biol, Chiang Mai 50200, Thailand. EM panuwan@gmail.com FU Commission on Higher Education, Thailand; Thailand Research Fund [RSA 5280010] FX We would like to thank the Commission on Higher Education, Thailand for support by Grant funding under the program of Strategic Scholarships for Frontier Research Network for the Joint Ph.D. Program Thai Doctoral degree for this research. Also we acknowledge the Thailand Research Fund (RSA 5280010) for financial support. We are grateful to Dr. Yanping Chen, Dr. Ingemar Fries and Dr. Requel Martin-Hernandez for providing bee samples. NR 29 TC 25 Z9 25 U1 3 U2 14 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0022-2011 J9 J INVERTEBR PATHOL JI J. Invertebr. Pathol. PD OCT PY 2010 VL 105 IS 2 BP 207 EP 210 DI 10.1016/j.jip.2010.06.005 PG 4 WC Zoology SC Zoology GA 650DN UT WOS:000281829300016 PM 20600087 ER PT J AU Pavicic, M McKay, BD Megill, ND Fresl, K AF Pavicic, Mladen McKay, Brendan D. Megill, Norman D. Fresl, Kresimir TI Graph approach to quantum systems SO JOURNAL OF MATHEMATICAL PHYSICS LA English DT Article ID KOCHEN-SPECKER THEOREM; SMALL STATE-SPACES; ORTHOMODULAR LATTICES; GREECHIE DIAGRAMS; HILBERT-SPACES; LOGIC; CONSTRUCTIONS; VARIETIES; MECHANICS; EQUATIONS AB Using a graph approach to quantum systems, we show that descriptions of 3-dim Kochen-Specker (KS) setups as well as descriptions of 3-dim spin systems by means of Greechie diagrams (a kind of lattice) that we find in the literature are wrong. Correct lattices generated by McKay-Megill-Pavicic (MMP) hypergraphs and Hilbert subspace equations are given. To enable future exhaustive generation of 3-dim KS setups by means of our recently found stripping technique, bipartite graph generation is used to provide us with lattices with equal numbers of elements and blocks (orthogonal triples of elements)-up to 41 of them. We obtain several new results on such lattices and hypergraphs, in particular, on properties such as superposition and orthoraguesian equations. (C) 2010 American Institute of Physics. [doi:10.1063/1.3491766] C1 [Pavicic, Mladen] Harvard Univ, Inst Theoret Atom Mol & Opt Phys, Dept Phys, Cambridge, MA 02138 USA. [Pavicic, Mladen] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Pavicic, Mladen] Univ Zagreb, Fac Civil Engn, Chair Phys, Zagreb 10000, Croatia. [McKay, Brendan D.] Australian Natl Univ, Sch Comp Sci, Canberra, ACT 0200, Australia. [Megill, Norman D.] Boston Informat Grp, Lexington, MA 02420 USA. [Fresl, Kresimir] Univ Zagreb, Fac Civil Engn, Dept Tech Mech, Zagreb 10000, Croatia. RP Pavicic, M (reprint author), Harvard Univ, Inst Theoret Atom Mol & Opt Phys, Dept Phys, Cambridge, MA 02138 USA. EM mpavicic@grad.hr FU U.S. National Science Foundation; Smithsonian Astrophysical Observatory and Ministry of Science, Education, and Sport of Croatia [082-0982562-3160] FX This work is supported by the U.S. National Science Foundation through a grant for the Institute for Theoretical Atomic, Molecular, and Optical Physics (ITAMP) at Harvard University and Smithsonian Astrophysical Observatory and Ministry of Science, Education, and Sport of Croatia through the Project No. 082-0982562-3160. NR 70 TC 6 Z9 6 U1 0 U2 3 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 0022-2488 EI 1089-7658 J9 J MATH PHYS JI J. Math. Phys. PD OCT PY 2010 VL 51 IS 10 AR 102103 DI 10.1063/1.3491766 PG 31 WC Physics, Mathematical SC Physics GA 674MR UT WOS:000283750800003 ER PT J AU Lambert, JB Heckenbach, EA Wu, YY Santiago-Blay, JA AF Lambert, Joseph B. Heckenbach, Eric A. Wu, Yuyang Santiago-Blay, Jorge A. TI Characterization of Plant Exudates by Principal-Component and Cluster Analyses with Nuclear Magnetic Resonance Variables SO JOURNAL OF NATURAL PRODUCTS LA English DT Article ID GAS CHROMATOGRAPHY/MASS SPECTROMETRY; IONIZATION MASS-SPECTROMETRY; PATTERN-RECOGNITION; SPECTROSCOPY; NMR; CLASSIFICATION; SOLVENTS; RESINS; URINE AB Principal-component and cluster analyses have been applied to nuclear magnetic resonance data for exudates derived from both conifers and angiosperms in order to classify these materials on the basis of molecular structure. The method succeeds in distinguishing resins produced by the conifer families Araucariaceae, Cupressaceae, and Pinaceae from each other and from resins produced by the angiosperm family Fabaceae. Other exudate types, including gums, gum resins, and kinos, also are distinguished from each other and from the resins. C1 [Lambert, Joseph B.; Heckenbach, Eric A.; Wu, Yuyang] Northwestern Univ, Dept Chem, Evanston, IL 60208 USA. [Santiago-Blay, Jorge A.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. RP Lambert, JB (reprint author), Northwestern Univ, Dept Chem, 2145 Sheridan Rd, Evanston, IL 60208 USA. EM jlambert@northwestern.edu FU Gallaudet University FX The authors are grateful to grants from Gallaudet University for support of this work and to K. Moy for data reduction. Individuals who provided samples have been acknowledged previously.5.7-10 NR 22 TC 6 Z9 8 U1 0 U2 6 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0163-3864 EI 1520-6025 J9 J NAT PROD JI J. Nat. Prod. PD OCT PY 2010 VL 73 IS 10 BP 1643 EP 1648 DI 10.1021/np100318n PG 6 WC Plant Sciences; Chemistry, Medicinal; Pharmacology & Pharmacy SC Plant Sciences; Pharmacology & Pharmacy GA 668SB UT WOS:000283288900005 PM 20860390 ER PT J AU Rothman, LS Gordon, IE Barber, RJ Dothe, H Gamache, RR Goldman, A Perevalov, VI Tashkun, SA Tennyson, J AF Rothman, L. S. Gordon, I. E. Barber, R. J. Dothe, H. Gamache, R. R. Goldman, A. Perevalov, V. I. Tashkun, S. A. Tennyson, J. TI HITEMP, the high-temperature molecular spectroscopic database SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE Spectroscopic database; Molecular spectroscopy; Molecular absorption; Line parameters; High-temperature spectroscopy; HITEMP ID POTENTIAL-ENERGY SURFACE; DIPOLE-MOMENT FUNCTION; EINSTEIN-A-COEFFICIENTS; BROADENED HALF-WIDTHS; WATER-VAPOR; LINE LIST; HITRAN DATABASE; CARBON-DIOXIDE; HIGH-ACCURACY; NITRIC-OXIDE AB A new molecular spectroscopic database for high-temperature modeling of the spectra of molecules in the gas phase is described. This database, called HITEMP, is analogous to the HITRAN database but encompasses many more bands and transitions than HITRAN for the absorbers H2O, CO2, CO, NO, and OH. HITEMP provides users with a powerful tool for a great many applications: astrophysics, planetary and stellar atmospheres, industrial processes, surveillance, non-local thermodynamic equilibrium problems, and investigating molecular interactions, to name a few. The sources and implementation of the spectroscopic parameters incorporated into HITEMP are discussed. (C) 2010 Elsevier Ltd. All rights reserved. C1 [Rothman, L. S.; Gordon, I. E.] Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. [Barber, R. J.; Tennyson, J.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Gamache, R. R.] Univ Massachusetts, Sch Marine Sci, Dept Environm Earth & Atmospher Sci, Lowell, MA 01854 USA. [Dothe, H.] Spectral Sci Inc, Burlington, MA 01803 USA. [Goldman, A.] Univ Denver, Dept Phys, Denver, CO 80208 USA. [Perevalov, V. I.; Tashkun, S. A.] Russian Acad Sci, Siberian Branch, Inst Atmospher Opt, Tomsk 634055, Russia. RP Rothman, LS (reprint author), Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, 60 Garden St, Cambridge, MA 02138 USA. EM LRothman@cfa.harvard.edu RI Tennyson, Jonathan/I-2222-2012; Tashkun, Sergey/E-8682-2014; OI Tennyson, Jonathan/0000-0002-4994-5238; Gordon, Iouli/0000-0003-4763-2841; Rothman, Laurence/0000-0002-3837-4847 FU NASA [NAG5-13534]; Planetary Atmospheres program [NNX10AB94G]; Spectral Sciences, Inc.; National Science Foundation [ATM-0803135]; Russian Fund of Basic Research [06-05-39016-(1)GammaPhiEH_a, 09-05-93105-HPiHalephJI_a] FX We acknowledge the support of NASA through the Earth Observing System (EOS) program under the Grant no. NAG5-13534 and the Planetary Atmospheres program under Grant no. NNX10AB94G. We also acknowledge the CHEMS (Computation of Highly Excited Molecular Spectra) SBIR project through Spectral Sciences, Inc. RRG acknowledges support of this research by the National Science Foundation through Grant no. ATM-0803135. VIP and SAT acknowledge support by the Russian Fund of Basic Research under the Grant nos. 06-05-39016-(1)Gamma Phi EH_a and 09-05-93105-H Pi H aleph JI_a. NR 85 TC 403 Z9 421 U1 6 U2 57 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD OCT PY 2010 VL 111 IS 15 SI SI BP 2139 EP 2150 DI 10.1016/j.jqsrt.2010.05.001 PG 12 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 643CE UT WOS:000281269800002 ER PT J AU Dubernet, ML Boudon, V Culhane, JL Dimitrijevic, MS Fazliev, AZ Joblin, C Kupka, F Leto, G Le Sidaner, P Loboda, PA Mason, HE Mason, NJ Mendoza, C Mulas, G Millar, TJ Nunez, LA Perevalov, VI Piskunov, N Ralchenko, Y Rixon, G Rothman, LS Roueff, E Ryabchikova, TA Ryabtsev, A Sahal-Brechot, S Schmitt, B Schlemmer, S Tennyson, J Tyuterev, VG Walton, NA Wakelam, V Zeippen, CJ AF Dubernet, M. L. Boudon, V. Culhane, J. L. Dimitrijevic, M. S. Fazliev, A. Z. Joblin, C. Kupka, F. Leto, G. Le Sidaner, P. Loboda, P. A. Mason, H. E. Mason, N. J. Mendoza, C. Mulas, G. Millar, T. J. Nunez, L. A. Perevalov, V. I. Piskunov, N. Ralchenko, Y. Rixon, G. Rothman, L. S. Roueff, E. Ryabchikova, T. A. Ryabtsev, A. Sahal-Brechot, S. Schmitt, B. Schlemmer, S. Tennyson, J. Tyuterev, V. G. Walton, N. A. Wakelam, V. Zeippen, C. J. TI Virtual atomic and molecular data centre SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE Atomic data; Molecular data; Astrophysics; Atmospheric physics; Fusion; Radiation; Lighting; Space physics; Planetology ID SPECTROSCOPIC DATABASE; ONLINE DATABASE; ICE; ASTROCHEMISTRY; ATMOSPHERE; MIXTURES; PROFILE; BAND; CH4 AB The Virtual Atomic and Molecular Data Centre (VAMDC, http://www.vamdc.eu) is a European Union funded collaboration between groups involved in the generation, evaluation, and use of atomic and molecular data. VAMDC aims to build a secure, documented, flexible and interoperable e-science environment-based interface to existing atomic and molecular data. The project will cover establishing the core consortium, the development and deployment of the infrastructure and the development of interfaces to the existing atomic and molecular databases. It will also provide a forum for training potential users and dissemination of expertise worldwide. This review describes the scope of the VAMDC project; it provides a survey of the atomic and molecular data sets that will be included plus a discussion of how they will be integrated. Some applications of these data are also discussed. (C) 2010 Elsevier Ltd. All rights reserved. C1 [Dubernet, M. L.] Univ Paris 06, CNRS INP, UMR 7092, Lab Phys Mol Atmosphere & Astrophys, F-75252 Paris 05, France. [Dubernet, M. L.; Roueff, E.] Observ Paris, CNRS INSU, UMR 8102, Lab Univers & Theories,Sect Meudon, F-92195 Meudon, France. [Boudon, V.] Univ Bourgogne, CNRS, UMR 5209, Lab Interdisciplinaire Carnot Bourgogne, F-21078 Dijon, France. [Culhane, J. L.] Univ Coll London, Mullard Space Sci Lab, Surrey RH5 6NT, England. [Dimitrijevic, M. S.] Astron Observ, Belgrade 11060, Serbia. [Fazliev, A. Z.; Perevalov, V. I.] Russian Acad Sci, Siberian Branch, VE Zuev Inst Atmospher Opt, Tomsk 634021, Russia. [Joblin, C.] Univ Toulouse 3, CNRS INSU, UMR 5187, Ctr Etud Spatiale Rayonnements, F-31028 Toulouse 9, France. [Kupka, F.] Univ Vienna, Fac Math, A-1090 Vienna, Austria. [Leto, G.] Osserv Astrofis Catania, Ist Nazl Astrofis, I-95123 Catania, Italy. [Le Sidaner, P.] Observ Paris, CNRS INSU, UMS 2201, VO Paris Data Ctr,Div Informat Observ, F-92195 Meudon, France. [Loboda, P. A.] All Russian Inst Tech Phys RFNTC VNIITF, Russian Fed Nucl Ctr, Snezhinsk 456770, Chelyabinsk Reg, Russia. [Mason, H. E.] Ctr Math Sci, Dept Appl Math & Theoret Phys, Cambridge CB3 0WA, England. [Mason, N. J.] Open Univ, Fac Sci, Milton Keynes MK7 6AA, Bucks, England. [Mendoza, C.; Nunez, L. A.] Univ Los Andes, CeCalCULA, Corp Parque Tecnol Merida, Ctr Nacl Calculo Cient, Merida 5101, Venezuela. [Mendoza, C.] Inst Venezolano Invest Cient, Ctr Fis, Caracas 1020A, Venezuela. [Nunez, L. A.] Univ Ind Santander, Esc Fis, GIRG, Bucaramanga, Colombia. [Mulas, G.] Osservatorio Astron Cagliari, Ist Nazl Astrofis, I-09012 Capoterra, CA, Italy. [Piskunov, N.] Uppsala Univ, Dept Phys & Astron, S-75120 Uppsala, Sweden. [Ralchenko, Y.] NIST, Atom Phys Div, Gaithersburg, MD 20899 USA. [Rothman, L. S.] Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. [Millar, T. J.] Queens Univ Belfast, Sch Math & Phys, Belfast BT7 1NN, Antrim, North Ireland. [Ryabchikova, T. A.] RAS, Inst Astron, Moscow 119017, Russia. [Ryabtsev, A.] RAS, Inst Spect, Troitsk 142190, Russia. [Sahal-Brechot, S.; Zeippen, C. J.] Observ Paris, CNRS INSU, UMR 8112, Lab Etud Rayonnement & Mat Astrophys, F-75014 Paris, France. [Schmitt, B.] Univ Grenoble 1, CNRS INSU, UMR 5109, Lab Planetol Grenoble, F-38041 Grenoble 9, France. [Schlemmer, S.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Tennyson, J.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Tyuterev, V. G.] Univ Reims, UFR Sci Exactes & Nat, CNRS INP, Grp Spect Mol & Atmospher,UMR 6089, F-51687 Reims 2, France. [Rixon, G.; Walton, N. A.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Wakelam, V.] Univ Bordeaux, CNRS INSU, UMR 5804, Lab Astrophys Bordeaux, F-33271 Floirac, France. RP Dubernet, ML (reprint author), Univ Paris 06, CNRS INP, UMR 7092, Lab Phys Mol Atmosphere & Astrophys, Case 76,4 Pl Jussieu, F-75252 Paris 05, France. EM Marie-Lise.Dubernet-Tuckey@upmc.FR RI BOUDON, Vincent/A-4504-2010; Ralchenko, Yuri/B-7687-2011; Ralchenko, Yuri/E-9297-2016; Schmitt, Bernard/A-1064-2009; Tennyson, Jonathan/I-2222-2012; Mulas, Giacomo/B-7480-2013; Nunez, Luis/D-3404-2013; Schlemmer, Stephan/E-2903-2015; Leto, Giuseppe/N-3355-2015; OI Ralchenko, Yuri/0000-0003-0083-9554; Schmitt, Bernard/0000-0002-1230-6627; Tennyson, Jonathan/0000-0002-4994-5238; Mulas, Giacomo/0000-0003-0602-6669; Nunez, Luis/0000-0003-4575-5899; Wakelam, Valentine/0000-0001-9676-2605; Millar, Tom/0000-0001-5178-3656; Schlemmer, Stephan/0000-0002-1421-7281; Leto, Giuseppe/0000-0002-0040-5011; Rothman, Laurence/0000-0002-3837-4847 FU VAMDC [INFRA-2008-1.2.2, 239108] FX VAMDC is funded under the "Combination of Collaborative Projects and Coordination and Support Actions" Funding Scheme of The Seventh Framework Program. Call topic: INFRA-2008-1.2.2 Scientific Data Infrastructure. Grant Agreement number: 239108. NR 55 TC 104 Z9 109 U1 1 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 OCT PY 2010 VL 111 IS 15 SI SI BP 2151 EP 2159 DI 10.1016/j.jqsa.2010.05.004 PG 9 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 643CE UT WOS:000281269800003 ER PT J AU Tennyson, J Bernath, PF Brown, LR Campargue, A Csaszar, AG Daumont, L Gamache, RR Hodges, JT Naumenko, OV Polyansky, OL Rothman, LS Toth, RA Vandaele, AC Zobov, NF Fally, S Fazliev, AZ Furtenbacher, T Gordon, IE Hu, SM Mikhailenko, SN Voronin, BA AF Tennyson, Jonathan Bernath, Peter F. Brown, Linda R. Campargue, Alain Csaszar, Attila G. Daumont, Ludovic Gamache, Robert R. Hodges, Joseph T. Naumenko, Olga V. Polyansky, Oleg L. Rothman, Laurence S. Toth, Robert A. Vandaele, Ann Carine Zobov, Nikolai F. Fally, Sophie Fazliev, Alexander Z. Furtenbacher, Tibor Gordon, Iouli E. Hu, Shui-Ming Mikhailenko, Semen N. Voronin, Boris A. TI IUPAC critical evaluation of the rotational-vibrational spectra of water vapor. Part II Energy levels and transition wavenumbers for (HDO)-O-16, (HDO)-O-17, and (HDO)-O-18 SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE Water vapor; Transition wavenumbers; Atmospheric physics; Energy levels; MARVEL; Information system; Database; W@DIS; Infrared spectra; Microwave spectra; (HDO)-O-16; (HDO)-O-17; (HDO)-O-18 ID FOURIER-TRANSFORM SPECTROSCOPY; LASER-ABSORPTION SPECTROSCOPY; BEAM-MASER SPECTROSCOPY; HETERODYNE FREQUENCY MEASUREMENTS; LORENTZ-BROADENING COEFFICIENTS; LINE-SHIFT COEFFICIENTS; HIGH-RESOLUTION; CM(-1) REGION; MU-M; HYPERFINE STRUCTURE AB This is the second of a series of articles reporting critically evaluated rotational-vibrational line positions, transition intensities, pressure dependences, and energy levels, with associated critically reviewed assignments and uncertainties, for all the main isotopologues of water. This article presents energy levels and line positions of the following singly deuterated isotopologues of water: (HDO)-O-16, (HDO)-O-17, and (HDO)-O-18. The MARVEL (measured active rotational-vibrational energy levels) procedure is used to determine the levels, the lines, and their self-consistent uncertainties for the spectral regions 0-22708, 0-1674, and 0-12 105 cm(-1) for (HDO)-O-16, (HDO)-O-17, and (HDO)-O-18, respectively. For (HDO)-O-16, 54 740 transitions were analyzed from 76 sources, the lines come from spectra recorded both at room temperature and from hot samples. These lines correspond to 36 690 distinct assignments and 8818 energy levels. For (HDO)-O-17, only 485 transitions could be analyzed from three sources; the lines correspond to 162 MARVEL energy levels. For (HDO)-O-18, 8729 transitions were analyzed from 11 sources and these lines correspond to 1864 energy levels. The energy levels are checked against ones determined from accurate variational nuclear motion computations employing exact kinetic energy operators. This comparison shows that the measured transitions account for about 86% of the anticipated absorbance of (HDO)-O-16 at 296 K and that the transitions predicted by the MARVEL energy levels account for essentially all the remaining absorbance. The extensive list of MARVEL lines and levels obtained are given in the Supplementary Material of this article, as well as in a distributed information system applied to water, W@DIS, where they can easily be retrieved. In addition, the transition and energy level information for (H2O)-O-17 and (H2O)-O-18, given in the first paper of this series [Tennyson, et al. J Quant Spectr Rad Transfer 2009;110:573-96], has been updated. (C) 2010 Elsevier Ltd. All rights reserved. C1 [Tennyson, Jonathan; Polyansky, Oleg L.] Univ London Univ Coll, Dept Phys & Astron, London WC1E 6BT, England. [Bernath, Peter F.] Univ York, York YO10 5DD, N Yorkshire, England. [Brown, Linda R.; Toth, Robert A.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Campargue, Alain] Univ Grenoble 1, Grenoble, France. [Csaszar, Attila G.; Furtenbacher, Tibor] Eotvos Lorand Univ, Budapest, Hungary. [Daumont, Ludovic] Univ Reims, Reims, France. [Gamache, Robert R.] Univ Massachusetts, Lowell, MA USA. [Hodges, Joseph T.] NIST, Gaithersburg, MD 20899 USA. [Naumenko, Olga V.; Fazliev, Alexander Z.; Mikhailenko, Semen N.; Voronin, Boris A.] Russian Acad Sci, VE Zuev Inst Atmospher Opt, Tomsk 634021, Russia. [Polyansky, Oleg L.; Zobov, Nikolai F.] Russian Acad Sci, Inst Appl Phys, Nizhnii Novgorod, Russia. [Rothman, Laurence S.; Gordon, Iouli E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Vandaele, Ann Carine] Inst Aeron Spatiale Belgique, B-1180 Brussels, Belgium. [Fally, Sophie] Univ Libre Bruxelles, Brussels, Belgium. [Hu, Shui-Ming] Univ Sci & Technol China, Lab Bond Select Chem, Hefei 230026, Peoples R China. RP Tennyson, J (reprint author), Univ London Univ Coll, Dept Phys & Astron, Gower St, London WC1E 6BT, England. EM j.tennyson@ucl.ac.UK RI Csaszar, Attila/A-5241-2009; Hu, Shuiming/C-4287-2008; Bernath, Peter/B-6567-2012; Tennyson, Jonathan/I-2222-2012; Voronin, Boris/A-3444-2014; OI Hu, Shuiming/0000-0002-1565-8468; Bernath, Peter/0000-0002-1255-396X; Tennyson, Jonathan/0000-0002-4994-5238; Voronin, Boris/0000-0002-8743-5554; Gordon, Iouli/0000-0003-4763-2841; Rothman, Laurence/0000-0002-3837-4847 FU International Union of Pure and Applied Chemistry [2004-035-1-100]; UK Natural Environment Research Council, the Royal Society [WWLC-008535-(reintegration) MCA FP6 EC]; Scientific Research Fund. of Hungary [OTKA K77825]; European Union; Russian Foundation for Basic Research; Belgian Federal Science Policy Office [EV/35/3A, SD/AT/01A, PRODEX 1514901NLSFe(IC)]; Communaute de Belgique (Action de Recherche Concertees); NASA [NNX08AD92G]; National Science Foundation [ATM-0803135]; CNRS (INSU) FX We all thank the International Union of Pure and Applied Chemistry for funding under project 2004-035-1-100 (A database of water transitions from experiment and theory). In addition, this work has received partial support from the UK Natural Environment Research Council, the Royal Society, Grant WWLC-008535-(reintegration) MCA FP6 EC, the Scientific Research Fund. of Hungary (Grant OTKA K77825), the European Union QUASAAR Marie Curie research training network, NATO, the Russian Foundation for Basic Research, the Belgian Federal Science Policy Office (contracts EV/35/3A, SD/AT/01A, PRODEX 1514901NLSFe(IC)), the Belgian National Fund for Scientific Research (FRFC contracts), the Communaute de Belgique (Action de Recherche Concertees), the NASA laboratory astrophysics program, NASA Earth Observing System (E0S), under Grant NNX08AD92G, the National Science Foundation, through Grant no. ATM-0803135, and the Programme National LEFE (CHAT) of CNRS (INSU). Part of the research described in this paper was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 150 TC 82 Z9 89 U1 8 U2 46 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 OCT PY 2010 VL 111 IS 15 SI SI BP 2160 EP 2184 DI 10.1016/j.jqsrt.2010.06.012 PG 25 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 643CE UT WOS:000281269800004 ER PT J AU Leshchishina, O Kassi, S Gordon, IE Rothman, LS Wang, L Campargue, A AF Leshchishina, Olga Kassi, Samir Gordon, Iouli E. Rothman, Laurence S. Wang, Le Campargue, Alain TI High sensitivity CRDS of the a(1)Delta X-g(3)Sigma(-)(g) band of oxygen near 1.27 mu m: Extended observations, quadrupole transitions, hot bands and minor isotopologues SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE Oxygen; O-2; Electric quadrupole; Singlet delta; Cavity ring down spectroscopy ID CAVITY RINGDOWN SPECTROSCOPY; SUBMILLIMETER-WAVE SPECTRUM; MICROWAVE-ABSORPTION LINES; MOLECULAR-OXYGEN; GROUND-STATE; RAMAN-SPECTRUM; PRESSURE; O-16(2); O-2; COEFFICIENTS AB The CW-Cavity Ring Down Spectroscopy (CW-CRDS) technique has been used to record the high sensitivity absorption spectrum of the a(1)Delta(g)-X 3 Sigma(g)- band of oxygen near 1.27 mu m. The spectra were obtained between 7640 and 7917 cm(-1) with "natural" oxygen and with a sample highly enriched in 180. The absolute intensities of 376 and 643 oxygen transitions were measured in the two spectra. They include the alpha(1)Delta(g)-X (3)Sigma(-)(g) (0-0) bands of O-16(2), (OO)-O-16-O-18, (OO)-O-16-O-17, (OO)-O-17-O-18 and O-18(2). The (0-0) bands of O-16(2) and O-18(2) show weak quadrupole transitions with line intensities ranging from 1 x 10(-30) to 1.9 x 10(-28) cm/molecule. They are accompanied by the alpha(1)Delta(g)- X E-3; (1-1) hot bands, which are reported for the first time. The line profiles of the transitions of the (OO)-O-16-O-17 and (OO)-O-17-O-18 isotopologues were observed to be broadened due to an unresolved magnetic hyperfine structure. Accurate spectroscopic parameters of the different energy levels involved in the observed bands were derived from a global fit of the observed line positions, combined with microwave and Raman measurements available in the literature. (C) 2010 Elsevier Ltd. All rights reserved. C1 [Leshchishina, Olga; Kassi, Samir; Wang, Le; Campargue, Alain] Univ Grenoble 1, CNRS, Spectrometrie Phys Lab, F-38402 St Martin Dheres, France. [Gordon, Iouli E.; Rothman, Laurence S.; Wang, Le] Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. [Leshchishina, Olga] Zuev Inst Atmospher Opt, Lab Theoret Spect, Tomsk 634021, Russia. RP Campargue, A (reprint author), Univ Grenoble 1, CNRS, Spectrometrie Phys Lab, F-38402 St Martin Dheres, France. EM Alain.CAMPARGUE@ujf-grenoble.fr FU ANR [NT09_436466]; NASA [NAGS-13534] FX We are very thankful to Shanshan Yu for her help in using the SPF1T program. Part of this work was performed at Grenoble University under the ANR project "IDEO" (NT09_436466). The HITRAN database is supported by NASA through the Earth Observing System (EOS) program under the Grant NAGS-13534. NR 42 TC 24 Z9 24 U1 0 U2 12 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD OCT PY 2010 VL 111 IS 15 SI SI BP 2236 EP 2245 DI 10.1016/j.jqsrt.2010.05.014 PG 10 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 643CE UT WOS:000281269800009 ER PT J AU Lamouroux, J Tran, H Laraia, AL Gamache, RR Rothman, LS Gordon, IE Hartmann, JM AF Lamouroux, J. Tran, H. Laraia, A. L. Gamache, R. R. Rothman, L. S. Gordon, I. E. Hartmann, J. -M. TI Updated database plus software for line-mixing in CO2 infrared spectra and their test using laboratory spectra in the 1.5-2.3 mu m region SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE CO2; Line mixing; Infrared spectra; Remote sensing ID MOLECULAR SPECTROSCOPIC DATABASE; ATMOSPHERIC CO2; WING REGIONS; Q BRANCHES; BANDS; MODEL; TEMPERATURE; COMPUTATION; ISOTOPOMERS; INTENSITIES AB In a previous series of papers, a model for the calculation of CO2-air absorption coefficients taking line-mixing into account and the corresponding database/software package were described and widely tested. In this study, we present an update of this package, based on the 2008 version of HITRAN, the latest currently available. The spectroscopic data for the seven most-abundant isotopologues are taken from HITRAN. When the HITRAN data are not complete up to J ''=70, the data files are augmented with spectroscopic parameters from the CD5D-296 database and the high-temperature CDSD-1000 if necessary. Previously missing spectroscopic parameters, the air-induced pressure shifts and CO2 line broadening coefficients with H2O, have been added. The quality of this new database is demonstrated by comparisons of calculated absorptions and measurements using CO2 high-pressure laboratory spectra in the 1.5-2.3 mu m region. The influence of the imperfections and inaccuracies of the spectroscopic parameters from the 2000 version of HITRAN is clearly shown as a big improvement of the residuals is observed by using the new database. The very good agreements between calculated and measured absorption coefficients confirm the necessity of the update presented here and further demonstrate the importance of line-mixing effects, especially for the high pressures investigated here. The application of the updated database/software package to atmospheric spectra should result in an increased accuracy in the retrieval of CO2 atmospheric amounts. This opens improved perspectives for the space-borne detection of carbon dioxide sources and sinks. (C) 2010 Elsevier Ltd. All rights reserved. C1 [Lamouroux, J.; Laraia, A. L.; Gamache, R. R.] Univ Massachusetts, Sch Marine Sci, Dept Environm Earth & Atmospher Sci, Lowell, MA 01854 USA. [Tran, H.; Hartmann, J. -M.] Univ Paris 12, CNRS, UMR 7583, LISA, F-94010 Creteil, France. [Tran, H.; Hartmann, J. -M.] Univ Paris 07, CNRS, UMR 7583, LISA, F-94010 Creteil, France. [Rothman, L. S.; Gordon, I. E.] Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. RP Hartmann, JM (reprint author), Univ Massachusetts, Sch Marine Sci, Dept Environm Earth & Atmospher Sci, 1 Univ Ave, Lowell, MA 01854 USA. EM hartmann@lisa.univ-paris12.fr RI Tran, Ha/I-5076-2013 FU National Science Foundation [ATM-0803135]; Centre National d'Etudes Spatiales FX J. Lamouroux, A.L. Laraia, and R.R. Gamache are pleased to acknowledge support of this research by the National Science Foundation through Grant no. ATM-0803135. Any opinions, findings, and conclusions or recommendations expressed in this material are those of the author(s) and do not necessarily reflect the views of the National Science Foundation. The authors from LISA acknowledge support by the TOSCA program of the Centre National d'Etudes Spatiales. NR 27 TC 54 Z9 59 U1 0 U2 23 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 OCT PY 2010 VL 111 IS 15 SI SI BP 2321 EP 2331 DI 10.1016/j.jqsrt.2010.03.006 PG 11 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 643CE UT WOS:000281269800018 ER PT J AU Hazari, Z Sonnert, G Sadler, PM Shanahan, MC AF Hazari, Zahra Sonnert, Gerhard Sadler, Philip M. Shanahan, Marie-Claire TI Connecting High School Physics Experiences, Outcome Expectations, Physics Identity, and Physics Career Choice: A Gender Study SO JOURNAL OF RESEARCH IN SCIENCE TEACHING LA English DT Article DE gender; females; physics education; identity; survey; career choice; pedagogy ID SELF-CONCEPT; COLLEGE-STUDENTS; EDUCATIONAL EXPECTATIONS; UNIVERSITY PHYSICS; SCIENCE CLASSROOMS; ACHIEVEMENT; GIRLS; PERFORMANCE; INTERESTS; MATH AB This study explores how students' physics identities are shaped by their experiences in high school physics classes and by their career outcome expectations. The theoretical framework focuses on physics identity and includes the dimensions of student performance, competence, recognition by others, and interest. Drawing data from the Persistence Research in Science and Engineering (PRiSE) project, which surveyed college English students nationally about their backgrounds, high school science experiences, and science attitudes, the study uses multiple regression to examine the responses of 3,829 students from 34 randomly selected US colleges/universities. Confirming the salience of the identity dimension for young persons' occupational plans, the measure for students' physics identity used in this study was found to strongly predict their intended choice of a physics career. Physics identity, in turn, was found to correlate positively with a desire for an intrinsically fulfilling career and negatively with a desire for personal/family time and opportunities to work with others. Physics identity was also positively predicted by several high school physics characteristics/experiences such as a focus on conceptual understanding, real-world/contextual connections, students answering questions or making comments, students teaching classmates, and having an encouraging teacher. Even though equally beneficial for both genders, females reported experiencing a conceptual focus and real-world/contextual connections less frequently. The explicit discussion of under-representation of women in science was positively related to physics identity for female students but had no impact for male students. Surprisingly, several experiences that were hypothesized to be important for females' physics identity were found to be non-significant including having female scientist guest speakers, discussion of women scientists' work, and the frequency of group work. This study exemplifies a useful theoretical framework based on identity, which can be employed to further examine persistence in science, and illustrates possible avenues for change in high school physics teaching. (C) 2010 Wiley Periodicals, Inc. J Res Sci Teach 47: 978-1003, 2010 C1 [Hazari, Zahra] Clemson Univ, Dept Engn & Sci Educ, Clemson, SC USA. [Hazari, Zahra] Clemson Univ, Dept Math Sci, Clemson, SC USA. [Sonnert, Gerhard; Sadler, Philip M.] Harvard Smithsonian Ctr Astrophys, Sci Educ Dept, Cambridge, MA 02138 USA. [Shanahan, Marie-Claire] Univ Alberta, Dept Elementary Educ, Edmonton, AB, Canada. RP Hazari, Z (reprint author), Clemson Univ, Dept Engn & Sci Educ, Clemson, SC USA. EM zahra@clemson.edu NR 117 TC 112 Z9 112 U1 13 U2 80 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0022-4308 EI 1098-2736 J9 J RES SCI TEACH JI J. Res. Sci. Teach. PD OCT PY 2010 VL 47 IS 8 BP 978 EP 1003 DI 10.1002/tea.20363 PG 26 WC Education & Educational Research SC Education & Educational Research GA 662FX UT WOS:000282793900004 ER PT J AU Cardona, A Valencia, V Garzon, A Montes, C Ojeda, G Ruiz, J Weber, M AF Cardona, A. Valencia, V. Garzon, A. Montes, C. Ojeda, G. Ruiz, J. Weber, M. TI Permian to Triassic I to S-type magmatic switch in the northeast Sierra Nevada de Santa Marta and adjacent regions, Colombian Caribbean: Tectonic setting and implications within Pangea paleogeography SO JOURNAL OF SOUTH AMERICAN EARTH SCIENCES LA English DT Article DE Pangea; Subduction; Accretion; Geochemistry; U-Pb geochronology ID U-PB ZIRCON; GEOLOGIC EVOLUTION; PALEOZOIC ROCKS; SOUTHERN MEXICO; GRANITIC-ROCKS; ANDES; RECONSTRUCTION; GEOCHRONOLOGY; VENEZUELA; GNEISSES AB The Late Paleozoic to Triassic tectonics of northwestern South America have major implications for the understanding of Laurentia-Gondwana interactions that formed Pangea, and the origin of several tectonostratigraphic terranes dispersed by the break-up of this supercontinent during the formation of the Caribbean. Two mylonitic and orthogneissic granitoid suites have been recognized in the northeastern segment of the Sierra Nevada de Santa Marta, the lower Magdalena basin and the Guajira Serranias, within the Caribbean region of Colombia. For the Santa Marta region U/Pb LAM-ICP-MS analysis yielded zircon crystallization ages of 288.1 +/- 4.5 Ma, 276.5 +/- 5,1 Ma and 264.9 +/- 4.0 Ma, related to the magmatic intrusion. Geochemical and modal variations show a compositional spectrum between diorite and granite, whereas LREE enrichment, Ti and Nb anomalies and geochemical discrimination suggest that this granitoid suite was formed within a magmatic arc setting. Inherited zircons suggest that this Early Permian plutonism was formed with the participation of Neoproterozoic and Grenvillian basement proximal to the South American continent. Evidence of a superimposed Early Triassic (ca. 250 Ma) deformational event in Santa Marta, together with a well defined S-type magmatism in the basement rocks from the adjacent lower Magdalena Valley and Guajira Peninsula regions are related to a major shift in the regional tectonic evolution. It's envisioned that this event records either terrane accretion or strong plate coupling during the final stages of Pangea agglutination. Connections with the main Alleghanian-Ouachitan Pangean orogen are precluded due to their timing differences. The plutons temporally and compositionally correlate with an arc found in the northern Andes and Mexican Gondwana terranes, and represent a broader magmatic event formed at the proto-Pacific margin, outside the nucleus of the Laurentia-Gondwana Alleghanian-Oachitan orogens. Evidence of lower temperature recrystallization is probably linked to a younger Late Cretaceous deformational event that reworked the margin during the accretion of the Caribbean arc to the northwest of South America. (C) 2010 Elsevier Ltd. All rights reserved. C1 [Cardona, A.; Montes, C.] Smithsonian Trop Res Inst, Ancon, Panama. [Cardona, A.; Ojeda, G.] Ecopetrol, Inst Colombiano Petr, Piedecuesta, Colombia. [Valencia, V.; Ruiz, J.] Univ Arizona, Dept Geosci, Tucson, AZ 85721 USA. [Garzon, A.] Univ Nacl Colombia, Dept Geociencias, Bogota, Colombia. [Weber, M.] Univ Nacl Colombia, Escuela Geociencias & Medio Ambiente, Medellin, Colombia. RP Cardona, A (reprint author), Smithsonian Trop Res Inst, Ancon, Panama. EM CardonaA@si.edu OI Montes, Camilo/0000-0002-3553-0787 FU ECOPETROL-ICP; INGEOMINAS; INVEMAR; Evolucion Geohistorica de la Sierra Nevada de Santa Marta; Fundacion para el Apoyo de la Investigacion y la Cultura del Banco de la Republica de Colombia [2289]; NSF [EAR-0443387]; International Geological Correlation Program, "Subduction zones of the Caribbean" FX ECOPETROL-ICP, INGEOMINAS and INVEMAR and the Project "Evolucion Geohistorica de la Sierra Nevada de Santa Marta" are acknowledged for their support. Field discussions with F. Colmenares, G. Guzman, and the GEOSEARCH LTDA Sierra Nevada team are fully appreciated. V. Arboleda is acknowledged for help during sampling of the granitoid cores. Discussions with C. Vinasco and M. Ibanez are highly appreciated. J. Duque, M. E. Velazquez and C. A. Salazar are acknowledged for helping with sample preparation. Key suggestions of two anonymous reviewers are highly appreciated. Analytical work was partially supported by a research grant from the Fundacion para el Apoyo de la Investigacion y la Cultura del Banco de la Republica de Colombia, Project 2289. A. Garcia-Casco is kindly acknowledged for access to microprobe analyses. Funding for the Arizona LaserChron Center is provided by NSF EAR-0443387. This is a contribution to Project 546 of the International Geological Correlation Program, "Subduction zones of the Caribbean". NR 72 TC 20 Z9 22 U1 0 U2 8 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0895-9811 J9 J S AM EARTH SCI JI J. South Am. Earth Sci. PD OCT PY 2010 VL 29 IS 4 SI SI BP 772 EP 783 DI 10.1016/j.jsames.2009.12.005 PG 12 WC Geosciences, Multidisciplinary SC Geology GA 691ZC UT WOS:000285120300003 ER PT J AU Cardona, A Valencia, V Bustamante, C Garcia-Casco, A Ojeda, G Ruiz, J Saldarriaga, M Weber, M AF Cardona, A. Valencia, V. Bustamante, C. Garcia-Casco, A. Ojeda, G. Ruiz, J. Saldarriaga, M. Weber, M. TI Tectonomagmatic setting and provenance of the Santa Marta Schists, northern Colombia: Insights on the growth and approach of Cretaceous Caribbean oceanic terranes to the South American continent SO JOURNAL OF SOUTH AMERICAN EARTH SCIENCES LA English DT Article DE Cretaceous; Caribbean plate; Provenance; Back-arc; U/Pb LAM-ICP-MS; Isotopes; Geochemistry; Colombia ID TRACE-ELEMENT GEOCHEMISTRY; U-PB AGES; CRUSTAL EVOLUTION; BASIN DEVELOPMENT; WESTERN COLOMBIA; TECTONIC HISTORY; VENEZUELA; PLATE; ANDES; CONSTRAINTS AB Metamorphosed volcano-sedimentary rocks accreted to the northern South American continental margin are major vestiges of the Caribbean oceanic plate evolution and its interactions with the continent. Selected whole rock geochemistry, Nd-Sr isotopes and detrital zircon geochronology were obtained in metabasic and metasedimentary rocks from the Santa Marta and San Lorenzo Schists in northernmost Colombia. Trace element patterns are characterized by primitive island arc and MORB signatures. Similarly initial Sr-87/Sr-86-epsilon(Nd) isotopic relations correlate with oceanic arcs and MORB reservoirs, suggesting that the protoliths were formed within a back-arc setting or at the transition between the inta-oceanic arc and the Caribbean oceanic crust. Trace element trends from associated metasedimentary rocks show that the provenance was controlled by a volcanic arc and a sialic continental domain, whereas detrital U/Pb zircons from the Santa Marta Schists and adjacent southeastern metamorphic units show Late Cretaceous and older Mesozoic, Late Paleozoic and Mesoproterozoic sources. Comparison with continental inland basins suggests that this arc-basin is allocthonous to its current position, and was still active by ca. 82 Ma. The geological features are comparable to other arc remnants found in northeastern Colombia and the Netherland Antilles. The geochemical and U/Pb detrital signatures from the metasedimentary rocks suggest that this tectonic domain was already in proximity to the continental margin, in a configuration similar to the modern Antilles or the Kermadec arc in the Pacific. The older continental detritus were derived from the ongoing Andean uplift feeding the intra-oceanic tectonic environment. Cross-cutting relations with granitoids and metamorphic ages suggest that metamorphism was completed by ca. 65 Ma. (C) 2009 Elsevier Ltd. All rights reserved. C1 [Cardona, A.] Smithsonian Trop Res Inst, Ancon, Panama. [Cardona, A.; Ojeda, G.] Inst Colombiano Petr, Piedecuesta, Colombia. [Valencia, V.; Ruiz, J.] Univ Arizona, Dept Geosci, Tucson, AZ 85721 USA. [Bustamante, C.; Saldarriaga, M.] Univ EAFIT, Dept Geol, Medellin, Colombia. [Garcia-Casco, A.] Univ Granada, Dept Mineral & Petrol, E-18071 Granada, Spain. [Weber, M.] Univ Nacl Colombia, Escuela Geociencias & Medio Ambiente, Medellin, Colombia. RP Cardona, A (reprint author), Smithsonian Trop Res Inst, Ancon, Panama. EM CardonaA@si.edu RI Garcia-Casco, Antonio/K-8295-2013; Bustamante, Camilo/N-6273-2015 OI Garcia-Casco, Antonio/0000-0002-8814-402X; Bustamante, Camilo/0000-0002-5527-598X FU ECOPETROL; INVEMAR; INGEOMINAS; Fundacion para el Apoyo de la Investigacion y la Cultura del Banco de la Republica de Colombia [2289]; NSF [EAR-0443387] FX ECOPETROL, INVEMAR and INGEOMINAS are acknowledged for providing support during several phases of this research. Discussions and support from G. Guzman, F. Colmenares and the Geo-search Ltda Sierra Nevada team are highly appreciated. Comments by two anonymous reviewer are highly appreciated Analytical work received support from the Fundacion para el Apoyo de la Investigacion y la Cultura del Banco de la Republica de Colombia, project 2289. Funding for the Arizona LaserChron Center is provided by NSF EAR-0443387. This is a contribution to the IGCP 546: "Subduction zones of the Caribbean." NR 101 TC 15 Z9 16 U1 0 U2 4 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0895-9811 J9 J S AM EARTH SCI JI J. South Am. Earth Sci. PD OCT PY 2010 VL 29 IS 4 SI SI BP 784 EP 804 DI 10.1016/j.jsames.2009.08.012 PG 21 WC Geosciences, Multidisciplinary SC Geology GA 691ZC UT WOS:000285120300004 ER PT J AU Weber, M Cardona, A Valencia, V Garcia-Casco, A Tobon, M Zapata, S AF Weber, M. Cardona, A. Valencia, V. Garcia-Casco, A. Tobon, M. Zapata, S. TI U/Pb detrital zircon provenance from late cretaceous metamorphic units of the Guajira Peninsula, Colombia: Tectonic implications on the collision between the Caribbean arc and the South American margin SO JOURNAL OF SOUTH AMERICAN EARTH SCIENCES LA English DT Article DE U-Pb detrital zircon provenance analysis; Caribbean arc; South American margin; Arc-continent collision; Guajira Peninsula ID P-T PATHS; EXHUMATION PROCESSES; BASIN DEVELOPMENT; EVOLUTION; PLATE; VENEZUELA; GEOCHRONOLOGY; CONSTRAINTS; SUBDUCTION; ANDES AB Mesozoic metamorphic units exposed along the northern margin of the South American plate record the different stages of subduction evolution or arc-continent collision between the margins of the Caribbean plate and the South American continent. U-Pb detrital zircon geochronology for provenance analysis was carried out on meta-sedimentary rocks of the Etpana formation and metamorphic boulders found within a nearby Tertiary conglomerate, including high-pressure rocks in the Colombian Caribbean. All samples have similar age populations, suggesting that they share a relatively common source and paleogeography. Prominent age peaks include Meso and Paleoproterozoic ages of ca. 1624 Ma and 1315 Ma, Cambrian to Neoproterozoic ages of ca. 630 Ma, 580 Ma and 547 Ma, and less abundant Jurassic and Permian ages of ca. 270 Ma and 160 Ma, which indicate that the South American margin is a major source for the sedimentary protoliths. There are also remnants of younger Cretaceous allocthonous Caribbean arc input at ca. 90-70 Ma. The deposition and metamorphism of these units records the ongoing Late Cretaceous continental subduction of the South American margin within the Caribbean intra-oceanic arc-subduction zone. This gave way to an arc-continent collision between the Caribbean and the South American plates, and sediments with continental signatures were incorporated into the subduction channel and the accretionary wedge. As convergence continued, sediments derived from a mix of South American and arc sources were deposited and included in the collisional wedge up until <71 Ma. (C) 2009 Elsevier Ltd. All rights reserved. C1 [Weber, M.; Tobon, M.; Zapata, S.] Univ Nacl Colombia, Medellin, Colombia. [Cardona, A.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Valencia, V.] Univ Arizona, Dept Geosci, Tucson, AZ 85721 USA. [Garcia-Casco, A.] Univ Granada, Dept Geosci, E-18071 Granada, Spain. RP Weber, M (reprint author), Univ Nacl Colombia, Medellin, Colombia. EM mweber@unal.edu.co RI Garcia-Casco, Antonio/K-8295-2013 OI Garcia-Casco, Antonio/0000-0002-8814-402X FU Universidad Nacional de Colombia through DIME [30805975]; Direccion Academica in Medellin; National Science Foundation [EAR-0443387]; Subduction zones of the Caribbean FX Oscar Talavera is acknowledged for discussions and encouragement during field work. Mauricio Ibanez is sincerely acknowledged for its hospitality and continuous help during analytical work at Tucson. The hospitality and help of the LASERCHRON staff is also sincerely acknowledged. Continuous help from Oscar Jaramillo at the Petrography Laboratory, Universidad Nacional de Colombia is greatly appreciated. This research was supported by the Universidad Nacional de Colombia through DIME Grant 30805975 and Direccion Academica in Medellin. Funding for the Arizona Laser-Chron Center is provided by National Science Foundation Grant EAR-0443387. This is a contribution to Project 546 of the International Geological Correlation Program "subduction zones of the Caribbean". NR 81 TC 14 Z9 15 U1 0 U2 4 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0895-9811 J9 J S AM EARTH SCI JI J. South Am. Earth Sci. PD OCT PY 2010 VL 29 IS 4 SI SI BP 805 EP 816 DI 10.1016/j.jsames.2009.10.004 PG 12 WC Geosciences, Multidisciplinary SC Geology GA 691ZC UT WOS:000285120300005 ER PT J AU Bayona, G Jimenez, G Silva, C Cardona, A Montes, C Roncancio, J Cordani, U AF Bayona, German Jimenez, Giovanny Silva, Cesar Cardona, Agustin Montes, Camilo Roncancio, Jairo Cordani, Umberto TI Paleomagnetic data and K-Ar ages from Mesozoic units of the Santa Marta massif: A preliminary interpretation for block rotation and translations SO JOURNAL OF SOUTH AMERICAN EARTH SCIENCES LA English DT Article DE Santa Marta massif; Vertical-axis rotation; Terrane translation; Caribbean tectonics; Jurassic paleogeography ID NORTHWESTERN SOUTH-AMERICA; COLOMBIAN ANDES; EASTERN CORDILLERA; TECTONIC HISTORY; JURASSIC ROCKS; GEOCHRONOLOGY; NORTHERN; BASIN; VENEZUELA; MODELS AB We report 6 K-Ar ages and paleomagnetic data from 28 sites collected in Jurassic, Lower Cretaceous and Paleocene rocks of the Santa Marta massif, to test previous hypothesis of rotations and translations of this massif, whose rock assemblage differs from other basement-cored ranges adjacent to the Guyana margin. Three magnetic components were identified in this study. A first component has a direction parallel to the present magnetic field and was uncovered in all units (D 352, I = 25.6, k = 57.35, a95 = 5.3, N = 12). A second component was isolated in Cretaceous limestone and Jurassic volcaniclastic rocks (D = 8.8, I = 8.3, k = 24.71, a95 = 13.7, N = 6), and it was interpreted as of Early Cretaceous age. In Jurassic sites with this component, Early Cretaceous K-Ar ages obtained from this and previous studies are interpreted as reset ages. The third component was uncovered in eight sites of Jurassic volcaniclastic rocks, and its direction indicates negative shallow to moderate inclinations and northeastward declinations. K-Ar ages in these sites are of Early (196.5 +/- 4.9 Ma) to early Late Jurassic age (156.6 +/- 8.9 Ma). Due to local structural complexity and too few Cretaceous outcrops to perform a reliable unconformity test, we only used two sites with (1) K-Ar ages, (2) less structural complexity, and (3) reliable structural data for Jurassic and Cretaceous rocks. The mean direction of the Jurassic component is (D = 20.4, I = -18.2, k = 46.9, a95 = 5.1, n = 18 specimens from two sites). These paleomagnetic data support previous models of northward along-margin translations of Grenvillian-cored massifs. Additionally, clockwise vertical-axis rotation of this massif, with respect to the stable craton, is also documented; the sense of rotation is similar to that proposed for the Perija Range and other ranges of the southern Caribbean margin. More data is needed to confirm the magnitudes of rotations and translations. (C) 2009 Elsevier Ltd. All rights reserved. C1 [Bayona, German; Jimenez, Giovanny; Silva, Cesar; Cardona, Agustin; Montes, Camilo] Corp Geol ARES, Bogota, Colombia. [Bayona, German; Silva, Cesar; Cardona, Agustin; Montes, Camilo] Smithsonian Trop Res Inst, Ancon, Panama. [Roncancio, Jairo] Geosearch Ltda, Bogota, Colombia. [Cordani, Umberto] Univ Sao Paulo, Dept Geosci, Sao Paulo, Brazil. RP Bayona, G (reprint author), Corp Geol ARES, Calle 57 24-11 202, Bogota, Colombia. EM gbayona@cgares.org RI Cordani, Umberto/F-3686-2014; OI Cordani, Umberto/0000-0003-4425-5905; Montes, Camilo/0000-0002-3553-0787 FU Ingeominas, Instituto Colombiano del Petroleo and Invemar FX This research was funded by Ingeominas, Instituto Colombiano del Petroleo and Invemar. We acknowledge Ricardo Trindade and Danielle Brant (University of Sao Paulo), and James Channell and Kainian Huang (University of Florida) for assistance and discussion of paleomagnetic data during our work in the Paleomagnetic Laboratories. The field geologist group of Geosearch Ltda contributed to the location of sites during the 2006-2007 field seasons. Johana Casas helped for access to the construction and tunnel of the Rancheria Dam, and Ivan Gutierrez helped in the collection of the samples. We thanks to Georgina Guzman (Invemar) for allowing us the publication of segments of the geologic map of the Sierra Nevada de Santa Marta (Invemar-Ingeominas-Ecopetrol - ICP-Geosearch Ltda, 2007). Comments and suggestions from Roberto Moliza Garza, Victoria Mejia and an anonymous reviewer contributed to improve the presentation of data and content of the manuscript. NR 67 TC 14 Z9 16 U1 0 U2 5 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0895-9811 J9 J S AM EARTH SCI JI J. South Am. Earth Sci. PD OCT PY 2010 VL 29 IS 4 SI SI BP 817 EP 831 DI 10.1016/j.jsames.2009.10.005 PG 15 WC Geosciences, Multidisciplinary SC Geology GA 691ZC UT WOS:000285120300006 ER PT J AU Montes, C Guzman, G Bayona, G Cardona, A Valencia, V Jaramillo, C AF Montes, Camilo Guzman, Georgina Bayona, German Cardona, Agustin Valencia, Victor Jaramillo, Carlos TI Clockwise rotation of the Santa Marta massif and simultaneous Paleogene to Neogene deformation of the Plato-San Jorge and Cesar-Rancheria basins SO JOURNAL OF SOUTH AMERICAN EARTH SCIENCES LA English DT Article DE Tectonics; Rotation; Northern Colombia; Santa Marta; Cerrejon; Perija; Plato; San Jorge; Paleomagnetism; Geochronology ID NORTHERN COLOMBIA; SOUTH-AMERICA; TECTONIC SIGNIFICANCE; VENEZUELA; ANDES; EVOLUTION; PERIJA; GNEISSES; SIERRA AB A moderate amount of vertical-axis clockwise rotation of the Santa Marta massif (30 degrees) explains as much as 115 km of extension (stretching of 1.75) along its trailing edge (Plato-San Jorge basin) and up to 56 km of simultaneous shortening with an angular shear of 0.57 along its leading edge (Perija range). Extensional deformation is recorded in the 260 km-wide, fan-shaped Plato-San Jorge basin by a 2-8 km thick, shallowing-upward and almost entirely fine-grained, upper Eocene and younger sedimentary sequence. The simultaneous initiation of shortening in the Cesar-Rancheria basin is documented by Mesozoic strata placed on to lower Eocene syntectonic strata (Tabaco Formation and equivalents) along the northwest-verging, shallow dipping (9-12 degrees to the southeast) and discrete Cerrejon thrust. First-order subsidence analysis in the Plato-San Jorge basin is consistent with crustal stretching values between 1.5 and 2, also predicted by the rigid-body rotation of the Santa Marta massif. The model predicts about 100 km of right-lateral displacement along the Oca fault and 45 km of left-lateral displacement along the Santa Marta-Bucaramanga fault. Clockwise rotation of a rigid Santa Marta massif, and simultaneous Paleogene opening of the Plato-San Jorge basin and emplacement of the Cerrejon thrust sheet would have resulted in the fragmentation of the Cordillera Central-Santa Marta massif province. New U/Pb ages (241 +/- 3 Ma) on granitoid rocks from industry boreholes in the Plato-San Jorge basin confirm the presence of fragments of a now segmented, Late Permian to Early Triassic age, two-mica, granitic province that once spanned the Santa Marta massif to the northernmost Cordillera Central. (C) 2009 Elsevier Ltd. All rights reserved. C1 [Montes, Camilo; Cardona, Agustin; Jaramillo, Carlos] Smithsonian Trop Res Inst, Unit 9100, Dpo, AA 34002 USA. [Guzman, Georgina] Invemar, Cerro Punta Betin, Santa Marta 1016, Colombia. [Bayona, German] Corp Geol Ares, Bogota, Colombia. [Valencia, Victor] Univ Arizona, Arizona Lasechron Ctr, Tucson, AZ USA. RP Montes, C (reprint author), Smithsonian Trop Res Inst, Unit 9100, Box 0948, Dpo, AA 34002 USA. EM montesc@si.edu OI Montes, Camilo/0000-0002-3553-0787 FU Banco de la Republica de Colombia [2289]; NSF [EAR-0443387] FX Banco de la Republica de Colombia partially funded analytical data, Project 2289. Funding for the Arizona LaserChron Center is provided by NSF EAR-0443387. This is a contribution to the IGCP 546: "Subduction zones of the Caribbean". Carbones del Cerrejon Ltd., provided support to students mapping the northern part of the Cesar-Rancheria valley. Thanks to I. Gutierrez for help in field expeditions, to G. Ojeda and C. Vargas for core sampling at the Litoteca Nacional and to N. Hoyos for help in the reconstructions. Backstrip OSX, and Gplates were used in this paper. Comprehensive reviews by F. Roure and an anonymous reviewer helped improve the quality of the manuscript, the authors, however, remain responsible for all errors of fact and interpretation. NR 72 TC 30 Z9 35 U1 0 U2 11 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0895-9811 J9 J S AM EARTH SCI JI J. South Am. Earth Sci. PD OCT PY 2010 VL 29 IS 4 SI SI BP 832 EP 848 DI 10.1016/j.jsames.2009.07.010 PG 17 WC Geosciences, Multidisciplinary SC Geology GA 691ZC UT WOS:000285120300007 ER PT J AU Johnson, KP Clayton, DH Dumbacher, JP Fleischer, RC AF Johnson, Kevin P. Clayton, Dale H. Dumbacher, John P. Fleischer, Robert C. TI The flight of the Passenger Pigeon: Phylogenetics and biogeographic history of an extinct species SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Ectopistes migratorius; Molecular systematics; Ancient DNA; Columbiformes; Doves ID COLUMBICOLA PHTHIRAPTERA; MITOCHONDRIAL; COLUMBIFORMES; NUCLEAR; GENUS; PHILOPTERIDAE; RADIATION; SEQUENCES; BIRDS; AVES AB The human-caused extinction of the Passenger Pigeon (Ectopistes migratorius) is one of the best known and documented of any bird. This event was particularly alarming because the Passenger Pigeon went from being one of the most numerous avian species in the world to extinct in a period of decades, when the last individual died in captivity in a Cincinnati Zoo in 1914. While a great deal of information exists on the likely direct and indirect causes of its demise, as well as information on life-history, the phylogenetic relationships of this species have been subject to considerable speculation. Here we use DNA sequences obtained from museum specimens to resolve the phylogenetic position of this species with respect to other pigeons and doves (Columbiformes). We show that the Passenger Pigeon is not related to the New World mourning doves (Zenaida) as many authors have suggested, but is the sister taxon of all other New World pigeons (Patagioenas). Biogeographic analysis suggests the Passenger Pigeon lineage may have colonized North America from Asia, and subsequently dispersed into South America, leading to a more extensive radiation of New World pigeons. (C) 2010 Published by Elsevier Inc. C1 [Johnson, Kevin P.] Univ Illinois, Illinois Nat Hist Survey, Champaign, IL 61820 USA. [Clayton, Dale H.] Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. [Dumbacher, John P.] Calif Acad Sci, San Francisco, CA 94103 USA. [Dumbacher, John P.; Fleischer, Robert C.] Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, Washington, DC 20008 USA. RP Johnson, KP (reprint author), Univ Illinois, Illinois Nat Hist Survey, 1816 S Oak St, Champaign, IL 61820 USA. EM kjohnson@inhs.uiuc.edu FU National Science Foundation [DEB-0107891, DEB-0612938, DEB-0816877] FX The authors thank the Field Museum of Natural History, US National Museum of Natural History, and University of Kansas Museum of Natural History for providing samples of Passenger Pigeon skins. This work was supported by National Science Foundation Grants DEB-0107891 and DEB-0612938 to K.P.J. and DEB-0816877 to D.H.C. NR 21 TC 11 Z9 13 U1 3 U2 60 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1055-7903 J9 MOL PHYLOGENET EVOL JI Mol. Phylogenet. Evol. PD OCT PY 2010 VL 57 IS 1 BP 455 EP 458 DI 10.1016/j.ympev.2010.05.010 PG 4 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 652GY UT WOS:000281992900039 PM 20478386 ER PT J AU Million, ET Werner, N Simionescu, A Allen, SW Nulsen, PEJ Fabian, AC Bohringer, H Sanders, JS AF Million, E. T. Werner, N. Simionescu, A. Allen, S. W. Nulsen, P. E. J. Fabian, A. C. Boehringer, H. Sanders, J. S. TI Feedback under the microscope - I. Thermodynamic structure and AGN-driven shocks in M87 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: individual: M87; intergalactic medium; X-rays: galaxies: clusters ID X-RAY SPECTROSCOPY; ANISOTROPIC THERMAL CONDUCTION; DEEP CHANDRA OBSERVATION; ACTIVE GALACTIC NUCLEI; XMM-NEWTON OBSERVATION; INTRACLUSTER MEDIUM; GALAXY CLUSTERS; SOUND-WAVES; GASEOUS ATMOSPHERE; PERSEUS CLUSTER AB We present the first in a series of papers discussing the thermodynamic properties of M87 and the central regions of the Virgo Cluster in unprecedented detail. Using a deep Chandra exposure (574 ks), we present high-resolution thermodynamic maps created from the spectra of similar to 16 000 independent regions, each with similar to 1000 net counts. The excellent spatial resolution of the thermodynamic maps reveals the dramatic and complex temperature, pressure, entropy and metallicity structure of the system. The 'X-ray arms', driven outwards from M87 by the central active galactic nuclei (AGN), are prominent in the brightness, temperature and entropy maps. Excluding the 'X-ray arms', the diffuse cluster gas at a given radius is strikingly isothermal. This suggests either that the ambient cluster gas, beyond the arms, remains relatively undisturbed by AGN uplift or that conduction in the intracluster medium (ICM) is efficient along azimuthal directions, as expected under action of the heat-flux-driven buoyancy instability (HBI). We confirm the presence of a thick (similar to 40 arcsec or similar to 3 kpc) ring of high-pressure gas at a radius of similar to 180 arcsec (similar to 14 kpc) from the central AGN. We verify that this feature is associated with a classical shock front, with an average Mach number M = 1.25. Another, younger shock-like feature is observed at a radius of similar to 40 arcsec (similar to 3 kpc) surrounding the central AGN, with an estimated Mach number M greater than or similar to 1.2. As shown previously, if repeated shocks occur every similar to 10 Myr, as suggested by these observations, then AGN-driven weak shocks could produce enough energy to offset radiative cooling of the ICM. A high significance enhancement of Fe abundance is observed at radii 350-400 arcsec (27-31 kpc). This ridge is likely formed in the wake of the rising bubbles filled with radio-emitting plasma that drag cool, metal-rich gas out of the central galaxy. We estimate that at least similar to 1.0 x 106 solar masses of Fe has been lifted and deposited at a radius of 350-400 arcsec; approximately the same mass of Fe is measured in the X-ray bright arms, suggesting that a single generation of buoyant radio bubbles may be responsible for the observed Fe excess at 350-400 arcsec. C1 [Million, E. T.; Werner, N.; Simionescu, A.; Allen, S. W.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Million, E. T.; Werner, N.; Simionescu, A.; Allen, S. W.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Nulsen, P. E. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fabian, A. C.; Sanders, J. S.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Boehringer, H.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. RP Million, ET (reprint author), Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, 382 Via Pueblo Mall, Stanford, CA 94305 USA. EM emillion@stanford.edu OI Sanders, Jeremy/0000-0003-2189-4501; Nulsen, Paul/0000-0003-0297-4493 FU National Aeronautics and Space Administration [PF8-90056, PF9-00070, NAS8-03060]; US Department of Energy [DE-AC02-76SF00515] FX We thank W. R. Forman, C. Jones and E. Churazov for helpful comments and R. G. Morris for computational support. NW and AS were supported by the National Aeronautics and Space Administration through Chandra/Einstein Postdoctoral Fellowship Award Number PF8-90056 and PF9-00070 issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics and Space Administration under contract NAS8-03060. This work was supported in part by the US Department of Energy under contract number DE-AC02-76SF00515. All computational analysis was carried out using the KIPAC XOC compute cluster at Stanford University and the Stanford Linear Accelerator Center (SLAC). NR 57 TC 45 Z9 45 U1 0 U2 1 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT 1 PY 2010 VL 407 IS 4 BP 2046 EP 2062 DI 10.1111/j.1365-2966.2010.17220.x PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 651ST UT WOS:000281948100002 ER PT J AU Werner, N Simionescu, A Million, ET Allen, SW Nulsen, PEJ von der Linden, A Hansen, SM Bohringer, H Churazov, E Fabian, AC Forman, WR Jones, C Sanders, JS Taylor, GB AF Werner, N. Simionescu, A. Million, E. T. Allen, S. W. Nulsen, P. E. J. von der Linden, A. Hansen, S. M. Boehringer, H. Churazov, E. Fabian, A. C. Forman, W. R. Jones, C. Sanders, J. S. Taylor, G. B. TI Feedback under the microscope - II. Heating, gas uplift and mixing in the nearest cluster core SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: individual: M87; intergalactic medium; X-rays: galaxies: clusters ID ACTIVE GALACTIC NUCLEI; X-RAY SPECTROSCOPY; COOLING-FLOW CLUSTERS; H-ALPHA FILAMENTS; XMM-NEWTON; INTRACLUSTER MEDIUM; SOUND-WAVES; GASEOUS ATMOSPHERE; CENTAURUS CLUSTER; ELLIPTIC GALAXIES AB Using a combination of deep (574 ks) Chandra data, XMM-Newton high-resolution spectra and optical H alpha+[N ii] images, we study the nature and spatial distribution of the multi-phase plasma in M87. Our results provide direct observational evidence of 'radio-mode' active galactic nuclei (AGN) feedback in action, stripping the central galaxy of its lowest entropy gas and therefore preventing star formation. This low entropy gas was entrained with and uplifted by the buoyantly rising relativistic plasma, forming long 'arms'. A number of arguments suggest that these arms are oriented within 15 degrees-30 degrees of our line-of-sight. The mass of the uplifted gas in the arms is comparable to the gas mass in the approximately spherically symmetric 3.8 kpc core, demonstrating that the AGN has a profound effect on its immediate surroundings. The coolest X-ray emitting gas in M87 has a temperature of similar to 0.5 keV and is spatially coincident with H alpha+[N ii] nebulae, forming a multi-phase medium where the cooler gas phases are arranged in magnetized filaments. We place strong upper limits of 0.06 M(circle dot) yr-1 (at 95 per cent confidence) on the amount of plasma cooling radiatively from 0.5 to 0.25 keV and show that a uniform, volume-averaged heating mechanism could not be preventing the cool gas from further cooling. All of the bright H alpha filaments in M87 appear in the downstream region of the < 3 Myr old shock front, at smaller radii than similar to 0.6 arcmin. We suggest that shocks induce shearing around the filaments, thereby promoting mixing of the cold gas with the ambient hot intra-cluster medium (ICM) via instabilities. By bringing hot thermal particles into contact with the cool, line-emitting gas, mixing can supply the power and ionizing particles needed to explain the observed optical spectra. Furthermore, mixing of the coolest X-ray emitting plasma with the cold optical line-emitting filamentary gas promotes efficient conduction between the two phases, allowing non-radiative cooling which could explain the lack of X-ray gas with temperatures under 0.5 keV. C1 [Werner, N.; Simionescu, A.; Million, E. T.; Allen, S. W.; von der Linden, A.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Werner, N.; Simionescu, A.; Million, E. T.; Allen, S. W.; von der Linden, A.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Nulsen, P. E. J.; Forman, W. R.; Jones, C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hansen, S. M.] Univ Calif Santa Cruz, Univ Calif Observ, Santa Cruz, CA 95064 USA. [Hansen, S. M.] Univ Calif Santa Cruz, Dept Astron, Santa Cruz, CA 95064 USA. [Boehringer, H.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Churazov, E.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Churazov, E.] Space Res Inst IKI, Moscow 117810, Russia. [Fabian, A. C.; Sanders, J. S.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Taylor, G. B.] Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA. RP Werner, N (reprint author), Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, 382 Via Pueblo Mall, Stanford, CA 94305 USA. EM norbertw@stanford.edu RI Churazov, Eugene/A-7783-2013; OI Sanders, Jeremy/0000-0003-2189-4501; Nulsen, Paul/0000-0003-0297-4493 FU National Aeronautics and Space Administration [PF8-90056, PF9-00070, NAS8-03060]; US Department of Energy [DE-AC02-76SF00515]; National Science Foundation [AST-0902010] FX Support for this work was provided by the National Aeronautics and Space Administration through Chandra/Einstein Postdoctoral Fellowship Award Number PF8-90056 and PF9-00070 issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics and Space Administration under contract NAS8-03060. This work was supported in part by the US Department of Energy under contract number DE-AC02-76SF00515. SMH is supported by the National Science Foundation Postdoctoral Fellowship program under award number AST-0902010. NR 78 TC 48 Z9 48 U1 0 U2 1 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT 1 PY 2010 VL 407 IS 4 BP 2063 EP 2074 DI 10.1111/j.1365-2966.2010.16755.x PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 651ST UT WOS:000281948100003 ER PT J AU Kipping, DM Tinetti, G AF Kipping, David M. Tinetti, Giovanna TI Nightside pollution of exoplanet transit depths SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: analytical; techniques: photometric; occultations; planetary systems; infrared: general ID EXTRASOLAR GIANT PLANETS; TIME-SERIES PHOTOMETRY; HD 189733B; LIGHT-CURVE; TRANSMISSION SPECTRA; MODEL ATMOSPHERES; MU-M; WATER; PARAMETERS; EMISSION AB Out of the known transiting extrasolar planets, the majority are gas giants orbiting their host star at close proximity. Both theoretical and observational studies support the hypothesis that such bodies emit significant amounts of flux relative to the host star, increasing towards infrared wavelengths. For the dayside of the exoplanet, this phenomenon typically permits detectable secondary eclipses at such wavelengths, which may be used to infer atmospheric composition. In this paper, we explore the effects of emission from the nightside of the exoplanet on the primary transit light curve, which is essentially a self-blend. Allowing for nightside emission, an exoplanet's transit depth is no longer exclusively a function of the ratio-of-radii. The nightside of an exoplanet is emitting flux, and the contrast to the star's emission is of the order of similar to 10-3 for hot Jupiters. Consequently, we show that the transit depth in the mid-infrared will be attenuated due to flux contribution from the nightside emission by similar to 10-4. We show how this effect can be compensated for in the case where exoplanet phase curves have been measured, in particular for HD 189733b. For other systems, it may be possible to make a first-order correction by using temperature estimates of the planet. Unless the effect is accounted for, transmission spectra will also be polluted by nightside emission, and we estimate that a Spitzer broad-band spectrum on a bright target is altered at the 1 Sigma level. Using archived Spitzer measurements, we show that the effect respectively increases the 8.0-mu m and 24.0-mu m transit depths by 1 Sigma and 0.5 Sigma per transit for HD 189733b. Consequently, we estimate that this would be similar to 5-10 Sigma effect for near future James Webb Space Telescope observations. C1 [Kipping, David M.; Tinetti, Giovanna] Univ London Univ Coll, Dept Phys & Astron, London WC1E 6BT, England. [Kipping, David M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kipping, DM (reprint author), Univ London Univ Coll, Dept Phys & Astron, Gower St, London WC1E 6BT, England. EM d.kipping@ucl.ac.uk OI Tinetti, Giovanna/0000-0001-6058-6654 FU UCL; Science Technology and Facilities Council (STFC); Harvard-Smithsonian Center for Astrophysics; NASA [NNX08AF23G]; Royal Society FX We thank the anonymous referees for their helpful comments in revising this manuscript. DMK has been supported by UCL, the Science Technology and Facilities Council (STFC) studentships, the Harvard-Smithsonian Center for Astrophysics and NASA grant NNX08AF23G. Special thanks to H. Knutson et al. for kindly providing us with their photometry and I. Ribas for providing limb-darkening coefficients. We would like to thank S. Fossey, M. Swain, J. P. Beaulieu, G. Bakos, G. Vashisht and A. Aylward for their support and discussions in preparing this manuscript. GT is supported by UCL and the Royal Society. NR 48 TC 16 Z9 16 U1 0 U2 2 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT 1 PY 2010 VL 407 IS 4 BP 2589 EP 2598 DI 10.1111/j.1365-2966.2010.17094.x PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 651ST UT WOS:000281948100043 ER PT J AU Fietz, J Klose, SM Kalko, EKV AF Fietz, Joanna Klose, Stefan M. Kalko, Elisabeth K. V. TI Behavioural and physiological consequences of male reproductive trade-offs in edible dormice (Glis glis) SO NATURWISSENSCHAFTEN LA English DT Article DE Oxygen consumption; Social thermoregulation; Reproduction small mammal ID YELLOW-PINE CHIPMUNKS; DAILY TORPOR; MYOXUS-GLIS; PLASMA TESTOSTERONE; THYROXINE CYCLES; BODY-TEMPERATURE; SEXUAL-ACTIVITY; METABOLIC-RATE; TESTES SIZE; DORMOUSE AB Testosterone mediates male reproductive trade-offs in vertebrates including mammals. In male edible dormice (Glis glis), reproductivity linked to high levels of testosterone reduces their ability to express torpor, which may be expected to dramatically increase thermoregulatory costs. Aims of this study were therefore to analyse behavioural and physiological consequences of reproductive activity in male edible dormice under ecologically and evolutionary relevant conditions in the field. As we frequently encountered sleeping groups in the field, we hypothesized that social thermoregulation should be an important measure to reduce energy expenditure especially in sexually active male edible dormice. Our results revealed that the occurrence of sleeping groups was negatively influenced by male body mass but not by reproductive status or ambient temperature. In reproductive as in non-reproductive males, the number of individuals huddling together was negatively influenced by their body mass. Thus in general males with a high body mass were sitting in smaller groups than males with a low body mass. However, in reproductive males group size was further negatively affected by ambient temperature and positively by testes size. Thus breeders formed larger sleeping groups at lower ambient temperatures and males with larger testes were found in larger groups than males with smaller testes. Measurements of oxygen consumption demonstrated that grouping behaviour represents an efficient strategy to reduce energy expenditure in edible dormice as it reduced energy requirements by almost 40%. In summary, results of this field study showcase how sexually active male edible dormice may, through behavioural adjustment, counterbalance high thermoregulatory costs associated with reproductive activity. C1 [Fietz, Joanna; Klose, Stefan M.; Kalko, Elisabeth K. V.] Univ Ulm, Inst Expt Ecol, D-89069 Ulm, Germany. [Fietz, Joanna] Univ Ulm, Inst Neurobiol, D-89069 Ulm, Germany. [Kalko, Elisabeth K. V.] Smithsonian Trop Res Inst, Balboa, Panama. RP Fietz, J (reprint author), Univ Ulm, Inst Expt Ecol, Albert Einstein Allee 11, D-89069 Ulm, Germany. EM joanna.fietz@uni-ulm.de FU German Research Foundation (DFG) [FI 831/3-1, 831/3-2]; German Wildlife Foundation FX T Kager, T Weis-Dootz, S Schauer and J Schmid helped in many ways with this field project. Financial support provided by the Margarete von Wrangell Programme, the German Research Foundation (DFG, FI 831/3-1; 831/3-2), and the German Wildlife Foundation, all to JF, made this study possible. Comments of four anonymous reviewers improved the manuscript. Our experiments were conducted under licence from the nature conservancy and the animal experiment department of the Regierungsprasidium Tubingen. NR 50 TC 8 Z9 8 U1 3 U2 13 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0028-1042 EI 1432-1904 J9 NATURWISSENSCHAFTEN JI Naturwissenschaften PD OCT PY 2010 VL 97 IS 10 BP 883 EP 890 DI 10.1007/s00114-010-0704-9 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 653LY UT WOS:000282094100002 PM 20697882 ER PT J AU Harper, SJM Bates, CR Guzman, HM Mair, JM AF Harper, Sarah J. M. Bates, C. Richard Guzman, Hector M. Mair, James M. TI Acoustic mapping of fish aggregation areas to improve fisheries management in Las Perlas Archipelago, Pacific Panama SO OCEAN & COASTAL MANAGEMENT LA English DT Article ID MARINE PROTECTED AREAS; BENTHIC HABITAT; CORAL-REEFS; POPULATION ASSESSMENT; COMMUNITY STRUCTURE; SIDESCAN SONAR; CLASSIFICATION; ASSEMBLAGES; COMPLEXITY; ABUNDANCE AB The purpose of this study was to investigate characterize and map areas of the seabed of Las Perlas Archipelago (LPA) Republic of Panama using swath-bathymetry acoustic sonar techniques and to assess these methods as tools for feeding information into management zoning policy In 2007 the LPA was granted conservation protection under national legislation However detailed management plans are still pending Seabed mapping plays a fundamental role in identifying areas which should be prioritized within the management framework Visual representation of habitat maps provides an effective medium for involving stakeholders in a co-management arena In this survey acoustically mapped areas of the seabed were ground-truthed using a combination of benthic grab samples drop-down video and diver observations The resulting mapped areas were then incorporated into a Geographic Information System (GIS) for further analysis The output was a physical characterization of the seabed at three locations selected for being areas of high rugosity (habitat complexity) and therefore their potential importance as valuable fish aggregation sites The rocky reefs and rhodolith beds identified in this survey represent particularly important fish aggregation and nursery habitats which should be considered priorities for protection under the management plans This survey demonstrated the use of acoustic techniques to spatially resolve topographic features and physical characteristics of the seabed illustrating their potential value as tools for fisheries management and marine reserve zoning in Las Perlas Archipelago and elsewhere (C) 2010 Elsevier Ltd All rights reserved C1 [Mair, James M.] Heriot Watt Univ, Sch Life Sci, Ctr Marine Biodivers & Biotechnol, Edinburgh EH14 4AS, Midlothian, Scotland. [Bates, C. Richard] Univ St Andrews, Dept Earth Sci, St Andrews KY16 9AL, Fife, Scotland. [Guzman, Hector M.] Smithsonian Trop Res Inst, MRC 0580 08, Panama City 03092, Panama. [Harper, Sarah J. M.] Univ British Columbia, AERL, Fisheries Ctr, Vancouver, BC V5Z 1M9, Canada. RP Mair, JM (reprint author), Heriot Watt Univ, Sch Life Sci, Ctr Marine Biodivers & Biotechnol, John Muir Bldg, Edinburgh EH14 4AS, Midlothian, Scotland. OI Bates, Charles Richard/0000-0001-9147-7151 FU UK government s Department for Environment Food and Rural Affairs (DEFRA); St Andrews University; Heriot-Watt University UK; Smithsonian Tropical Research Institute Panama FX We thank the Government of Panama for providing permits to work and collect in the area The authors would like to thank C Guevara R Scott and the crew of R/V Urraca for assisting during the fieldwork We thank our anonymous reviewer for comments on the manuscript Funding for this study was partially provided by the Darwin Initiative a programme of the UK government s Department for Environment Food and Rural Affairs (DEFRA) St Andrews University and Heriot-Watt University UK and the Smithsonian Tropical Research Institute Panama NR 46 TC 5 Z9 6 U1 5 U2 18 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0964-5691 J9 OCEAN COAST MANAGE JI Ocean Coastal Manage. PD OCT PY 2010 VL 53 IS 10 BP 615 EP 623 DI 10.1016/j.ocecoaman.2010.07.001 PG 9 WC Oceanography; Water Resources SC Oceanography; Water Resources GA 682XZ UT WOS:000284437600002 ER PT J AU Minton, MS Mack, RN AF Minton, Mark S. Mack, Richard N. TI Naturalization of plant populations: the role of cultivation and population size and density SO OECOLOGIA LA English DT Article DE Environmental stochasticity; Field trials; Founder population; Invasion; Propagule pressure ID PROPAGULE PRESSURE; ENVIRONMENTAL STOCHASTICITY; RAINFALL VARIABILITY; UNITED-STATES; BIOLOGY; EXTINCTION; INVASIONS; DYNAMICS; CONSERVATION; GRASSLAND AB Field experimentation is required to assess the effects of environmental stochasticity on small immigrant plant populations-a widely understood but largely unexplored aspect of predicting any species' likelihood of naturalization and potential invasion. Cultivation can mitigate this stochasticity, although the outcome for a population under cultivation nevertheless varies enormously from extinction to persistence. Using factorial experiments, we investigated the effects of population size, density, and cultivation (irrigation) on the fate of founder populations for four alien species with different life history characteristics (Echinochloa frumentacea, Fagopyrum esculentum, Helianthus annuus, and Trifolium incarnatum) in eastern Washington, USA. The fate of founder populations was highly variable within and among the 3 years of experimentation and illustrates the often precarious environment encountered by plant immigrants. Larger founder populations produced more seeds (P < 0.001); the role of founder population size, however, differed among years. Irrigation resulted in higher percent survival (P < 0.001) and correspondingly larger net reproductive rate (R (0); P < 0.001). But the minimum level of irrigation for establishment, R (0) > 1, differed among years and species. Sowing density did not affect the likelihood of establishment for any species. Our results underscore the importance of environmental stochasticity in determining the fate of founder populations and the potential of cultivation and large population size in countering the long odds against naturalization. Any implementation of often proposed post-immigration field trials to assess the risk of an alien species becoming naturalized, a requisite step toward invasion, will need to assess different sizes of founder populations and the extent and character of cultivation (intentional or unintentional) that the immigrants might receive. C1 [Minton, Mark S.; Mack, Richard N.] Washington State Univ, Sch Biol Sci, Pullman, WA 99164 USA. RP Minton, MS (reprint author), Smithsonian Environm Res Ctr, Edgewater, MD 21307 USA. EM mintonm@si.edu OI Minton, Mark/0000-0002-9439-4930 FU Betty Higinbotham Trust; Washington State University FX We thank R. A. Black, R. M. Hannan, C. L. Kinter, E. L. Minton, R. R. Pattison and R. B. Pratt for their support and comments throughout the project. R. Colautti provided helpful comments on an earlier draft of the manuscript. K. Tetrich and the USDA Plant Introduction Facility in Central Ferry, Washington provided essential help. Finally, we are grateful to numerous volunteers, who assisted with the implementation and harvesting of these experiments. This research was supported by grants to M. S. M. from the Betty Higinbotham Trust and a Natural Resources Conservation Grant at Washington State University. Experiments reported in this work comply with the current laws of the United States of America. NR 62 TC 14 Z9 14 U1 1 U2 30 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0029-8549 J9 OECOLOGIA JI Oecologia PD OCT PY 2010 VL 164 IS 2 BP 399 EP 409 DI 10.1007/s00442-010-1667-4 PG 11 WC Ecology SC Environmental Sciences & Ecology GA 650PB UT WOS:000281860700012 PM 20532919 ER PT J AU Puerta-Pinero, C AF Puerta-Pinero, Carolina TI Changes in riparian forest composition along a sedimentation rate gradient SO PLANT ECOLOGY LA English DT Article DE Landscape ecology; Pre-dispersal seed predation; Post-dispersal seed predation; Quercus ilex; Recruitment; Spatial analysis ID POSTDISPERSAL SEED PREDATION; SPATIAL-PATTERNS; QUERCUS-ILEX; JANZEN-CONNELL; LANDSCAPE ECOLOGY; SUS-SCROFA; RECRUITMENT; DISPERSAL; OAK; ESTABLISHMENT AB Riparian forests are highly valued for maintaining water quality through the retention of sediments and nutrients. They also provide some of the most diverse and species-rich habitats in the world. What is largely unknown, however, is how sediment deposition affects plant community composition in these forests. The objective of this study was to examine changes in plant community composition across a gradient of increasing rates of sedimentation in riparian forests in the southeastern Coastal Plain, USA. Seventeen plots were established within riparian forests receiving between 0 and 5.5 cm year(-1) of sediment deposits. Species density and biomass estimates were collected annually from 2002 to 2006 for overstory and mid-story plant species within each plot. Percent cover and nested frequency of understory plant species were determined annually during 2004-2006. Measures of community composition in the understory, mid-story, and overstory layers of forests were compared to changes in environmental factors associated with increased sedimentation. In the understory, annual, exotic, and upland species had higher importance values in plots receiving high sediment deposition. The densities of shade-intolerant and N-fixing species in the mid-story also increased with increasing sedimentation rates. Increased overstory mortality was associated with high sedimentation rates, though increases in understory light levels in these gaps were not the main driver of understory species changes. Edaphic factors, such as soil texture, moisture, and temperature, were significantly correlated to species composition in all three forest layers, suggesting that changes in soil physical structure due to sedimentation may drive community-level changes in these forests. C1 [Puerta-Pinero, Carolina] Univ Granada, Dept Ecol, Fac Ciencias, Granada 18071, Spain. RP Puerta-Pinero, C (reprint author), Smithsonian Trop Res Inst, Unit 9100, Box 0948, DPO, AA 34002 USA. EM puertac@si.edu RI Puerta Pinero, Carolina/B-3186-2012 OI Puerta Pinero, Carolina/0000-0002-0584-7548 FU Spanish Ministry of Science and Education [AP2003-344]; University of Granada [REN2003-07048, CSD2008-00040]; CTFC; Fundacion Caja Madrid FX Jose Maria Gomez Reyes kindly supervised all the intellectual processes of this manuscript. Manuel Martinez helped in constructing all the enclosures in the lab. Abby Britten nicely revised the English writing. Gustavo P. Bornemann, Seila Lopez, Carla Steffler and Alba Puerta Pinero gave vital assistance during the field work. The headquarters of the Sierra Nevada National Park and Jardin Botanico de la Cortijuela offered support for working in the field. Several anonymous referees and JM Espelta deeply improved preliminary versions of this manuscript. This study was supported by the Spanish Ministry of Science and Education via the FPU fellowship AP2003-344, and financial project REN2003-07048 and CSD2008-00040 and postdoctoral fellowships from the University of Granada, CTFC and Fundacion Caja Madrid. NR 56 TC 13 Z9 13 U1 4 U2 21 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1385-0237 J9 PLANT ECOL JI Plant Ecol. PD OCT PY 2010 VL 210 IS 2 BP 213 EP 224 DI 10.1007/s11258-010-9750-9 PG 12 WC Plant Sciences; Ecology; Forestry SC Plant Sciences; Environmental Sciences & Ecology; Forestry GA 642ZE UT WOS:000281259700002 ER PT J AU Henry, TJ AF Henry, Thomas J. TI NEW PLANT BUG (HEMIPTERA: HETEROPTERA: MIRIDAE) RECORDS FOR WEST VIRGINIA SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Insecta; Hemiptera; Heteroptera; Miridae; West Virginia; USA; new records ID NORTH-AMERICA HETEROPTERA; EASTERN-UNITED-STATES; PILOPHORINI HETEROPTERA; PHYLINAE; REVISION; FIEBER; GENUS; HAHN AB Thirty-two species of Miridae are recorded for the first time from West Virginia. With an additional six species reported in the literature and two subsequent synonymies since the 1983 "Annotated List..." by Wheeler, Mason, and Henry, 283 species of Miridae are now known from the state. The new records include six species in the subfamily Bryocorinae, two in Cylapinae, two in Deraeocorinae, twelve in Mirinae, seven in Orthotylinae, and three in Phylinae. Locality information, specific dates, associated host data, and number of specimens and sex are given for each species. Names used in the previous 1983 list are updated. C1 Smithsonian Inst, Natl Museum Nat Hist, Systemat Entomol Lab, Inst Plant Sci,ARS,USDA, Washington, DC 20013 USA. RP Henry, TJ (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Systemat Entomol Lab, Inst Plant Sci,ARS,USDA, POB 37012, Washington, DC 20013 USA. EM thomas.henry@ars.usda.gov NR 49 TC 1 Z9 1 U1 1 U2 1 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD OCT PY 2010 VL 112 IS 4 BP 490 EP 499 DI 10.4289/0013-8797.112.4.490 PG 10 WC Entomology SC Entomology GA 708IN UT WOS:000286355600002 ER PT J AU Wheeler, AG Evans, GA Vandenberg, NJ AF Wheeler, A. G., Jr. Evans, Gregory A. Vandenberg, Natalia J. TI PSEUDOCOCCUS SACCHARICOLA TAKAHASHI (HEMIPTERA: PSEUDOCOCCIDAE) IN THE BRITISH VIRGIN ISLANDS: FIRST WESTERN HEMISPHERE RECORDS, WITH RECORDS OF A CO-OCCURRING LADY BEETLE, HYPERASPIS SCUTIFERA (MULSANT) (COLEOPTERA: COCCINELLIDAE) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Insecta; yellowish sugarcane mealybug; adventive species; insect detection; new records; new synonymy; West Indies ID DISPERSAL; INSECTS; INDIES; NORTH; PESTS AB Pseudococcus saccharicola Takahashi was collected on Guana Island, and nearby Beef Island and Tortola, in the British Virgin islands (BVI). The records are the first in the Western Hemisphere for this potentially important Old World pest of sugarcane and certain other graminoid crops. Host plants on Guana were Chloris barbata Sw. (swollen fingergrass), C. radiata (L.) (radiate fingergrass), Cynodon dactylon L. (bermudagrass), and Saccharum officinarum L. (sugarcane). A probable mealybug predator associated with colonies of P. saccharicola on all three islands was the hyperaspidine coccinellid Hyperaspis scutifera (Mulsant), previously recorded in the West Indies only from the Leeward Antilles (Curacao). Both the mealybug and lady beetle are considered adventive in the BVI. Diagnoses and illustrations of both species are provided to facilitate their recognition. Hyperaspis sanctaeritae Dobzhansky, 1941, described from Arizona, USA, is proposed (by N.J.V.) as a junior synonym of H. scutifera (Mulsant 1850). C1 [Wheeler, A. G., Jr.] Clemson Univ, Dept Entomol Soils & Plant Sci, Clemson, SC 29634 USA. [Evans, Gregory A.] USDA APHIS, Systemat Entomol Lab, PSI, BARC W, Beltsville, MD 20705 USA. [Vandenberg, Natalia J.] Smithsonian Inst, Natl Museum Nat Hist, Systemat Entomol Lab, PSI,USDA ARS, Washington, DC 20013 USA. RP Wheeler, AG (reprint author), Clemson Univ, Dept Entomol Soils & Plant Sci, Clemson, SC 29634 USA. EM awhlr@clemson.edu; Gregory.A.Evans@aphis.usda.gov; Natalia.Vandenberg@ars.usda.gov NR 53 TC 0 Z9 0 U1 1 U2 2 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD OCT PY 2010 VL 112 IS 4 BP 565 EP 575 DI 10.4289/0013-8797.112.4.565 PG 11 WC Entomology SC Entomology GA 708IN UT WOS:000286355600011 ER PT J AU Loinard, L Rodriguez, LF Gomez, L Canto, J Raga, AC Goodman, AA Arce, HG AF Loinard, L. Rodriguez, L. F. Gomez, L. Canto, J. Raga, A. C. Goodman, A. A. Arce, H. G. TI A REASSESSMENT OF THE KINEMATICS OF PV CEPHEI BASED ON ACCURATE PROPER MOTION MEASUREMENTS SO REVISTA MEXICANA DE ASTRONOMIA Y ASTROFISICA LA English DT Article DE astrometry; ISM: individual (PV Cep); ISM: jets and outflows; stars: pre-main sequence ID SYSTEM IRAS 16293-2422; YOUNG STELLAR-SYSTEM; MULTIPLE SYSTEM; RADIO-SOURCES; SIDE WIND; JET; ORION; STAR; EJECTION; REGION AB We present two Very Large Array observations of the pre-main-sequence star PV Cephei, taken with a separation of 10.5 years. These data show that the proper motions of this star are mu(alpha) cos delta = +10.9 +/- 3.0 mas yr(-1); mu(alpha) = +0.2 +/- 1.8 mas yr(-1), very similar to those -previously known- of HD 200775, the B2Ve star that dominates the illumination of the nearby reflection nebula NGC 7023. This result suggests that PV Cephei is not a rapidly moving runaway star as suggested by previous studies. The large velocity of PV Cephei had been inferred from the systematic eastward displacement of the bisectors of successive pairs of Herbig Haro knots along its flow. These systematic shifts might instead result from an intrinsic asymmetry in the ejection mechanisms, or in the distribution of the circumstellar material. C1 [Loinard, L.; Rodriguez, L. F.] Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico. [Canto, J.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. [Raga, A. C.] Univ Nacl Autonoma Mexico, Inst Ciencias Nucl, Mexico City 04510, DF, Mexico. [Gomez, L.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Goodman, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Arce, H. G.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. RP Loinard, L (reprint author), Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Apdo Postal 3-72 Xangari, Morelia 58089, Michoacan, Mexico. EM l.loinard@crya.unam.mx; l.rodriguez@crya.unam.mx; lgo-mez@mpifr.de; raga@nucleares.unam.mx; agoodman@cfa.harvard.edu; hector.arce@yale.edu RI Goodman, Alyssa/A-6007-2010 OI Goodman, Alyssa/0000-0003-1312-0477 FU DGAPA, Universidad Nacional Autonoma de Mexico; International Max Planck Research School (IMPRS); Conacyt (Mexico) FX LFR, LL, JC and ACE acknowledge the support of DGAPA, Universidad Nacional Autonoma de Mexico, and of Conacyt (Mexico). L. G. was supported for this research through a stipend from the International Max Planck Research School (IMPRS) for Astronomy and Astrophysics at the Universities of Bonn and Cologne. This research has made use of the SIMBAD database, operated. at CDS, Strasbourg, France. NR 34 TC 0 Z9 0 U1 0 U2 0 PU UNIV NACIONAL AUTONOMA MEXICO, INST DE ASTRONOMIA PI MEXICO CITY PA APDO POSTAL 70-264, MEXICO CITY 04510, MEXICO SN 0185-1101 J9 REV MEX ASTRON ASTR JI Rev. Mex. Astron. Astrofis. PD OCT PY 2010 VL 46 IS 2 BP 367 EP 375 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 659WC UT WOS:000282596800016 ER PT J AU Holman, MJ Fabrycky, DC Ragozzine, D Ford, EB Steffen, JH Welsh, WF Lissauer, JJ Latham, DW Marcy, GW Walkowicz, LM Batalha, NM Jenkins, JM Rowe, JF Cochran, WD Fressin, F Torres, G Buchhave, LA Sasselov, DD Borucki, WJ Koch, DG Basri, G Brown, TM Caldwell, DA Charbonneau, D Dunham, EW Gautier, TN Geary, JC Gilliland, RL Haas, MR Howell, SB Ciardi, DR Endl, M Fischer, D Furesz, G Hartman, JD Isaacson, H Johnson, JA MacQueen, PJ Moorhead, AV Morehead, RC Orosz, JA AF Holman, Matthew J. Fabrycky, Daniel C. Ragozzine, Darin Ford, Eric B. Steffen, Jason H. Welsh, William F. Lissauer, Jack J. Latham, David W. Marcy, Geoffrey W. Walkowicz, Lucianne M. Batalha, Natalie M. Jenkins, Jon M. Rowe, Jason F. Cochran, William D. Fressin, Francois Torres, Guillermo Buchhave, Lars A. Sasselov, Dimitar D. Borucki, William J. Koch, David G. Basri, Gibor Brown, Timothy M. Caldwell, Douglas A. Charbonneau, David Dunham, Edward W. Gautier, Thomas N., III Geary, John C. Gilliland, Ronald L. Haas, Michael R. Howell, Steve B. Ciardi, David R. Endl, Michael Fischer, Debra Fueresz, Gabor Hartman, Joel D. Isaacson, Howard Johnson, John A. MacQueen, Phillip J. Moorhead, Althea V. Morehead, Robert C. Orosz, Jerome A. TI Kepler-9: A System of Multiple Planets Transiting a Sun-Like Star, Confirmed by Timing Variations SO SCIENCE LA English DT Article ID EXTRA-SOLAR PLANETS; SUPER-EARTHS; SOLID EXOPLANETS; HARPS SEARCH; MASS; RESONANCES; DYNAMICS; MOTION; PERFORMANCE; STABILITY AB The Kepler spacecraft is monitoring more than 150,000 stars for evidence of planets transiting those stars. We report the detection of two Saturn-size planets that transit the same Sun-like star, based on 7 months of Kepler observations. Their 19.2- and 38.9-day periods are presently increasing and decreasing at respective average rates of 4 and 39 minutes per orbit; in addition, the transit times of the inner body display an alternating variation of smaller amplitude. These signatures are characteristic of gravitational interaction of two planets near a 2: 1 orbital resonance. Six radial-velocity observations show that these two planets are the most massive objects orbiting close to the star and substantially improve the estimates of their masses. After removing the signal of the two confirmed giant planets, we identified an additional transiting super-Earth-size planet candidate with a period of 1.6 days. C1 [Holman, Matthew J.; Fabrycky, Daniel C.; Ragozzine, Darin; Latham, David W.; Fressin, Francois; Torres, Guillermo; Buchhave, Lars A.; Sasselov, Dimitar D.; Charbonneau, David; Geary, John C.; Fueresz, Gabor; Hartman, Joel D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ford, Eric B.; Moorhead, Althea V.; Morehead, Robert C.] Univ Florida, Gainesville, FL 32611 USA. [Steffen, Jason H.] Fermilab Ctr Particle Astrophys, Batavia, IL 60510 USA. [Welsh, William F.; Orosz, Jerome A.] San Diego State Univ, San Diego, CA 92182 USA. [Lissauer, Jack J.; Jenkins, Jon M.; Rowe, Jason F.; Borucki, William J.; Koch, David G.; Caldwell, Douglas A.; Haas, Michael R.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Lissauer, Jack J.] Stanford Univ, Stanford, CA 94305 USA. [Marcy, Geoffrey W.; Walkowicz, Lucianne M.; Basri, Gibor; Isaacson, Howard] Univ Calif Berkeley, Berkeley, CA 94720 USA. [Batalha, Natalie M.] San Jose State Univ, San Jose, CA 95192 USA. [Jenkins, Jon M.; Caldwell, Douglas A.] SETI Inst, Mountain View, CA 94043 USA. [Cochran, William D.; Endl, Michael; MacQueen, Phillip J.] Univ Texas Austin, Austin, TX 78712 USA. [Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Ciardi, David R.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Brown, Timothy M.] Global Telescope, Las Cumbres Observ, Goleta, CA 93117 USA. [Dunham, Edward W.] Lowell Observ, Flagstaff, AZ 86001 USA. [Gautier, Thomas N., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Gilliland, Ronald L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Howell, Steve B.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Fischer, Debra] Yale Univ, New Haven, CT 06510 USA. [Brown, Timothy M.] Univ Calif Santa Barbara, Santa Barbara, CA 93106 USA. RP Holman, MJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mholman@cfa.harvard.edu RI Steffen, Jason/A-4320-2013; Ragozzine, Darin/C-4926-2013; Caldwell, Douglas/L-7911-2014; OI Caldwell, Douglas/0000-0003-1963-9616; Buchhave, Lars A./0000-0003-1605-5666; Ciardi, David/0000-0002-5741-3047; Fabrycky, Daniel/0000-0003-3750-0183 FU NASA's Science Mission Directorate; NASA [NCC2-1390]; NSF [0707203] FX Funding for this Discovery mission is provided by NASA's Science Mission Directorate. We acknowledge NASA Cooperative Agreement NCC2-1390. D. C. F. acknowledges support from the Michelson Fellowship, supported by NASA and administered by the NASA Exoplanet Science Institute. This material is based on work supported by the NSF under grant no. 0707203. This work is based, in part, on observations obtained at the W. M. Keck Observatory, which is operated by the Univ. of California and the California Institute of Technology. Some of the observations in this paper were obtained at Kitt Peak National Observatory, National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy under cooperative agreement with the NSF. J.F.R. is a NASA postdoctoral program fellow. We are grateful to N. Haghighipour for many helpful comments and suggestions. NR 44 TC 213 Z9 213 U1 1 U2 11 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD OCT 1 PY 2010 VL 330 IS 6000 BP 51 EP 54 DI 10.1126/science.1195778 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 656KW UT WOS:000282334500030 PM 20798283 ER PT J AU Clough, GW AF Clough, G. Wayne TI Show and Tell SO SMITHSONIAN LA English DT Editorial Material C1 Smithsonian Inst, Washington, DC 20560 USA. RP Clough, GW (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SMITHSONIAN ASSOC PI WASHINGTON PA 900 JEFFERSON DR, WASHINGTON, DC 20560 USA SN 0037-7333 J9 SMITHSONIAN JI Smithsonian PD OCT PY 2010 VL 41 IS 6 BP 28 EP 28 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 655IP UT WOS:000282243500008 ER PT J AU Wakelam, V Smith, IWM Herbst, E Troe, J Geppert, W Linnartz, H Oberg, K Roueff, E Agundez, M Pernot, P Cuppen, HM Loison, JC Talbi, D AF Wakelam, V. Smith, I. W. M. Herbst, E. Troe, J. Geppert, W. Linnartz, H. Oeberg, K. Roueff, E. Agundez, M. Pernot, P. Cuppen, H. M. Loison, J. C. Talbi, D. TI Reaction Networks for Interstellar Chemical Modelling: Improvements and Challenges SO SPACE SCIENCE REVIEWS LA English DT Review DE Astrochemistry; Reaction rate coefficients; Gas-phase chemistry; Grain-surface chemistry; Chemical modelling; Uncertainty propagation; Sensitivity analysis ID MOLECULAR-HYDROGEN FORMATION; GAS-PHASE REACTIONS; PHOTOCHEMICAL KINETICS UNCERTAINTIES; ENVELOPE SURROUNDING IRC+10216; NEUTRAL-NEUTRAL REACTIONS; MONTE-CARLO SIMULATIONS; ADIABATIC CHANNEL MODEL; ELEY-RIDEAL MECHANISM; GRAPHITE SURFACE; TITANS ATMOSPHERE AB We survey the current situation regarding chemical modelling of the synthesis of molecules in the interstellar medium. The present state of knowledge concerning the rate coefficients and their uncertainties for the major gas-phase processes-ion-neutral reactions, neutral-neutral reactions, radiative association, and dissociative recombination-is reviewed. Emphasis is placed on those key reactions that have been identified, by sensitivity analyses, as 'crucial' in determining the predicted abundances of the species observed in the interstellar medium. These sensitivity analyses have been carried out for gas-phase models of three representative, molecule-rich, astronomical sources: the cold dense molecular clouds TMC-1 and L134N, and the expanding circumstellar envelope IRC +10216. Our review has led to the proposal of new values and uncertainties for the rate coefficients of many of the key reactions. The impact of these new data on the predicted abundances in TMC-1 and L134N is reported. Interstellar dust particles also influence the observed abundances of molecules in the interstellar medium. Their role is included in gas-grain, as distinct from gas-phase only, models. We review the methods for incorporating both accretion onto, and reactions on, the surfaces of grains in such models, as well as describing some recent experimental efforts to simulate and examine relevant processes in the laboratory. These efforts include experiments on the surface-catalyzed recombination of hydrogen atoms, on chemical processing on and in the ices that are known to exist on the surface of interstellar grains, and on desorption processes, which may enable species formed on grains to return to the gas-phase. C1 [Wakelam, V.] Univ Bordeaux, Observ Aquitain Sci Univers, F-33271 Floirac, France. [Wakelam, V.] CNRS, Lab Astrophys Bordeaux, UMR 5804, F-33271 Floriac, France. [Smith, I. W. M.] Univ Chem Labs, Cambridge CB2 1EW, England. [Herbst, E.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Herbst, E.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Herbst, E.] Ohio State Univ, Dept Chem, Columbus, OH 43210 USA. [Troe, J.] Univ Gottingen, Inst Phys Chem, D-37077 Gottingen, Germany. [Troe, J.] Max Planck Inst Biophys Chem, D-37077 Gottingen, Germany. [Geppert, W.] Univ Stockholm, Dept Phys, S-10691 Stockholm, Sweden. [Linnartz, H.; Oeberg, K.; Cuppen, H. M.] Leiden Univ, Sackler Lab Astrophys, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Oeberg, K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Roueff, E.] Univ Paris 07, F-92195 Meudon, France. [Roueff, E.] CNRS, Observ Paris, LUTH, UMR 8102, F-92195 Meudon, France. [Agundez, M.] Observ Paris, LUTH, F-92190 Meudon, France. [Pernot, P.] Univ Paris 11, Chim Phys Lab, UMR 8000, F-91405 Orsay, France. [Pernot, P.] CNRS, F-91405 Orsay, France. [Loison, J. C.] Univ Bordeaux 1, Inst Mol Sci, CNRS, UMR 5255, F-33405 Talence, France. [Talbi, D.] Univ Montpellier 2, GRAAL, CNRS, UMR 5024, F-34095 Montpellier, France. RP Wakelam, V (reprint author), Univ Bordeaux, Observ Aquitain Sci Univers, BP 89, F-33271 Floirac, France. EM wakelam@obs.u-bordeaux1.fr RI PERNOT, Pascal/C-2643-2008; Cuppen, Herma/F-9729-2015; Agundez, Marcelino/I-5369-2012; OI PERNOT, Pascal/0000-0001-8586-6222; Cuppen, Herma/0000-0003-4397-0739; Agundez, Marcelino/0000-0003-3248-3564; Wakelam, Valentine/0000-0001-9676-2605 FU French program PCMI; Center for the Chemistry of the Universe (NSF, US); Royal Society FX We acknowledge the "International Space Science Institute" for hosting the meetings of the international team "A new generation of databases for interstellar chemical modeling in preparation for HSO and ALMA". We would also like to thank the following people who took part in one or both of the ISSI meetings but did not contribute a section to this report: Nathalie Carrasco, Prof. Ewine van Dishoeck, Prof. Dieter Gerlich, Eric Hebrard, Liv Hornekaer, Andrew Markwick, Prof. Tom Millar, Anton Vasyunin. V.W. thanks Astrid Bergeat for discussions about N + NO reaction. V.W., JC.L. and D. T. thank the French program PCMI for partial funding of this work. E. H. wishes to thank the Center for the Chemistry of the Universe (NSF, US) for support of his program in chemical kinetics. VW and IWMS thank the Royal Society for a grant to facilitate their co-operation. NR 200 TC 104 Z9 104 U1 6 U2 58 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 EI 1572-9672 J9 SPACE SCI REV JI Space Sci. Rev. PD OCT PY 2010 VL 156 IS 1-4 BP 13 EP 72 DI 10.1007/s11214-010-9712-5 PG 60 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 726WX UT WOS:000287758700002 ER PT J AU Dorr, LJ Wiersema, JH AF Dorr, Laurence J. Wiersema, John H. TI Typification of names of American species of vascular plants proposed by Linnaeus and based on Loefling's Iter Hispanicum (1758) SO TAXON LA English DT Article DE Nicolaus Joseph von Jacquin; neotype; nomenclature; lectotype; Linnaean names; Pehr Loefling; Iter Hispanicum AB Neotypes are proposed for the names of ten species of American plants that Linnaeus based in whole or in part on descriptions in Loefling's Iter Hispanicum:Allionia incarnata, Allionia violacea, Ayenia tomentosa, Byttneria scabra, Krameria ixine, Lecythis ollaria, Moniera trifolia, Viola arborea, Viola calceolaria, and Viola oppositifolia. Lectotypes are proposed for the names of six species of American plants that Linnaeus based in whole or in part on descriptions in the same work: Ayenia magna, Cecropia peltata, Ellisia acuta, jussiaea pubescens, Loranthus occidentalis, and Spermacoce strigosa. A neotype also is proposed for a Jacquin name, Hybanthus havanensis, which Linnaeus renamed as Viola hybanthus. We also argue that Laetia americana is neotypified by the type applied to the illegitimate name Laetia apetala. C1 [Dorr, Laurence J.] Natl Museum Nat Hist, Dept Bot, Smithsonian Inst, Washington, DC 20013 USA. [Wiersema, John H.] USDA ARS, Natl Germplasm Resources Lab, Beltsville Agr Res Ctr BARC W, Beltsville, MD 20705 USA. RP Dorr, LJ (reprint author), Natl Museum Nat Hist, Dept Bot, Smithsonian Inst, MRC 166,POB 37012, Washington, DC 20013 USA. EM dorrl@si.edu NR 35 TC 7 Z9 8 U1 0 U2 1 PU INT ASSOC PLANT TAXONOMY-IAPT PI BRATISLAVA PA C/O INST BOTANY, SLOVAK ACAD SCIENCES DUBRAVSKA CESTA 9, SK-845 23 BRATISLAVA, SLOVAKIA SN 0040-0262 EI 1996-8175 J9 TAXON JI Taxon PD OCT PY 2010 VL 59 IS 5 BP 1571 EP 1577 PG 7 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA 663XZ UT WOS:000282924800021 ER PT J AU Pretzer, WS AF Pretzer, William S. TI Structures of Change in the Mechanical Age: Technological Innovation in the United States, 1790-1865 SO TECHNOLOGY AND CULTURE LA English DT Book Review C1 [Pretzer, William S.] Smithsonian Inst, Natl Museum African Amer Hist & Culture, Washington, DC 20560 USA. RP Pretzer, WS (reprint author), Smithsonian Inst, Natl Museum African Amer Hist & Culture, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU JOHNS HOPKINS UNIV PRESS PI BALTIMORE PA JOURNALS PUBLISHING DIVISION, 2715 NORTH CHARLES ST, BALTIMORE, MD 21218-4363 USA SN 0040-165X J9 TECHNOL CULT JI Technol. Cult. PD OCT PY 2010 VL 51 IS 4 BP 1026 EP 1028 PG 3 WC History & Philosophy Of Science SC History & Philosophy of Science GA 685YN UT WOS:000284664100021 ER PT J AU Litaker, RW Vandersea, MW Faust, MA Kibler, SR Nau, AW Holland, WC Chinain, M Holmes, MJ Tester, PA AF Litaker, R. Wayne Vandersea, Mark W. Faust, Maria A. Kibler, Steven R. Nau, Amy W. Holland, William C. Chinain, Mireille Holmes, Michael J. Tester, Patricia A. TI Global distribution of ciguatera causing dinoflagellates in the genus Gambierdiscus SO TOXICON LA English DT Article DE Biogeography; CFP; Ciguatera fish poisoning; Gambierdiscus australes; G. belizeanus; G. caribaeus; G. carpenteri; G. carolinianus; G. pacificus; G. polynesiensis; G. ruetzleri; G. toxicus; G. yasumotoi; Maitotoxin; Monitoring; Phylogeny; Ribotype ID WATER-SOLUBLE TOXIN; JACK CARANX-LATUS; FRENCH-POLYNESIA; INDIAN-OCEAN; CARIBBEAN CIGUATOXINS; FUKUYO DINOPHYCEAE; FLORIDA KEYS; CORAL-REEF; TOXICITY; FISH AB Dinoflagellates in the genus Gambierdiscus produce toxins that bioaccumulate in tropical and sub-tropical fishes causing ciguatera fish poisoning (CFP). Little is known about the diversity and distribution of Gambierdiscus species, the degree to which individual species vary in toxicity, and the role each plays in causing CFP. This paper presents the first global distribution of Gambierdiscus species. Phylogenetic analyses of the existing isolates indicate that five species are endemic to the Atlantic (including the Caribbean/West Indies and Gulf of Mexico), five are endemic to the tropical Pacific, and that two species. Gambierdiscus carpenteri and Gambierdiscus caribaeus are globally distributed. The differences in Gambierdiscus species composition in the Atlantic and Pacific correlated with structural differences in the ciguatoxins reported from Atlantic and Pacific fish. This correlation supports the hypothesis that Gambierdiscus species in each region produce different toxin suites. A literature survey indicated a >100-fold variation in toxicity among species compared with a 2 to 9-fold within species variation due to changing growth conditions. These observations suggest that CFP events are driven more by inherent differences in species toxicity than by environmental modulation. How variations in species toxicity may affect the development of an early warning system for CFP is discussed. Published by Elsevier Ltd. C1 [Litaker, R. Wayne; Vandersea, Mark W.; Kibler, Steven R.; Nau, Amy W.; Holland, William C.; Tester, Patricia A.] NOAA, NOS, Ctr Coastal Fisheries & Habitat Res, Beaufort, NC 28516 USA. [Faust, Maria A.] Smithsonian Inst, United States Natl Herbarium, Dept Bot, Suitland, MD 20746 USA. [Chinain, Mireille] Inst Louis Malarde, Lab Microalgues Tox, Papeete 98713, Tahiti, Fr Polynesia. [Holmes, Michael J.] Queensland Dept Environm & Resource Management, Brisbane, Qld 4001, Australia. RP Litaker, RW (reprint author), NOAA, NOS, Ctr Coastal Fisheries & Habitat Res, 101 Pivers Isl Rd, Beaufort, NC 28516 USA. EM wayne.litaker@noaa.gov FU Smithsonian Institution; Smithsonian Institution Hunterdon Oceanographic Research Endowment; NOAA FX We thank Dr. Klaus Rutzler, National Museum of Natural History, Smithsonian Institution for his long-term support of the research program in Belize from which we have benefited greatly. Special thanks to Michael Carpenter and Bertol Pfeiffer for logistic support. Dr. Clement Lewsey from NOAA's International Programs Office provided critical support for the sampling efforts in the Puerto Rico region. Partial support for the research also came from grants provided by the Smithsonian Institution Caribbean Coral Reef Ecosystem Program (CCRE), the Smithsonian Institution Hunterdon Oceanographic Research Endowment and NOAA program funds. This is contribution number 844 of the Caribbean Coral Reef Ecosystems Program. We thank Paula Whitfield, Christine Addison, Brian Degan, Roldan Munoz, John Burke, Dave Cerino, Michael Dowgiallo, Wilson Freshwater, David Johnson, Brett Harrison, Doug Kesling, William Lee, Roger Mays, James Morris, Brandon Puckett, Sherry Reed, and Brad Teer for assisting in sample collection from the Caribbean and West Indies. NR 137 TC 73 Z9 79 U1 6 U2 41 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0041-0101 J9 TOXICON JI Toxicon PD OCT PY 2010 VL 56 IS 5 SI SI BP 711 EP 730 DI 10.1016/j.toxicon.2010.05.017 PG 20 WC Pharmacology & Pharmacy; Toxicology SC Pharmacology & Pharmacy; Toxicology GA 645XN UT WOS:000281499600008 PM 20561539 ER PT J AU Hoffman, RN Dailey, P Hopsch, S Ponte, RM Quinn, K Hill, EM Zachry, B AF Hoffman, Ross N. Dailey, Peter Hopsch, Susanna Ponte, Rui M. Quinn, Katherine Hill, Emma M. Zachry, Brian TI An Estimate of Increases in Storm Surge Risk to Property from Sea Level Rise in the First Half of the Twenty-First Century SO WEATHER CLIMATE AND SOCIETY LA English DT Article AB Sea level is rising as the World Ocean warms and ice caps and glaciers melt. Published estimates based on data from satellite altimeters, beginning in late 1992, suggest that the global mean sea level has been rising on the order of 3 mm yr(-1). Local processes, including ocean currents and land motions due to a variety of causes, modulate the global signal spatially and temporally. These local signals can be much larger than the global signal, and especially so on annual or shorter time scales. Even increases on the order of 10 cm in sea level can amplify the already devastating losses that occur when a hurricane-driven storm surge coincides with an astronomical high tide. To quantify the sensitivity of property risk to increasing sea level, changes in expected annual losses to property along the U. S. Gulf and East Coasts are calculated as follows. First, observed trends in sea level rise from tide gauges are extrapolated to the year 2030, and these changes are interpolated to all coastal locations. Then a 10 000-yr catalog of simulated hurricanes is used to define critical wind parameters for each event. These wind parameters then drive a parametric time-evolving storm surge model that accounts for bathymetry, coastal geometry, surface roughness, and the phase of the astronomical tide. The impact of the maximum storm surge height on a comprehensive inventory of commercial and residential property is then calculated, using engineering models that take into account the characteristics of the full range of construction types. Average annual losses projected to the year 2030 are presented for regions and key states and are normalized by aggregate property value on a zip code by zip code basis. Comparisons to the results of a control run reflecting the risk today quantify the change in risk per dollar of property on a percentage basis. Increases in expected losses due to the effect of sea level rise alone vary by region, with increases of 20% or more being common. Further sensitivity tests quantify the impact on the risk of sea level rise plus additional factors, such as changes in hurricane frequency and intensity as a result of rising sea surface temperatures. C1 [Hoffman, Ross N.; Hopsch, Susanna; Ponte, Rui M.; Quinn, Katherine] Atmospher & Environm Res Inc, Lexington, MA 02421 USA. [Dailey, Peter; Hopsch, Susanna; Zachry, Brian] AIR Worldwide Corp, Boston, MA USA. [Hill, Emma M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Hoffman, RN (reprint author), Atmospher & Environm Res Inc, 131 Hartwell Ave, Lexington, MA 02421 USA. EM rhoffman@aer.com RI Hill, Emma/B-7037-2011; OI Hill, Emma/0000-0003-0231-5818; Ponte, Rui/0000-0001-7206-6461 FU NASA [NNX07AM77G]; NSF [OCE-0961507] FX Tide gauge data used in this study came from the PSMSL and NOAA (NOAA 2007). E. M. Hill and R. M. Ponte were supported by the NASA Grant NNX07AM77G. Additional support at AER was provided by NSF Grant OCE-0961507. NR 48 TC 10 Z9 14 U1 2 U2 10 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1948-8327 EI 1948-8335 J9 WEATHER CLIM SOC JI Weather Clim. Soc. PD OCT PY 2010 VL 2 IS 4 BP 271 EP 293 DI 10.1175/2010WCAS1050.1 PG 23 WC Environmental Studies; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA V22HT UT WOS:000208267000003 ER PT J AU Mathis, WN Marinoni, L AF Mathis, Wayne N. Marinoni, Luciane TI A review of Diphuia (Diptera: Ephydridae) with description of two new species from southern Brazil SO ZOOLOGIA LA English DT Review DE Neotropical; New World; shore-fly; taxonomy ID CRESSON DIPTERA; REVISION AB The species of Diphuia Cresson, 1944 are reviewed with an emphasis on the fauna from southern Brazil, where two new species have been discovered and herein are described: Diphuia antonina sp. nov. and Diphuia grandis sp. nov. All known species are placed into two species groups (the anomala and nitida groups), which are characterized, and a key to these species is included. To facilitate identification of species of this uncommon genus, we have included diagnoses of the genus and tribe Hecamedini and have also provided an annotated key to New World genera in the tribe and to the known species of Diphuia. We have also provided illustrations of structures of the male terminalia of all included species. The species from southern Brazil, including the new ones, are illustrated. C1 [Mathis, Wayne N.] Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA. [Marinoni, Luciane] Univ Fed Parana, Dept Zool, BR-81531980 Curitiba, Parana, Brazil. RP Mathis, WN (reprint author), Smithsonian Inst, Dept Entomol, NHB 169,POB 37012, Washington, DC 20013 USA. EM mathisw@si.edu; lmarinoni@ufpr.br RI Marinoni, Luciane /C-5720-2013 FU CNPq [401609/2009-0] FX Recent field work in Brazil (December 2009-June 2010) that resulted in the vast majority of specimens studied in this paper was supported by a grant from CNPq (Visiting Researcher/Process 401609/2009-0), which we gratefully acknowledge and thank. We thank Dianne Mathis for helping with all aspects of the production of this paper, especially the field work in Brazil. We also thank A. Bernardo Carvalho and his lab (Elisa, Monica, Susana) for hosting us while conducting field work along the coast of Sao Paulo. NR 17 TC 2 Z9 2 U1 0 U2 2 PU SOC BRASILEIRA ZOOLOGIA, UNIV FEDERAL PARANA PI CURITIBA PA CAIXA POSTAL 19020, CURITIBA, PARANA 81531-980, BRAZIL SN 1984-4670 J9 ZOOLOGIA-CURITIBA JI Zoologia PD OCT PY 2010 VL 27 IS 5 BP 803 EP 812 DI 10.1590/S1984-46702010000500017 PG 10 WC Zoology SC Zoology GA 699LX UT WOS:000285666000017 ER PT J AU Baeza, JA AF Baeza, J. Antonio TI Molecular systematics of peppermint and cleaner shrimps: phylogeny and taxonomy of the genera Lysmata and Exhippolysmata (Crustacea: Caridea: Hippolytidae) SO ZOOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE Exhippolysmata; hermaphrodite; Hippolytidae; Lysmata; Merguia ID PROTANDRIC SIMULTANEOUS HERMAPHRODITISM; SEX ALLOCATION; MARINE SHRIMP; GENUS LYSMATA; EVOLUTION; DECAPODA; DNA AB Shrimps from the ecologically diverse genera Lysmata and Exhippolysmata are rare among marine invertebrates because they are protandric simultaneous hermaphrodites: shrimps initially mature and reproduce solely as males, and later in life become functional simultaneous hermaphrodites. Considerable progress on the reproductive ecology of members from these two genera has been achieved during the last decade. However, several outstanding issues of systematic nature remain to be addressed. Here, a molecular phylogeny of these two genera was used to examine the overall evolutionary relationship within and between species and genera, and to answer various questions related to the systematic status of several species. The present phylogenetic analysis, including 53 sequences and 26 species of Lysmata and Exhippolysmata, indicates that semiterrestrial shrimps from the genus Merguia represent the sister group to a second natural clade composed by shrimps from the genera Lysmata and Exhippolysmata. Also, the phylogenetic analysis confirmed that the genus Lysmata is paraphyletic, and includes the genus Exhippolysmata, as noted in a preliminary study. The tree partially supports the separation of species with or without a developed accessory branch into two different genera or subgenera ( i. e. Lysmata and Hippolysmata having a well- developed accessory branch, or not, respectively). The genetic distance between the cleaner shrimps Lysmata amboinensis and Lysmata grabhami was smaller than has been observed between other sister species. On the other hand, the topology of the tree indicates that these two entities are reciprocally monophyletic. Thus, this latter result, together with minor but constant differences in the colour pattern reported for these two entities, indicates that there is no reason to stop treating them as different valid species. This study enabled the long overdue resolution of standing taxonomic questions in shrimps from the genera Lysmata and Exhippolysmata. In the future, this phylogeny will help to reveal the conditions favouring the origins of several behavioural and morphological novelties in these unique shrimps. c 2010 The Linnean Society of London, Zoological Journal of the Linnean Society, 2010, 160, 254-265. doi: 10.1111/ j. 1096-3642.2009.00605. x C1 [Baeza, J. Antonio] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Baeza, J. Antonio] Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. [Baeza, J. Antonio] Univ Catolica Norte, Fac Ciencias Mar, Dept Biol Marina, Larrondo 1281, Coquimbo, Chile. RP Baeza, JA (reprint author), Smithsonian Trop Res Inst, Apartado Postal 0843-03092, Balboa, Ancon, Panama. EM baezaa@si.edu OI Baeza, Juan Antonio/0000-0002-2573-6773 FU STRI; SMSFP; National Geographic Society, USA FX Many thanks to Bill Hoffman from the Smithsonian Marine Ecosystems Exhibit (SMEE), Valerie Paul, Raphael Ritson-Williams, and Julie Piraino from the Smithsonian Marine Station at Fort Pierce (SMSFP), Narissa Bax from New Zealand, Luis Ignacio Vilchis and William A. Newman from the Scripps Institution of Oceanography (SIO), University of California at San Diego, Juan Bolanos, Jesus Enrique Hernandez, and Regulo Lopez from the Universidad de Oriente (UDO), Boca del Rio, Venezuela, Adriane A. Braga from the Universidade Estadual Paulista (UNESP), Botucatu, Brazil, Arthur Anker from the University of Florida, Gainsville, USA, Carla Piantonni from the National Museum of Natural History, Washington D.C., USA, Arcadio Ortiz from the Smithsonian Tropical Research Institute (STRI), Panama, Nancy Voss from the University of Miami and Fernando Alvarez from the Universidad Nacional Autonoma de Mexico (UNAM), Mexico City, for their help during the different steps of specimen collection and loans. My sincere appreciation goes to Juan Bolanos for inviting me to dictate a course on the Behaviour of Marine Invertebrates at Isla Margarita, where a great portion of this manuscript was written. Especial thanks to Jeff Hunt and Lee Weigt at the Laboratory of Analytical Biology, NMNH, Washington D.C. for their logistical support. JAB thanks the support from a STRI Marine Postdoctoral Fellowship and a SMSFP Postdoctoral Fellowship. This study was partial funded by a National Geographic Research Grant from the National Geographic Society, USA. Raymond T. Bauer (University of Louisiana at Lafayette, USA) and Christoph Schubart (Regensburg Universitat, Germany) helped improve preliminary versions of this manuscript. The comments of two anonymous reviewers substantially improved this manuscript. This is contribution number 790 of the Smithsonian Marine Station at Fort Pierce. NR 45 TC 17 Z9 17 U1 1 U2 10 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0024-4082 EI 1096-3642 J9 ZOOL J LINN SOC-LOND JI Zool. J. Linn. Soc. PD OCT PY 2010 VL 160 IS 2 BP 254 EP 265 DI 10.1111/j.1096-3642.2009.00605.x PG 12 WC Zoology SC Zoology GA 656HY UT WOS:000282321100002 ER PT J AU Mah, C Nizinski, M Lundsten, L AF Mah, Christopher Nizinski, Martha Lundsten, Lonny TI Phylogenetic revision of the Hippasterinae (Goniasteridae; Asteroidea): systematics of deep sea corallivores, including one new genus and three new species SO ZOOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Review DE Arctic; deep-sea coral; deep-sea echinoderm; Evoplosoma; feeding biology; Hippasteria; onshore-offshore; phylogeny; taxonomy ID CORAL LOPHELIA-PERTUSA; ATLANTIC; FAUNA; ECHINODERMATA; CALIFORNIA; STARFISH; GULF; BIOGEOGRAPHY; MEGAFAUNA; HABITAT AB The Hippasterinae is a subfamily within the Goniasteridae, consisting of five genera and 26 species, which occur in cold-water settings ranging from subtidal to abyssal depths. All known genera were included in a cladistic analysis resulting in two most parsimonious trees, supporting the Hippasterinae as monophyletic. Our review supports Sthenaster emmae gen. et sp. nov. as a new genus and species from the tropical Atlantic and two new Evoplosoma species, Evoplosoma claguei sp. nov. and Evoplosoma voratus sp. nov. from seamounts in the North Pacific. Hippasteria caribaea is reassigned to the genus Gilbertaster, which previously contained a single Pacific species. Our analysis supports Evoplosoma as a derived deep water lineage relative to its continental-shelf, shallow water sister taxa. The genus Hippasteria contains approximately 15 widely distributed, but similar-looking species, which occur in the northern and southern hemispheres. Except for Gilbertaster, at least one species in each genus has been observed or is inferred to prey on deep-sea corals, suggesting that this lineage is important to the conservation of deep-sea coral habitats. The Hippasterinae shares several morphological similarities with Circeaster and Calliaster, suggesting that they may be related. c 2010 The Linnean Society of London, Zoological Journal of the Linnean Society, 2010, 160, 266- 301. doi: 10.1111/ j. 1096-3642.2010.00638.x C1 [Mah, Christopher] Natl Museum Nat Hist, Smithsonian Inst Invertebrate Zool, Washington, DC 20013 USA. [Nizinski, Martha] Natl Museum Nat Hist, Natl Marine Fisheries Serv, Natl Systemat Lab, Washington, DC 20013 USA. [Lundsten, Lonny] Monterey Bay Aquarium Res Inst, Video Lab, Moss Landing, CA 95039 USA. RP Mah, C (reprint author), Natl Museum Nat Hist, Smithsonian Inst Invertebrate Zool, MRC 163,POB 37012, Washington, DC 20013 USA. EM mahch@si.edu FU NOAA Office of Ocean Exploration; NMNH; NSF [0631245] FX The authors of this study are indebted to Cynthia Gust Ahearn (deceased), collection manager for the NMNH Echinodermata Collection, and Cheryl Ames (UNCW, National Systematics Laboratory, NMFS) for curatorial assistance. Steve Cairns, curator of Coelenterates, NMNH identified the gorgonian spicules. Dave Pawson, Paul Greenhall, and Linda Ward (NMNH) provided additional logistical and technical support. Mary Catherine Boyett (MCZ) prepared the loan of type material from MCZ. David Clague and James Barry (MBARI) made recent collections available. Support for sampling off the south-eastern coast of the US was provided by grants from NOAA Office of Ocean Exploration (S.W. Ross, lead Investigator). The science party, the crew of the R/V Seward Johnson, and the pilots of the Johnson Sea Link are greatly acknowledged for assistance with collection of western Atlantic material. We thank the crew of the R/V Western Flyer and the pilots of the ROV Tiburon for their assistance with Pacific collections as well as the David and Lucile Packard Foundation for support of MBARI. Michael Carlson prepared the map for Atlantic collections in Figure 1. We also thank Christopher Kelley, Hawaiian Undersea Research Laboratory, for making in situ observations available to us. Daniel Blake, University of Illinois at Urbana Champaign, Andy Gale, University of Portsmouth, and an anonymous reviewer provided useful comments that improved the manuscript. C. Mah was supported by the United States Antarctic Research Program at the NMNH and NSF OPP Postdoctoral Fellows grant # 0631245. NR 131 TC 25 Z9 30 U1 1 U2 13 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0024-4082 J9 ZOOL J LINN SOC-LOND JI Zool. J. Linn. Soc. PD OCT PY 2010 VL 160 IS 2 BP 266 EP 301 DI 10.1111/j.1096-3642.2010.00638.x PG 36 WC Zoology SC Zoology GA 656HY UT WOS:000282321100003 ER PT J AU Zeugin, F Potvin, C Jansa, J Scherer-Lorenzen, M AF Zeugin, F. Potvin, C. Jansa, J. Scherer-Lorenzen, M. TI Is tree diversity an important driver for phosphorus and nitrogen acquisition of a young tropical plantation? SO FOREST ECOLOGY AND MANAGEMENT LA English DT Article DE Biodiversity and ecosystem functioning; Nutrient use efficiency; Sardinilla; Panama; Tropical tree plantations; Resource complementarity; Environmental heterogeneity ID NUTRIENT-USE EFFICIENCY; MIXED-SPECIES PLANTATIONS; COSTA-RICA; HUMID TROPICS; ABOVEGROUND BIOMASS; FOREST PLANTATIONS; ECOSYSTEM FUNCTION; SECONDARY FORESTS; SOIL INTERACTIONS; PURE PLANTATIONS AB Many tropical plantations in Central America are monocultures of fast growing, mostly exotic species such as a teak, eucalypts and pines. This has been perceived as a problem for ecosystem stability, pest control, local biodiversity and long-term nutrient availability. In our study, we followed the effects of increasing tree diversity (1,3 and 6 native species) on aboveground nitrogen (N) and phosphorus (P) pools in a young experimental biodiversity plantation (central Panama) over two subsequent years. Our results show a positive but not consistent net effect of biodiversity on the N and P pools, mainly explained by the complementarity effect. N and P use efficiencies strongly varied among the investigated tree species and the species richness gradient. Anacardium excelsum and Luehea seemannii were associated with higher N and P use efficiencies while Hura crepitans and Tabebuia rosea were less efficient in aboveground biomass production per unit N or P. Tree species tended to have lower P use efficiencies in the intermediate diversity level compared to monocultures and six-species mixtures. Although the environmental conditions explained a large part of the variation in the N and P pools (58%) in our experiment, we argue that incorporating tree mixtures in the management can bring additional benefits and improve tree growth and nutrient uptake as compared to the monocultures. (C) 2010 Elsevier B.V. All rights reserved. C1 [Zeugin, F.; Scherer-Lorenzen, M.] ETH, Inst Plant Anim & Agroecosyst Sci, CH-8092 Zurich, Switzerland. [Potvin, C.] McGill Univ, Dept Biol, Montreal, PQ H3A 1B1, Canada. [Potvin, C.] Smithsonian Trop Res Inst, Panama City, Panama. [Jansa, J.] Swiss Fed Inst Technol, Inst Plant Anim & Agroecosyst Sci, CH-8315 Lindau, Switzerland. RP Zeugin, F (reprint author), ETH, Inst Plant Anim & Agroecosyst Sci, CH-8092 Zurich, Switzerland. EM fabienne.zeugin@ipw.agrl.ethz.ch RI Jansa, Jan/H-3161-2014 OI Jansa, Jan/0000-0002-0331-1774 FU Swiss National Science Foundation [3100A0-110031/1] FX We are grateful to Iliana & Jose Monteza, Felipe Rodriguez and all the field workers in Sardinilla for great help in the field. We would like to thank Ben Turner (Smithsonian Tropical Research Institute, Panama), Karin Sorgel, Annika Lenz and Thomas Flura (ETH Zurich, Switzerland) for help with the lab analyses. Information on the elevation and the slope inclination of each plot and the plantation map were kindly provided by Sebastian Wolf (ETH Zurich, Switzerland). Authors are indebted to Yvonne Oelmann (Johannes Gutenberg University Mainz, Germany) who accepted to share raw data on stem N and P concentrations with us, and to Else Bunemann and Thomas Seitlinger (ETH Zurich and University Zurich, Switzerland), who kindly provided part of the soil phosphorus data. We also like to thank Christian Schob and Petr Smilauer for their advices on the statistical analyses. We are grateful to the Smithsonian Tropical Research Institute, Panama, and especially to Raineldo Urriola, for constant support. This research was made possible by a grant of the Swiss National Science Foundation (3100A0-110031/1). NR 67 TC 17 Z9 17 U1 2 U2 41 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0378-1127 J9 FOREST ECOL MANAG JI For. Ecol. Manage. PD SEP 30 PY 2010 VL 260 IS 9 BP 1424 EP 1433 DI 10.1016/j.foreco.2010.07.020 PG 10 WC Forestry SC Forestry GA 670WO UT WOS:000283458600002 ER PT J AU Arvidson, RE Bell, JF Bellutta, P Cabrol, NA Catalano, JG Cohen, J Crumpler, LS Marais, DJD Estlin, TA Farrand, WH Gellert, R Grant, JA Greenberger, RN Guinness, EA Herkenhoff, KE Herman, JA Iagnemma, KD Johnson, JR Klingelhofer, G Li, R Lichtenberg, KA Maxwell, SA Ming, DW Morris, RV Rice, MS Ruff, SW Shaw, A Siebach, KL de Souza, PA Stroupe, AW Squyres, SW Sullivan, RJ Talley, KP Townsend, JA Wang, A Wright, JR Yen, AS AF Arvidson, R. E. Bell, J. F., III Bellutta, P. Cabrol, N. A. Catalano, J. G. Cohen, J. Crumpler, L. S. Marais, D. J. Des Estlin, T. A. Farrand, W. H. Gellert, R. Grant, J. A. Greenberger, R. N. Guinness, E. A. Herkenhoff, K. E. Herman, J. A. Iagnemma, K. D. Johnson, J. R. Klingelhoefer, G. Li, R. Lichtenberg, K. A. Maxwell, S. A. Ming, D. W. Morris, R. V. Rice, M. S. Ruff, S. W. Shaw, A. Siebach, K. L. de Souza, P. A. Stroupe, A. W. Squyres, S. W. Sullivan, R. J. Talley, K. P. Townsend, J. A. Wang, A. Wright, J. R. Yen, A. S. TI Spirit Mars Rover Mission: Overview and selected results from the northern Home Plate Winter Haven to the side of Scamander crater SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID THERMODYNAMIC BEHAVIOR; THEORETICAL PREDICTION; AQUEOUS ELECTROLYTES; HIGH PRESSURES; TEMPERATURES; DEPOSITS; LIFE AB This paper summarizes Spirit Rover operations in the Columbia Hills, Gusev crater, from sol 1410 (start of the third winter campaign) to sol 2169 (when extrication attempts from Troy stopped to winterize the vehicle) and provides an overview of key scientific results. The third winter campaign took advantage of parking on the northern slope of Home Plate to tilt the vehicle to track the sun and thus survive the winter season. With the onset of the spring season, Spirit began circumnavigating Home Plate on the way to volcanic constructs located to the south. Silica-rich nodular rocks were discovered in the valley to the north of Home Plate. The inoperative right front wheel drive actuator made climbing soil-covered slopes problematical and led to high slip conditions and extensive excavation of subsurface soils. This situation led to embedding of Spirit on the side of a shallow, 8 m wide crater in Troy, located in the valley to the west of Home Plate. Examination of the materials exposed during embedding showed that Spirit broke through a thin sulfate-rich soil crust and became embedded in an underlying mix of sulfate and basaltic sands. The nature of the crust is consistent with dissolution and precipitation in the presence of soil water within a few centimeters of the surface. The observation that sulfate-rich deposits in Troy and elsewhere in the Columbia Hills are just beneath the surface implies that these processes have operated on a continuing basis on Mars as landforms have been shaped by erosion and deposition. C1 [Arvidson, R. E.; Catalano, J. G.; Greenberger, R. N.; Guinness, E. A.; Lichtenberg, K. A.; Shaw, A.; Siebach, K. L.; Wang, A.] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. [Bell, J. F., III; Rice, M. S.; Squyres, S. W.; Sullivan, R. J.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Bellutta, P.; Estlin, T. A.; Herman, J. A.; Maxwell, S. A.; Stroupe, A. W.; Talley, K. P.; Townsend, J. A.; Wright, J. R.; Yen, A. S.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Cabrol, N. A.; Marais, D. J. Des] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Cabrol, N. A.] SETI Inst, Mountain View, CA USA. [Cohen, J.] Honeybee Robot Spacecraft Mech Corp, New York, NY 10001 USA. [Crumpler, L. S.] New Mexico Museum Nat Hist & Sci, Albuquerque, NM 87104 USA. [Farrand, W. H.] Space Sci Inst, Boulder, CO 80301 USA. [Gellert, R.] Univ Guelph, Dept Phys, Guelph, ON N1G 2W1, Canada. [Grant, J. A.] Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. [Herkenhoff, K. E.; Johnson, J. R.] US Geol Survey, Flagstaff, AZ 86001 USA. [Iagnemma, K. D.] MIT, Dept Mech Engn, Cambridge, MA 02139 USA. [Klingelhoefer, G.] Johannes Gutenberg Univ Mainz, Inst Anorgan & Analyt Chem, D-55099 Mainz, Germany. [Li, R.] Ohio State Univ, Dept Civil & Environm Engn & Geodet Sci, Columbus, OH 43210 USA. [Ming, D. W.; Morris, R. V.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Ruff, S. W.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [de Souza, P. A.] CSIRO, Informat & Commun Technol Ctr, Hobart, Tas 7001, Australia. RP Arvidson, RE (reprint author), Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. EM arvidson@rsmail.wustl.edu RI de Souza, Paulo/B-8961-2008; Centre, TasICT/D-1212-2011; Catalano, Jeffrey/A-8322-2013; Johnson, Jeffrey/F-3972-2015; OI de Souza, Paulo/0000-0002-0091-8925; Catalano, Jeffrey/0000-0001-9311-977X; Siebach, Kirsten/0000-0002-6628-6297; Greenberger, Rebecca/0000-0003-1583-0261 FU NASA FX We thank the capable team of engineers and scientists at the Jet Propulsion Laboratory and elsewhere who made the Spirit mission possible. We also thank support from NASA for the science team. NR 34 TC 40 Z9 41 U1 1 U2 16 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD SEP 30 PY 2010 VL 115 AR E00F03 DI 10.1029/2010JE003633 PG 19 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 658TF UT WOS:000282511600003 ER PT J AU Yeates, AR Mackay, DH van Ballegooijen, AA Constable, JA AF Yeates, A. R. Mackay, D. H. van Ballegooijen, A. A. Constable, J. A. TI A nonpotential model for the Sun's open magnetic flux SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID CORONAL MASS EJECTIONS; GLOBAL SOLAR CORONA; LONG-TERM VARIATION; ACTIVE-REGION 10953; LARGE-SCALE CORONA; FILAMENT CHANNELS; EVOLUTION MODEL; SOURCE SURFACE; FIELD MODEL; INTERPLANETARY AB Measurements of the interplanetary magnetic field (IMF) over several solar cycles do not agree with computed values of open magnetic flux from potential field extrapolations. The discrepancy becomes greater around solar maximum in each cycle when the IMF can be twice as strong as predicted by the potential field model. Here we demonstrate that this discrepancy may be resolved by allowing for electric currents in the low corona (below 2.5R(circle dot)). We present a quasi-static numerical model of the large-scale coronal magnetic evolution, which systematically produces these currents through flux emergence and shearing by surface motions. The open flux is increased by 75%-85% at solar maximum, but only 25% at solar minimum, bringing it in line with estimates from IMF measurements. The additional open flux in the nonpotential model arises through inflation of the magnetic field by electric currents, with superimposed fluctuations due to coronal mass ejections. The latter are modeled by the self-consistent ejection of twisted magnetic flux ropes. C1 [Yeates, A. R.] Univ Dundee, Div Math, Dundee DD1 4HN, Scotland. [Yeates, A. R.; van Ballegooijen, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Mackay, D. H.; Constable, J. A.] Univ St Andrews, Sch Math & Stat, St Andrews KY16 9SS, Fife, Scotland. RP Yeates, AR (reprint author), Univ Dundee, Div Math, Dundee DD1 4HN, Scotland. EM anthony@maths.dundee.ac.uk; duncan@mcs.st-and.ac.uk RI Yeates, Anthony/D-1338-2014 OI Yeates, Anthony/0000-0002-2728-4053 FU UK/STFC; NASA [NNM07AB07C, NNX08AW53]; Royal Society FX We thank the referees for constructive suggestions. A.R.Y. and D.H.M. acknowledge financial support from the UK/STFC, and A.R.Y. was also supported by NASA contract NNM07AB07C to SAO (where much of this work was undertaken). Simulations used the UKMHD parallel computer in St. Andrews (SRIF/STFC), and support from a Royal Society research grant to D.H.M. The visit of J.A.C. to SAO was supported by NASA grant NNX08AW53. Synoptic magnetogram data from NSO/Kitt Peak were produced cooperatively by NSF/NOAO, NASA/GSFC, and NOAA/SEL and made publicly accessible on the World Wide Web. The OMNI IMF data were obtained from the GSFC/SPDF OMNIWeb interface at http://omniweb.gsfc.nasa.gov. NR 62 TC 22 Z9 22 U1 1 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD SEP 29 PY 2010 VL 115 AR A09112 DI 10.1029/2010JA015611 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 658TU UT WOS:000282513100004 ER PT J AU Liu, CX Liu, Y Cai, ZN Gao, ST Bian, JC Liu, XO Chance, K AF Liu, Chuanxi Liu, Yi Cai, Zhaonan Gao, Shouting Bian, Jianchun Liu, Xiong Chance, Kelly TI Dynamic formation of extreme ozone minimum events over the Tibetan Plateau during northern winters 1987-2001 SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID MADDEN-JULIAN OSCILLATION; TROPOSPHERIC OZONE; LOWER STRATOSPHERE; CLIMATOLOGY; TROPOPAUSE; HEMISPHERE; PACIFIC; HOLES AB Wintertime extreme ozone minima in the total column ozone over the Tibetan Plateau (TP) between 1978 and 2001 are analyzed using observations from the Total Ozone Mapping Spectrometer (TOMS), Global Ozone Monitoring Experiment (GOME), and reanalysis data from both National Centers for Environmental Prediction and European Centre for Medium-Range Weather Forecasts. Results show that total column ozone reduction in nine persistent (lasting for at least 2 days) and four transient events can be substantially attributed to ozone reduction in the upper troposphere and lower stratosphere region (below 25 km). This reduction is generally caused by uplift of the local tropopause and northward transport of tropical ozone-poor air associated with an anomalous anticyclone in the upper troposphere. These anticyclonic anomalies are closely related to anomalous tropical deep convective heating, which is, however, not necessarily phase locked with the tropical Madden-Julian Oscillation as in our earlier case study. Considering stratospheric processes, the selected 13 events can be combined into nine independent events. Moreover, five of the nine independent events, especially the persistent events, are coupled with contributions from stratospheric dynamics between 25 and 40 km, i.e., 15%-40% derived from GOME observations for events in November 1998, February 1999, and December 2001. On the basis of these events, stratospheric column ozone reduction over the TP region can be attributed to the dynamics (development and/or displacement) of the two main stratospheric systems, namely, the polar vortex and the Aleutian High. The effect of a "low-ozone pocket" inside the Aleutian High on the total column ozone in East Asia requires further study. C1 [Liu, Chuanxi; Liu, Yi; Cai, Zhaonan; Bian, Jianchun] Chinese Acad Sci, Inst Atmospher Phys, Key Lab Middle Atmosphere & Global Environm Obser, Beijing 100029, Peoples R China. [Liu, Xiong; Chance, Kelly] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gao, Shouting] Chinese Acad Sci, Inst Atmospher Phys, LACS, Beijing 100029, Peoples R China. [Liu, Xiong] Univ Maryland, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. [Liu, Chuanxi; Cai, Zhaonan] Chinese Acad Sci, Grad Univ, Beijing 100029, Peoples R China. RP Liu, CX (reprint author), Chinese Acad Sci, Inst Atmospher Phys, Key Lab Middle Atmosphere & Global Environm Obser, Beijing 100029, Peoples R China. RI Liu, Xiong/P-7186-2014; OI Liu, Xiong/0000-0003-2939-574X; Chance, Kelly/0000-0002-7339-7577 FU National Basic Research Program of China [2010CB428604]; National Science Foundation of China [40633015]; Dragon 2 Programme [5311]; NASA; Smithsonian Institution FX This work was funded by the National Basic Research Program of China (grant 2010CB428604), National Science Foundation of China (grant 40633015), and the Dragon 2 Programme (ID: 5311). We thank the European Space Agency and the German Aerospace Center for their ongoing cooperation in the GOME program. The meteorological analysis was kindly provided by ECMWF and NCEP. Research at SAO was funded by NASA and the Smithsonian Institution. NR 46 TC 6 Z9 7 U1 0 U2 17 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD SEP 24 PY 2010 VL 115 AR D18311 DI 10.1029/2009JD013130 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 656ID UT WOS:000282321800001 ER PT J AU France, K McCray, R Heng, K Kirshner, RP Challis, P Bouchet, P Crotts, A Dwek, E Fransson, C Garnavich, PM Larsson, J Lawrence, SS Lundqvist, P Panagia, N Pun, CSJ Smith, N Sollerman, J Sonneborn, G Stocke, JT Wang, LF Wheeler, JC AF France, Kevin McCray, Richard Heng, Kevin Kirshner, Robert P. Challis, Peter Bouchet, Patrice Crotts, Arlin Dwek, Eli Fransson, Claes Garnavich, Peter M. Larsson, Josefin Lawrence, Stephen S. Lundqvist, Peter Panagia, Nino Pun, Chun S. J. Smith, Nathan Sollerman, Jesper Sonneborn, George Stocke, John T. Wang, Lifan Wheeler, J. Craig TI Observing Supernova 1987A with the Refurbished Hubble Space Telescope SO SCIENCE LA English DT Article ID BALMER-DOMINATED SHOCKS; SNR 1987A; REVERSE SHOCK; CIRCUMSTELLAR RING; OPTICAL-EMISSION; LINE EMISSION; SN-1987A; ULTRAVIOLET; REMNANTS; NEBULA AB Observations with the Hubble Space Telescope (HST), conducted since 1990, now offer an unprecedented glimpse into fast astrophysical shocks in the young remnant of supernova 1987A. Comparing observations taken in 2010 with the use of the refurbished instruments on HST with data taken in 2004, just before the Space Telescope Imaging Spectrograph failed, we find that the Ly alpha and H alpha lines from shock emission continue to brighten, whereas their maximum velocities continue to decrease. We observe broad, blueshifted Ly alpha, which we attribute to resonant scattering of photons emitted from hot spots on the equatorial ring. We also detect N v lambda lambda 1239, 1243 angstrom line emission, but only to the red of Ly alpha. The profiles of the N v lines differ markedly from that of H alpha, suggesting that the N(4+) ions are scattered and accelerated by turbulent electromagnetic fields that isotropize the ions in the collisionless shock. C1 [Heng, Kevin] ETH, Inst Astron, CH-8093 Zurich, Switzerland. [France, Kevin; Stocke, John T.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [McCray, Richard] Univ Colorado, JILA, Boulder, CO 80309 USA. [Heng, Kevin] Inst Adv Study, Sch Nat Sci, Princeton, NJ 08540 USA. [Kirshner, Robert P.; Challis, Peter] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bouchet, Patrice] Commissariat Energie Atom & Energies Alternat, Serv Astrophys, FR-91191 Gif Sur Yvette, France. [Crotts, Arlin] Columbia Univ, Dept Astron, New York, NY 10027 USA. [Dwek, Eli; Sonneborn, George] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Fransson, Claes; Larsson, Josefin; Sollerman, Jesper] Stockholm Univ, Oskar Klein Ctr, Dept Astron, S-10691 Stockholm, Sweden. [Garnavich, Peter M.] Univ Notre Dame, Notre Dame, IN 46556 USA. [Lawrence, Stephen S.] Hofstra Univ, Dept Phys & Astron, Hempstead, NY 11549 USA. [Panagia, Nino] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Panagia, Nino] Osserv Astrofis Catania, Inst Nazl Astrofis, I-95123 Catania, Italy. [Pun, Chun S. J.] Univ Hong Kong, Dept Phys, Hong Kong, Hong Kong, Peoples R China. [Smith, Nathan] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Wang, Lifan] Texas A&M Univ, Dept Phys & Astron, College Stn, TX USA. [Wheeler, J. Craig] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. RP Heng, K (reprint author), ETH, Inst Astron, Wolfgang Pauli Str 27, CH-8093 Zurich, Switzerland. EM kheng@phys.ethz.ch RI Dwek, Eli/C-3995-2012; Sonneborn, George/D-5255-2012; OI Sollerman, Jesper/0000-0003-1546-6615; /0000-0003-0065-2933 FU Space Telescope Science Institute [GO-11181]; NASA [NAS5-26555] FX K.F. thanks M. Beasley for enjoyable discussions. Support for this research was provided by NASA through grant GO-11181 from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, under NASA contract NAS5-26555. NR 25 TC 12 Z9 12 U1 0 U2 12 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD SEP 24 PY 2010 VL 329 IS 5999 BP 1624 EP 1627 DI 10.1126/science.1192134 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 653NK UT WOS:000282098100034 PM 20813921 ER PT J AU Johnson, WE Onorato, DP Roelke, ME Land, ED Cunningham, M Belden, RC McBride, R Jansen, D Lotz, M Shindle, D Howard, J Wildt, DE Penfold, LM Hostetler, JA Oli, MK O'Brien, SJ AF Johnson, Warren E. Onorato, David P. Roelke, Melody E. Land, E. Darrell Cunningham, Mark Belden, Robert C. McBride, Roy Jansen, Deborah Lotz, Mark Shindle, David Howard, JoGayle Wildt, David E. Penfold, Linda M. Hostetler, Jeffrey A. Oli, Madan K. O'Brien, Stephen J. TI Genetic Restoration of the Florida Panther SO SCIENCE LA English DT Article ID FELIS-CONCOLOR-CORYI; CONSERVATION BIOLOGY; DEPLETION; PUMAS AB The rediscovery of remnant Florida panthers (Puma concolor coryi) in southern Florida swamplands prompted a program to protect and stabilize the population. In 1995, conservation managers translocated eight female pumas (P. c. stanleyana) from Texas to increase depleted genetic diversity, improve population numbers, and reverse indications of inbreeding depression. We have assessed the demographic, population-genetic, and biomedical consequences of this restoration experiment and show that panther numbers increased threefold, genetic heterozygosity doubled, survival and fitness measures improved, and inbreeding correlates declined significantly. Although these results are encouraging, continued habitat loss, persistent inbreeding, infectious agents, and possible habitat saturation pose new dilemmas. This intensive management program illustrates the challenges of maintaining populations of large predators worldwide. C1 [Johnson, Warren E.; O'Brien, Stephen J.] NCI, Lab Genom Divers, Frederick, MD 21702 USA. [Onorato, David P.; Land, E. Darrell; Cunningham, Mark; Lotz, Mark; Shindle, David] Florida Fish & Wildlife Conservat Commiss, Naples, FL 34114 USA. [Roelke, Melody E.] NCI, SAIC Frederick, Lab Genom Divers, Frederick, MD 21702 USA. [Belden, Robert C.] US Fish & Wildlife Serv, Vero Beach, FL 32960 USA. [McBride, Roy] Livestock Protect Co, Alpine, TX 79832 USA. [Jansen, Deborah] Big Cypress Natl Preserve, Ochopee, FL 34141 USA. [Howard, JoGayle; Wildt, David E.] Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. [Penfold, Linda M.] White Oak Conservat Ctr, Yulee, FL 32046 USA. [Hostetler, Jeffrey A.; Oli, Madan K.] Univ Florida, Dept Wildlife Ecol & Conservat, Gainesville, FL 32611 USA. RP Johnson, WE (reprint author), NCI, Lab Genom Divers, Frederick, MD 21702 USA. EM warjohns@mail.nih.gov; Dave.Onorato@MyFWC.com; stephenobrien@nih.gov RI Hostetler, Jeffrey/A-3345-2011; Johnson, Warren/D-4149-2016 OI Hostetler, Jeffrey/0000-0003-3669-1758; Johnson, Warren/0000-0002-5954-186X FU Florida Fish and Wildlife Conservation Commission (FWC); Everglades National Park (EVER); BCNP; U.S. Fish and Wildlife Service; National Cancer Institute, National Institutes of Health (NIH) [N01-CO-12400]; NIH, National Cancer Institute, Center for Cancer Research; Florida Panther Research and Management Trust FX We dedicate this study to the memory of Ulysses Seal and Ernst Mayr, important heroes in the conservation struggle of the Florida panther. Funded by the Florida Fish and Wildlife Conservation Commission (FWC) via purchases of Florida panther license plates. Other major funding for the field work was provided by Everglades National Park (EVER), the BCNP, and federal funds from the U.S. Fish and Wildlife Service (especially in the early years) as well as from the National Cancer Institute, National Institutes of Health (NIH), under contract number N01-CO-12400. This research was supported in part by the Intramural Research Program of NIH, National Cancer Institute, Center for Cancer Research, and the Florida Panther Research and Management Trust Fund. All panther captures, sampling, and radio collaring were authorized by U. S. Fish and Wildlife Service Endangered Species Permits TE01553-3 (FWC) and TE146761-1 (BCNP). We thank many individuals for their help in this project, who are named in SOM reference S25. NR 22 TC 136 Z9 139 U1 34 U2 282 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD SEP 24 PY 2010 VL 329 IS 5999 BP 1641 EP 1645 DI 10.1126/science.1192891 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 653NK UT WOS:000282098100040 PM 20929847 ER PT J AU Robinson, H Skvarla, JJ AF Robinson, Harold Skvarla, John J. TI The restoration of the genus Vernonella Sond. (Vernonieae: Asteraceae) SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article ID POLLEN MORPHOLOGY; COMPOSITAE; WORLD AB Vernonella Sond. is restored as a distinct genus from synonymy under Vernonia and Centrapalus. Included are the type species Vernonella africana and 10 additional species with thinly scarious-margined involucral bracts and distinctive small, short-colpate type A pollen. C1 [Robinson, Harold] Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, Washington, DC 20013 USA. [Skvarla, John J.] Univ Oklahoma, Oklahoma Biol Survey, Dept Bot & Microbiol, Norman, OK 73018 USA. RP Robinson, H (reprint author), Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, MRC 166,POB 37012, Washington, DC 20013 USA. EM robinsoh@si.edu; jskvarla@ou.edu NR 28 TC 4 Z9 5 U1 0 U2 3 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD SEP 23 PY 2010 VL 123 IS 3 BP 181 EP 192 PG 12 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 660UW UT WOS:000282672900001 ER PT J AU Opresko, DM Breedy, O AF Opresko, D. M. Breedy, Odalisca TI A new species of antipatharian coral (Cnidaria: Anthozoa: Antipatharia: Schizopathidae) from the Pacific coast of Costa Rica SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB A new species of antipatharian coral (Anthozoa: Antipatharia) is described from the Pacific coast of Costa Rica. Lillipathes ritamariae, new species, forms large, multi-branched, flabellate colonies that reach a height of 60 cm or more. The genus Lillipathes is characterized by pinnules in four rows and arranged in bilateral alternating pairs. In L. ritamariae, the pinnules occur in only two rows in portions of the corallum; however, the characteristic Lillipathes pinnulation pattern is common enough to support assigning this species to this genus. The species can be distinguished from its cogeners by its very short pinnules (mostly 1-1.5 cm in length) and the development of many of the lateral pinnules into pinnulated branches. In contrast, in L. wingi, the pinnules are up to 5 cm long and only a few in the colony develop into branches. In L. quadribrachiata, the pinnules are up to about 3 cm long, and in Lillipathes lilliei, the pinnules are more than 10 cm in length, and only a small number develop into branches. C1 [Opresko, D. M.] Oak Ridge Natl Lab, Div Environm Sci, Oak Ridge, TN 37831 USA. [Breedy, Odalisca] Smithsonian Trop Res Inst, Balboa, Panama. [Breedy, Odalisca] Univ Costa Rica, Ctr Invest Ciencias Mar & Limnol, San Jose, Costa Rica. [Breedy, Odalisca] Univ Costa Rica, Ctr Invest Estruct Microscopicas, San Jose, Costa Rica. RP Opresko, DM (reprint author), Oak Ridge Natl Lab, Div Environm Sci, POB 2008, Oak Ridge, TN 37831 USA. EM opreskodm@ornl.gov; odalisca.breedy@ucr.ac.cr FU NSF [OCE-0939557]; Smithsonian Institution; Oak Ridge National Laboratory, Oak Ridge, Tennessee FX The first author is especially grateful to Jorge Cortes for his invitation to visit San Jose to study the antipatharian corals in the university collection and for his kind hospitality during that visit. The authors also wish to thank Rita M. Vargas (Museo de Zoologia, University of Costa Rica) for her assistance with the coral collection. Special thanks to Lisa Levin (Chief Scientist), Greg Rouse and Harim Cha (Scripps Institution of Oceanography, University of California at San Diego) for collecting the material and for providing associated information on the specimens and photographs of the colonies in situ and after collection. The specimens were collected as part of research activities conducted under NSF grant OCE-0939557 to Lisa Levin and Greg Rouse. Photomicrographs were prepared in the Scanning Electron Microscopy Laboratories at the CIEMIC, Microscopic Structures Research Centre, University of Costa Rica, San Jose. Thanks also to C. Bright, W. Keel, P. Greenhall, and L. Ward of the National Museum of Natural History, Smithsonian Institution for their assistance during the first author's visit to the Museum Support Center and for processing the type material. The authors appreciate the indepth reviews of the manuscript by T. Molodtsova and a second anonymous reviewer.; This work was supported in part by the Smithsonian Institution; and Oak Ridge National Laboratory, Oak Ridge, Tennessee. D. Opresko is a Research Associate at the National Museum of Natural History, Smithsonian Institution, and gratefully acknowledges that affiliation. NR 7 TC 2 Z9 2 U1 0 U2 2 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD SEP 23 PY 2010 VL 123 IS 3 BP 234 EP 241 PG 8 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 660UW UT WOS:000282672900006 ER PT J AU Micheli, CJ AF Micheli, Charyn J. TI Nomenclatural changes within West Indian Acanthocinini (Coleoptera: Cerambycidae: Lamiinae) SO ZOOTAXA LA English DT Letter C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. RP Micheli, CJ (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, POB 37012,MRC 187, Washington, DC 20013 USA. EM MicheliC@si.edu NR 10 TC 0 Z9 0 U1 0 U2 0 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD SEP 23 PY 2010 IS 2622 BP 65 EP 67 PG 3 WC Zoology SC Zoology GA 657VC UT WOS:000282444900005 ER PT J AU Chen, GX Kirby, K Brickhouse, NS Lin, T Silver, E AF Chen, G. X. Kirby, K. Brickhouse, N. S. Lin, T. Silver, E. TI Reply to "Comment on 'Dirac R-matrix method for the calculation of x-ray line polarization'" SO PHYSICAL REVIEW A LA English DT Letter AB In response to the Comment written by Zhang et al. [Phys. Rev. A 82, 036701 (2010)] we show that the main ideas and results (about the physics and method) reported in our paper [Phys. Rev. A 79, 062715 (2009)] still appear to be correct. Although none of the conjectures given in the Comment about the potential problems in our code are correct, there was a small error in our code, so the part of our paper with numerical data, presented to support our method, appears to be incorrect. The wealth of resonance features in the x-ray line 3D demonstrated in our paper still appears to be real and is reconfirmed by a revised calculation with the error fixed. C1 [Chen, G. X.; Kirby, K.; Brickhouse, N. S.; Lin, T.; Silver, E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Chen, GX (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Brickhouse, Nancy/0000-0002-8704-4473 NR 5 TC 3 Z9 3 U1 0 U2 1 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD SEP 22 PY 2010 VL 82 IS 3 AR 036702 DI 10.1103/PhysRevA.82.036702 PG 2 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 653ML UT WOS:000282095500014 ER PT J AU Vari, RP Zanata, AM Camelier, P AF Vari, Richard P. Zanata, Angela M. Camelier, Priscila TI New Species of Cyphocharax (Ostariophysi: Characiformes: Curimatidae) from the Rio de Contas Drainage, Bahia, Brazil SO COPEIA LA English DT Article AB Cyphocharax pinnilepis, a species of curimatid characiform apparently endemic to the Rio de Contas system in Bahia, Brazil, is described as new. It is only the sixth member of the Curimatidae known from the coastal rivers of Brazil across the expanse from south of the mouth of the Amazon River to the state of Sao Paulo, but the third curimatid species from the Rio de Contas. The basis for the assignment of the species to Cyphocharax is discussed, and it is diagnosed from congeners on details of pigmentation, the pattern of scales on the lobes of the caudal fin, meristics, and morphometrics. C1 [Vari, Richard P.] Smithsonian Inst, Div Fishes, Dept Vertebrate Zool, Natl Museum Nat Hist, Washington, DC 20013 USA. [Zanata, Angela M.; Camelier, Priscila] Univ Fed Bahia, Dept Zool, Inst Biol, BR-40170290 Salvador, BA, Brazil. RP Vari, RP (reprint author), Smithsonian Inst, Div Fishes, Dept Vertebrate Zool, Natl Museum Nat Hist, MRC-159,POB 37012, Washington, DC 20013 USA. EM varir@si.edu; a_zanata@yahoo.com.br; pricamelier@yahoo.com.br FU Herbert R. and Evelyn Axelrod Chair in Systematic Ichthyology in the Division of Fishes; National Museum of Natural History of the Smithsonian Institution; Conselho Nacional de Desenvolvimento Cientifico e Tecnologico FX Support for this project was provided by the Herbert R. and Evelyn Axelrod Chair in Systematic Ichthyology in the Division of Fishes, National Museum of Natural History of the Smithsonian Institution (RPV) and Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (AMZ). E. Baena (MZUSP) assisted with the photography of the holotype, S. Raredon (USNM) with radiography of portions of the type series, and L. Sousa (MZUSP) with the map. R. Burger, A. Goes, and T. Carvalho (all UFBA) participated in the fieldwork that yielded the samples that served as the basis for this paper. P. Carvalho (MZUSP) collected and made available a portion of the paratype series. We thank O. Oyakawa (MZUSP) for the loan of comparative specimens. NR 13 TC 11 Z9 11 U1 0 U2 5 PU AMER SOC ICHTHYOLOGISTS & HERPETOLOGISTS PI MIAMI PA MAUREEN DONNELLY, SECRETARY FLORIDA INT UNIV BIOLOGICAL SCIENCES, 11200 SW 8TH STREET, MIAMI, FL 33199 USA SN 0045-8511 EI 1938-5110 J9 COPEIA JI Copeia PD SEP 21 PY 2010 IS 3 BP 382 EP 387 DI 10.1643/CI-09-140 PG 6 WC Zoology SC Zoology GA 655PL UT WOS:000282261800004 ER PT J AU Reece, JS Smith, DG Holm, E AF Reece, Joshua S. Smith, David G. Holm, Erling TI The Moray Eels of the Anarchias cantonensis Group (Anguilliformes: Muraenidae), with Description of Two New Species SO COPEIA LA English DT Article ID HAWAIIAN-ISLANDS; LINE ISLANDS; K-AR; PACIFIC-OCEAN; INDIAN-OCEAN; EVOLUTION; GEOLOGY; AGE; PHILIPPINES; VOLCANISM AB The broadly distributed Indo-Pacific moray eel Anarchlas cantonensis (Schultz, 1943), heretofore treated as a single species, consists of three species: A. cantonensis, A. exulatus, a new species, and A. schultzi, a new species, based on geographic distribution, coloration, external morphometrics, and vertebral counts. We examined 112 specimens and determined that the true A. cantonensis is distributed throughout the eastern Indian Ocean, western Pacific, and tropical central Pacific, and has a mean vertebral formula of 91/93/104. Anarchlas exulatus is distributed anti-tropically in the central and southeastern Pacific and is characterized by a unique mottling pattern and a mean vertebral formula of 100/103/114. A third species, named here as A. schultzi, is characterized by a mean vertebral formula of 96/99/109, a plain brown coloration in adult form, and is restricted geographically to Tonga, New Caledonia, the Solomon Islands, and the Caroline Islands. At the Tonga Islands, which reside on the edge of Australian and Pacific tectonic plates, all three species are present, but maintain their morphological distinctiveness and segregate ecologically. C1 [Reece, Joshua S.] Washington Univ, Dept Biol, St Louis, MO 63130 USA. [Smith, David G.] Museum Support Ctr MRC 534, Div Fishes, Smithsonian Inst, Suitland, MA 20746 USA. [Holm, Erling] Royal Ontario Museum, Dept Nat Hist, Toronto, ON M5S 2C6, Canada. RP Reece, JS (reprint author), Washington Univ, Dept Biol, Box 1137,1 Brookings Dr, St Louis, MO 63130 USA. EM jsreece@wustl.edu; smithd@si.edu; erlingh@rom.on.ca FU Society of Systematic Biologists; DeepFin Fish Phylogeny Project; Smithsonian Institution; Washington University in Saint Louis; AMS; ANSP; BPBM; FMNH; SIO FX Funding for this research was provided by grants to JSR by the Society of Systematic Biologists Mini-PEET Award and the DeepFin Fish Phylogeny Project. Institutional support was provided by the Smithsonian Institution and Washington University in Saint Louis. We thank the following for loan of specimens: M. McGrouther (AMS), M. Sabaj-Perez (ANSP), A. Suzumoto (BPBM), M. Rogers (FMNH), H. Walker (SIO). NR 37 TC 5 Z9 7 U1 0 U2 7 PU AMER SOC ICHTHYOLOGISTS HERPETOLOGISTS PI CHARLESTON PA UNIV CHARLESTON, GRICE MARINE LABORATORY, 205 FORT JOHNSON RD, CHARLESTON, SC 29412 USA SN 0045-8511 J9 COPEIA JI Copeia PD SEP 21 PY 2010 IS 3 BP 421 EP 430 DI 10.1643/CI-09-189 PG 10 WC Zoology SC Zoology GA 655PL UT WOS:000282261800009 ER PT J AU Narayanan, D Dey, A Hayward, CC Cox, TJ Bussmann, RS Brodwin, M Jonsson, P Hopkins, PF Groves, B Younger, JD Hernquist, L AF Narayanan, Desika Dey, Arjun Hayward, Christopher C. Cox, Thomas J. Bussmann, R. Shane Brodwin, Mark Jonsson, Patrik Hopkins, Philip F. Groves, Brent Younger, Joshua D. Hernquist, Lars TI A physical model for z similar to 2 dust-obscured galaxies SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE dust, extinction; galaxies: formation; galaxies: high-redshift; galaxies: ISM; galaxies: starburst; cosmology: theory ID ACTIVE GALACTIC NUCLEI; STAR-FORMING GALAXIES; ULTRALUMINOUS INFRARED GALAXIES; SPECTRAL ENERGY-DISTRIBUTION; REDSHIFT SUBMILLIMETER GALAXIES; SUPERMASSIVE BLACK-HOLES; PARTICLE HYDRODYNAMICS SIMULATIONS; SPITZER MIDINFRARED SPECTROSCOPY; POLYCYCLIC AROMATIC-HYDROCARBON; STELLAR MASS DENSITY AB We present a physical model for the origin of z similar to 2 dust-obscured galaxies (DOGs), a class of high-redshift ultraluminous infrared galaxies (ULIRGs) selected at 24 mu m which are particularly optically faint (F(24 mu m)/F(R) > 1000). By combining N-body/smoothed particle hydrodynamic simulations of high-redshift galaxy evolution with 3D polychromatic dust radiative transfer models, we find that luminous DOGs (with F(24) greater than or similar to 0.3mJy at z similar to 2) are well modelled as extreme gas-rich mergers in massive (similar to 5 x 10(12)-10(13) M(circle dot)) haloes, with elevated star formation rates (SFR; similar to 500-1000M(circle dot)yr(-1)) and/or significant active galactic nuclei (AGN) growth (M BH greater than or similar to 0.5M(circle dot) yr(-1)), whereas less luminous DOGs are more diverse in nature. At final coalescence, merger-driven DOGs transition from being starburst dominated to AGN dominated, evolving from a 'bump' to a power-law (PL) shaped mid-IR (Infrared Array Camera, IRAC) spectral energy distribution (SED). After the DOG phase, the galaxy settles back to exhibiting a 'bump' SED with bluer colours and lower SFRs. While canonically PL galaxies are associated with being AGN dominated, we find that the PL mid-IR SED can owe both to direct AGN contribution and to a heavily dust obscured stellar bump at times that the galaxy is starburst dominated. Thus, PL galaxies can be either starburst or AGN dominated. Less luminous DOGs can be well-represented either by mergers or by massive (M(baryon) similar to 5 x 10(11)M(circle dot)) secularly evolving gas-rich disc galaxies (with SFR similar to 50M(circle dot) yr(-1)). By utilizing similar models as those employed in the submillimetre galaxy (SMG) formation study of Narayanan et al., we investigate the connection between DOGs and SMGs. We find that the most heavily star-forming merger-driven DOGs can be selected as submillimetre galaxies, while both merger-driven and secularly evolving DOGs typically satisfy the BzK selection criteria. The model SEDs from the simulated galaxies match observed data reasonably well, though Mrk 231 and Arp 220 templates provide worse matches. Our models provide testable predictions of the physical masses, dust temperatures, CO linewidths and location on the MBH-Mbulge relation of DOGs. Finally, we provide public SED templates derived from these simulations. C1 [Narayanan, Desika; Hayward, Christopher C.; Cox, Thomas J.; Brodwin, Mark; Younger, Joshua D.; Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Dey, Arjun] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Cox, Thomas J.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [Bussmann, R. Shane] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Jonsson, Patrik] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Hopkins, Philip F.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Hopkins, Philip F.] Univ Calif Berkeley, Theoret Astrophys Ctr, Berkeley, CA 94720 USA. [Groves, Brent] Leiden Univ, Sterrewacht Leiden, NL-233 CA Leiden, Netherlands. [Younger, Joshua D.] Inst Adv Study, Princeton, NJ 08544 USA. RP Narayanan, D (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM dnarayanan@cfa.harvard.edu RI Hayward, Christopher/I-4756-2012 OI Hayward, Christopher/0000-0003-4073-3236 FU W. M. Keck Foundation [GO10890]; AURA [NAS5-26555, HST-AR-10678, 10958] FX We are grateful to Ranga-Ram Chary, Vandana Desai, Brandon Kelly, Kai Noeske, Jason Melbourne and Alex Pope for helpful conversations. DN thanks the NOAO in Tucson for hospitality, where part of this study was conducted. The authors are grateful to the W. M. Keck Foundation for hosting the Napa Galaxy Evolution workshop where the ideas for much of this project came about. AD is supported byNOAO, which is operated by the Association ofUniversities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. CCH was funded by an NSF Graduate Research Fellowship. TC and MB acknowledge support from the W. M. Keck Foundation. RSB acknowledges financial assistance from HST grant GO10890, which is provided by NASA through a grant from the Space Telescope Science Institute which is operated by AURA under NASA contract NAS5-26555. PJ was supported by programsHST-AR-10678 and 10958, 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, and by Spitzer Theory Grant 30183 from the Jet Propulsion Laboratory. Support for PFH was provided by the Miller Institute for Basic Research in Science, University of California, Berkeley. The simulations in this paper were run on the Odyssey cluster supported by the Harvard FAS Research Computing Group. NR 149 TC 77 Z9 77 U1 0 U2 1 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD SEP 21 PY 2010 VL 407 IS 3 BP 1701 EP 1720 DI 10.1111/j.1365-2966.2010.16997.x PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 649TX UT WOS:000281797900022 ER PT J AU Bloemen, S Marsh, TR Steeghs, D Ostensen, RH AF Bloemen, S. Marsh, T. R. Steeghs, D. Ostensen, R. H. TI Spin-resolved spectroscopy of the intermediate polar DQ Her SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; binaries: close; binaries: eclipsing; stars: individual: DQ Herculis; novae, cataclysmic variables ID RAPID LIGHT VARIATIONS; 71 2ND OSCILLATION; OLD NOVA DQ; ACCRETION DISKS; CATACLYSMIC VARIABLES; HERCULIS 1934; DOPPLER TOMOGRAPHY; SPIRAL STRUCTURE; BINARY-SYSTEMS; SPACED DATA AB We present high-speed spectroscopic observations of the intermediate polar (IP) DQ Herculis. Doppler tomography of two He I lines reveals a spiral density structure in the accretion disc around the white dwarf (WD) primary. The spirals look very similar to the spirals seen in dwarf novae during outburst. DQ Her is the first well-established IP in which spirals are seen, which are in addition likely persistent because of the system's high mass transfer rate. Spiral structures give an alternative explanation for sidebands of the WD spin frequency that are found in IP light curves. The Doppler tomogram of He II lambda 4686 indicates that a large part of the emission is not disc-like. Spin trails of spectra reveal a pulsation in the He II lambda 4686 emission that is believed to result from reprocessing of X-rays from the WD's magnetic poles in the accretion flow close to the WD. We confirm the previous finding that the pulsation is only visible in the redshifted part of the line when the beam points to the back side of the disc. The absence of reprocessed light from the front side of the disc can be explained by obscuration by the front rim of the disc, but the absence of extra emission from the blueshifted back side of the disc is puzzling. Reprocessing in accretion curtains can be an answer to the problem and can also explain the highly non-Keplerian velocity components that are found in the He II lambda 4686 line. Our spin trails can form a strong test for future accretion curtain models, with the possibility of distinguishing between a spin period of 71 or 142 s. Spin trails of data taken at selected orbital phases show little evidence for a significant contribution of the bright spot to the pulsations and allow us to exclude a recent suggestion that 71 s is the beat period and 70.8 s the spin period. C1 [Bloemen, S.; Ostensen, R. H.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Leuven, Belgium. [Marsh, T. R.; Steeghs, D.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Steeghs, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Bloemen, S (reprint author), Katholieke Univ Leuven, Inst Sterrenkunde, Celestijnenlaan 200D, B-3001 Leuven, Belgium. EM steven.bloemen@ster.kuleuven.be RI Steeghs, Danny/C-5468-2009 OI Steeghs, Danny/0000-0003-0771-4746 FU European Research Council under the European Community [227224]; Research Council of K. U. Leuven [GOA/2008/04]; UK's Science and Technology Facilities Council (STFC) [ST/F002599/1, PP/D005914/1] FX The research leading to these results has received funding from the European Research Council under the European Community's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement No. 227224 (PROSPERITY), as well as from the Research Council of K. U. Leuven grant agreement GOA/2008/04. During this research TRM and DS were supported under grants from the UK's Science and Technology Facilities Council (STFC; ST/F002599/1 and PP/D005914/1). NR 49 TC 8 Z9 8 U1 0 U2 1 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD SEP 21 PY 2010 VL 407 IS 3 BP 1903 EP 1912 DI 10.1111/j.1365-2966.2010.17035.x PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 649TX UT WOS:000281797900040 ER PT J AU Chen, HX Strand, M Norenburg, JL Sun, SC Kajihara, H Chernyshev, AV Maslakova, SA Sundberg, P AF Chen, Haixia Strand, Malin Norenburg, Jon L. Sun, Shichun Kajihara, Hiroshi Chernyshev, Alexey V. Maslakova, Svetlana A. Sundberg, Per TI Statistical Parsimony Networks and Species Assemblages in Cephalotrichid Nemerteans (Nemertea) SO PLOS ONE LA English DT Article ID PHYLUM NEMERTEA; DNA TAXONOMY; SEQUENCES; ARCHINEMERTEA; DELIMITATION; PHYLOGENY; INTERFACE; CHECKLIST; ANOPLA; GENERA AB Background: It has been suggested that statistical parsimony network analysis could be used to get an indication of species represented in a set of nucleotide data, and the approach has been used to discuss species boundaries in some taxa. Methodology/Principal Findings: Based on 635 base pairs of the mitochondrial protein-coding gene cytochrome c oxidase I (COI), we analyzed 152 nemertean specimens using statistical parsimony network analysis with the connection probability set to 95%. The analysis revealed 15 distinct networks together with seven singletons. Statistical parsimony yielded three networks supporting the species status of Cephalothrix rufifrons, C. major and C. spiralis as they currently have been delineated by morphological characters and geographical location. Many other networks contained haplotypes from nearby geographical locations. Cladistic structure by maximum likelihood analysis overall supported the network analysis, but indicated a false positive result where subnetworks should have been connected into one network/species. This probably is caused by undersampling of the intraspecific haplotype diversity. Conclusions/Significance: Statistical parsimony network analysis provides a rapid and useful tool for detecting possible undescribed/cryptic species among cephalotrichid nemerteans based on COI gene. It should be combined with phylogenetic analysis to get indications of false positive results, i.e., subnetworks that would have been connected with more extensive haplotype sampling. C1 [Chen, Haixia; Sun, Shichun] Ocean Univ China, Inst Evolut & Marine Biodivers, Qingdao, Peoples R China. [Chen, Haixia; Sundberg, Per] Univ Gothenburg, Dept Zool, Gothenburg, Sweden. [Strand, Malin] Sven Loven Ctr Marine Sci, Tjarno, Sweden. [Norenburg, Jon L.] Smithsonian Inst, Dept Invertebrate Zool, Natl Museum Nat Hist, Washington, DC 20560 USA. [Kajihara, Hiroshi] Hokkaido Univ, Fac Sci, Dept Nat Hist Sci, Sapporo, Hokkaido 060, Japan. [Chernyshev, Alexey V.] Russian Acad Sci, Far E Div, AV Zhirmunsky Inst Marine Biol, Vladivostok 690022, Russia. [Maslakova, Svetlana A.] Univ Oregon, Oregon Inst Marine Biol, Charleston, OR USA. RP Chen, HX (reprint author), Ocean Univ China, Inst Evolut & Marine Biodivers, Qingdao, Peoples R China. EM p.sundberg@zool.gu.se RI Kajihara, Hiroshi/A-8822-2012; Norenburg, Jon/K-3481-2015 OI Norenburg, Jon/0000-0001-7776-1527 FU National Natural Science Foundation of China [30970333]; Swedish Research Council; Research Institute of Marine Invertebrates, Japan [FY2008]; NSF [DEB 9712463]; Smithsonian Institution FX The study was supported by the National Natural Science Foundation of China (30970333 to SCS), the Swedish Research Council (to PS), the Research Institute of Marine Invertebrates, Japan (FY2008, No. 14 to HK), NSF PEET award (DEB 9712463 to JLN) and various funds from the Smithsonian Institution. This publication represents contribution 817 of the Smithsonian Marine Station at Fort Pierce, Florida and 891 of the Smithsonian Caribbean Coral Reef Ecosystem program in Belize. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 43 TC 35 Z9 37 U1 0 U2 9 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 185 BERRY ST, STE 1300, SAN FRANCISCO, CA 94107 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD SEP 21 PY 2010 VL 5 IS 9 AR e12885 DI 10.1371/journal.pone.0012885 PG 7 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 652JO UT WOS:000282002900017 PM 20877627 ER PT J AU Greene, JE Peng, CY Kim, MJ Kuo, CY Braatz, JA Impellizzeri, CMV Condon, JJ Lo, KY Henkel, C Reid, MJ AF Greene, Jenny E. Peng, Chien Y. Kim, Minjin Kuo, Cheng-Yu Braatz, James A. Impellizzeri, C. M. Violette Condon, James J. Lo, K. Y. Henkel, Christian Reid, Mark J. TI PRECISE BLACK HOLE MASSES FROM MEGAMASER DISKS: BLACK HOLE-BULGE RELATIONS AT LOW MASS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: bulges; galaxies: nuclei; galaxies: Seyfert ID ACTIVE GALACTIC NUCLEI; EARLY-TYPE GALAXIES; DIGITAL SKY SURVEY; AGN MONITORING PROJECT; LATE-TYPE SPIRALS; VELOCITY DISPERSION CORRELATION; DWARF SEYFERT NUCLEI; BROAD-LINE REGION; BH-SIGMA RELATION; ACCRETION DISK AB The black hole (BH)-bulge correlations have greatly influenced the last decade of efforts to understand galaxy evolution. Current knowledge of these correlations is limited predominantly to high BH masses (M(BH) greater than or similar to 10(8) M(circle dot)) that can be measured using direct stellar, gas, and maser kinematics. These objects, however, do not represent the demographics of more typical L < L* galaxies. This study transcends prior limitations to probe BHs that are an order of magnitude lower in mass, using BH mass measurements derived from the dynamics of H(2)O megamasers in circumnuclear disks. The masers trace the Keplerian rotation of circumnuclear molecular disks starting at radii of a few tenths of a pc from the central BH. Modeling of the rotation curves, presented by Kuo et al., yields BH masses with exquisite precision. We present stellar velocity dispersion measurements for a sample of nine megamaser disk galaxies based on long-slit observations using the B&C spectrograph on the Dupont telescope and the Dual Imaging Spectrograph on the 3.5 m telescope at Apache Point. We also perform bulge-to-disk decomposition of a subset of five of these galaxies with Sloan Digital Sky Survey imaging. The maser galaxies as a group fall below the M(BH)-sigma(*) relation defined by elliptical galaxies. We show, now with very precise BH mass measurements, that the low-scatter power-law relation between M(BH) and sigma(*) seen in elliptical galaxies is not universal. The elliptical galaxy M(BH)-sigma* relation cannot be used to derive the BH mass function at low mass or the zero point for active BH masses. The processes (perhaps BH self-regulation or minor merging) that operate at higher mass have not effectively established an M(BH)-sigma* relation in this low-mass regime. C1 [Greene, Jenny E.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Peng, Chien Y.] NRC Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Kim, Minjin; Kuo, Cheng-Yu; Braatz, James A.; Impellizzeri, C. M. Violette; Condon, James J.; Lo, K. Y.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Henkel, Christian] Max Planck Inst Radio Astron, Bonn, Germany. [Reid, Mark J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Greene, JE (reprint author), Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. FU National Aeronautics and Space Administration; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England; American Museum of Natural History; Astrophysical Institute Potsdam; University of Basel; University of Cambridge; Case Western Reserve University; University of Chicago; Drexel University; Fermilab; Institute for Advanced Study; Japan Participation Group; Johns Hopkins University; Joint Institute for Nuclear Astrophysics; Kavli Institute for Particle Astrophysics and Cosmology; Korean Scientist Group; Chinese Academy of Sciences; 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 Many people have contributed substantively to our thinking in the writing of this paper. We first thank the referee for a very prompt and thorough report. We gratefully acknowledge useful conversations with A. Barth, L. Ho, J. Kormendy, G. van de Venn, and N. Drory. P. Erwin and J. Mulchaey both provided optical images of various galaxies presented here and K. Gultekin assisted in our implementation of his fitting methodology. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. We further acknowledge the usage of the HyperLeda database (http://leda.univ-lyon1.fr). Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web Site is http://www.sdss.org/. The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington. NR 172 TC 121 Z9 122 U1 1 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 2010 VL 721 IS 1 BP 26 EP 45 DI 10.1088/0004-637X/721/1/26 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 654TI UT WOS:000282192900002 ER PT J AU Cohen, O Drake, JJ Kashyap, VL Hussain, GAJ Gombosi, TI AF Cohen, O. Drake, J. J. Kashyap, V. L. Hussain, G. A. J. Gombosi, T. I. TI THE CORONAL STRUCTURE OF AB DORADUS SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: activity; stars: coronae; stars: magnetic field ID ANGULAR-MOMENTUM LOSS; X-RAY SPECTROSCOPY; SOLAR-TYPE STARS; MAGNETIC-FIELD; DIFFERENTIAL ROTATION; POLYTROPIC INDEX; STELLAR WINDS; EVOLUTION; MODELS; DOR AB We perform a numerical simulation of the corona of the young, rapidly rotating K0 dwarf AB Doradus using a global magnetohydrodynamic (MHD) model. The model is driven by a surface map of the radial magnetic field constructed using Zeeman-Doppler Imaging. We find that the global structure of the stellar corona is dominated by strong azimuthal tangling of the magnetic field due to the rapid rotation. The MHD solution enables us to calculate realistic Alfven surfaces, and we can therefore estimate the stellar mass loss rate and angular momentum loss rate without making undue theoretical simplifications. We consider three cases, parameterized by the base density of the corona, that span the range of possible solutions for the system. We find that overall the mass and angular momentum loss rates are higher than in the solar case; the mass loss rates are 10-500 times higher, and the angular momentum loss rate can be up to 3 x 10(4) higher than present-day solar values. Our simulations show that this model can be used to constrain the wide parameter space of stellar systems. It also shows that an MHD approach can provide more information about the physical system over the commonly used potential field extrapolation. C1 [Cohen, O.; Drake, J. J.; Kashyap, V. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hussain, G. A. J.] ESO, D-85748 Garching, Germany. [Gombosi, T. I.] Univ Michigan, Ctr Space Environm Modeling, Ann Arbor, MI 48109 USA. RP Cohen, O (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Gombosi, Tamas/G-4238-2011; OI Gombosi, Tamas/0000-0001-9360-4951; Cohen, Ofer/0000-0003-3721-0215 FU SHINE through NSF [ATM-0823592]; NASA [NNG05GM44G, NAS8-39073]; NSF FX We thank to an unknown referee for his/her useful comments. O.C. is supported by SHINE through NSF ATM-0823592 grant, and by NASA-LWSTRT Grant NNG05GM44G. J.J.D. and V. L. K. were funded by NASA contract NAS8-39073 to the Chandra X-ray Center. Simulation results were obtained using the Space Weather Modeling Framework, developed by the Center for Space Environment Modeling, at the University of Michigan with funding support from NASA ESS, NASA ESTO-CT, NSF KDI, and DoD MURI. NR 57 TC 19 Z9 19 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 2010 VL 721 IS 1 BP 80 EP 89 DI 10.1088/0004-637X/721/1/80 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 654TI UT WOS:000282192900006 ER PT J AU Brodwin, M Ruel, J Ade, PAR Aird, KA Andersson, K Ashby, MLN Bautz, M Bazin, G Benson, BA Bleem, LE Carlstrom, JE Chang, CL Crawford, TM Crites, AT De Haan, T Desai, S Dobbs, MA Dudley, JP Fazio, GG Foley, RJ Forman, WR Garmire, G George, EM Gladders, MD Gonzalez, AH Halverson, NW High, FW Holder, GP Holzapfel, WL Hrubes, JD Jones, C Joy, M Keisler, R Knox, L Lee, AT Leitch, EM Lueker, M Marrone, DP McMahon, JJ Mehl, J Meyer, SS Mohr, JJ Montroy, TE Murray, SS Padin, S Plagge, T Pryke, C Reichardt, CL Rest, A Ruhl, JE Schaffer, KK Shaw, L Shirokoff, E Song, J Spieler, HG Stalder, B Stanford, SA Staniszewski, Z Stark, AA Stubbs, CW Vanderlinde, K Vieira, JD Vikhlinin, A Williamson, R Yang, Y Zahn, O Zenteno, A AF Brodwin, M. Ruel, J. Ade, P. A. R. Aird, K. A. Andersson, K. Ashby, M. L. N. Bautz, M. Bazin, G. Benson, B. A. Bleem, L. E. Carlstrom, J. E. Chang, C. L. Crawford, T. M. Crites, A. T. De Haan, T. Desai, S. Dobbs, M. A. Dudley, J. P. Fazio, G. G. Foley, R. J. Forman, W. R. Garmire, G. George, E. M. Gladders, M. D. Gonzalez, A. H. Halverson, N. W. High, F. W. Holder, G. P. Holzapfel, W. L. Hrubes, J. D. Jones, C. Joy, M. Keisler, R. Knox, L. Lee, A. T. Leitch, E. M. Lueker, M. Marrone, D. P. McMahon, J. J. Mehl, J. Meyer, S. S. Mohr, J. J. Montroy, T. E. Murray, S. S. Padin, S. Plagge, T. Pryke, C. Reichardt, C. L. Rest, A. Ruhl, J. E. Schaffer, K. K. Shaw, L. Shirokoff, E. Song, J. Spieler, H. G. Stalder, B. Stanford, S. A. Staniszewski, Z. Stark, A. A. Stubbs, C. W. Vanderlinde, K. Vieira, J. D. Vikhlinin, A. Williamson, R. Yang, Y. Zahn, O. Zenteno, A. TI SPT-CL J0546-5345: A MASSIVE z > 1 GALAXY CLUSTER SELECTED VIA THE SUNYAEV-ZEL'DOVICH EFFECT WITH THE SOUTH POLE TELESCOPE SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: individual (SPT-CL J0546-5345); galaxies: distances and redshifts; galaxies: evolution ID IRAC SHALLOW SURVEY; X-RAY; VELOCITY DISPERSIONS; PHOTOMETRIC REDSHIFTS; TEMPERATURE RELATION; COSMOLOGY; CHANDRA; PROFILES; SAMPLE; GAS AB We report the spectroscopic confirmation of SPT-CL J0546-5345 at < z > = 1.067. To date this is the most distant cluster to be spectroscopically confirmed from the 2008 South Pole Telescope (SPT) catalog, and indeed the first z > 1 cluster discovered by the Sunyaev-Zel'dovich Effect (SZE). We identify 21 secure spectroscopic members within 0.9 Mpc of the SPT cluster position, 18 of which are quiescent, early-type galaxies. From these quiescent galaxies we obtain a velocity dispersion of 1179-(+232)(167) km s(-1), ranking SPT-CL J0546-5345 as the most dynamically massive cluster yet discovered at z > 1. Assuming that SPT-CL J0546-5345 is virialized, this implies a dynamical mass of M(200) = 1.0(-0.4)(+0.6) x 10(15) M(circle dot), in agreement with the X-ray and SZE mass measurements. Combining masses from several independent measures leads to a best-estimate mass of M(200) = (7.95 +/- 0.92) x 10(14) M(circle dot). The spectroscopic confirmation of SPT-CL J0546-5345, discovered in the wide-angle, mass-selected SPT cluster survey, marks the onset of the high-redshift SZE-selected galaxy cluster era. C1 [Brodwin, M.; Ashby, M. L. N.; Fazio, G. G.; Foley, R. J.; Forman, W. R.; Jones, C.; Murray, S. S.; Stalder, B.; Stark, A. A.; Stubbs, C. W.; Vikhlinin, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ruel, J.; High, F. W.; Rest, A.; Stubbs, C. W.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Ade, P. A. R.] Cardiff Univ, Dept Phys & Astron, Cardiff CF24 3YB, S Glam, Wales. [Aird, K. A.; Hrubes, J. D.; Marrone, D. P.] Univ Chicago, Chicago, IL 60637 USA. [Andersson, K.; Bautz, M.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Bazin, G.; Mohr, J. J.; Zenteno, A.] Univ Munich, Dept Phys, D-81679 Munich, Germany. [Bazin, G.; Mohr, J. J.; Zenteno, A.] Excellence Cluster Univ, D-85758 Garching, Germany. [Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; Keisler, R.; Leitch, E. M.; Marrone, D. P.; McMahon, J. J.; Mehl, J.; Meyer, S. S.; Padin, S.; Pryke, C.; Schaffer, K. K.; Vieira, J. D.; Williamson, R.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Benson, B. A.; Carlstrom, J. E.; Chang, C. L.; McMahon, J. J.; Meyer, S. S.; Pryke, C.; Schaffer, K. K.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Bleem, L. E.; Carlstrom, J. E.; Keisler, R.; Meyer, S. S.; Vieira, J. D.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. [Carlstrom, J. E.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; Leitch, E. M.; Mehl, J.; Meyer, S. S.; Padin, S.; Plagge, T.; Pryke, C.; Williamson, R.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [De Haan, T.; Dobbs, M. A.; Dudley, J. P.; Holder, G. P.; Shaw, L.; Vanderlinde, K.] McGill Univ, Dept Phys, Quebec City, PQ H3A 2T8, Canada. [Desai, S.; Song, J.; Yang, Y.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Garmire, G.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [George, E. M.; Holzapfel, W. L.; Lee, A. T.; Lueker, M.; Plagge, T.; Reichardt, C. L.; Shirokoff, E.; Zahn, O.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Gonzalez, A. H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Halverson, N. W.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Halverson, N. W.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA. [Joy, M.] NASA Marshall Space Flight Ctr, Dept Space Sci, Huntsville, AL 35812 USA. [Knox, L.; Stanford, S. A.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Lee, A. T.; Spieler, H. G.] Univ Calif Berkeley, Lawrence Berkeley Lab, Div Phys, Berkeley, CA 94720 USA. [McMahon, J. J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Mohr, J. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Montroy, T. E.; Ruhl, J. E.; Staniszewski, Z.] Case Western Reserve Univ, Dept Phys, Cleveland, OH 44106 USA. [Montroy, T. E.; Ruhl, J. E.; Staniszewski, Z.] Case Western Reserve Univ, CERCA, Cleveland, OH 44106 USA. [Shaw, L.] Yale Univ, Dept Phys, New Haven, CT 06520 USA. RP Brodwin, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Stubbs, Christopher/C-2829-2012; Williamson, Ross/H-1734-2015; Holzapfel, William/I-4836-2015; OI Stark, Antony/0000-0002-2718-9996; Stubbs, Christopher/0000-0003-0347-1724; Williamson, Ross/0000-0002-6945-2975; Aird, Kenneth/0000-0003-1441-9518; Reichardt, Christian/0000-0003-2226-9169 FU National Science Foundation [ANT-0638937]; NSF Physics Frontier Center [PHY-0114422]; Kavli Foundation; Gordon and Betty Moore Foundation; NASA; Chandra Xray Observatory [SV4-74018, A31]; W. M. Keck Foundation; Brinson Foundation FX Visiting astronomer, Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, under contract with the National Science Foundation; The SPT is supported by the National Science Foundation through grant ANT-0638937. Partial support is also provided by the NSF Physics Frontier Center grant PHY-0114422 to the Kavli Institute of Cosmological Physics at the University of Chicago, the Kavli Foundation, and the Gordon and Betty Moore Foundation. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. This paper includes data gathered with the 6.5 meter Magellan Telescopes located at Las Campanas Observatory, Chile. This work is based in part on observations obtained with the Chandra Xray Observatory, under contract SV4-74018, A31 with the Smithsonian Astrophysical Observatory which operates the Chandra for NASA. We are very grateful for the efforts of the Spitzer, Chandra, Magellan, and CTIO support staff without whom this paper would not be possible. Support for M. B. was provided by the W. M. Keck Foundation. B. S. acknowledges support from the Brinson Foundation. NR 60 TC 74 Z9 75 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 2010 VL 721 IS 1 BP 90 EP 97 DI 10.1088/0004-637X/721/1/90 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 654TI UT WOS:000282192900007 ER PT J AU Kartaltepe, JS Sanders, DB Le Floc'h, E Frayer, DT Aussel, H Arnouts, S Ilbert, O Salvato, M Scoville, NZ Surace, J Yan, L Capak, P Caputi, K Carollo, CM Cassata, P Civano, F Hasinger, G Koekemoer, AM Le Fevre, O Lilly, S Liu, CT McCracken, HJ Schinnerer, E Smolcic, V Taniguchi, Y Thompson, DJ Trump, J Baldassare, VF Fiorenza, SL AF Kartaltepe, Jeyhan S. Sanders, D. B. Le Floc'h, E. Frayer, D. T. Aussel, H. Arnouts, S. Ilbert, O. Salvato, M. Scoville, N. Z. Surace, J. Yan, L. Capak, P. Caputi, K. Carollo, C. M. Cassata, P. Civano, F. Hasinger, G. Koekemoer, A. M. Le Fevre, O. Lilly, S. Liu, C. T. McCracken, H. J. Schinnerer, E. Smolcic, V. Taniguchi, Y. Thompson, D. J. Trump, J. Baldassare, V. F. Fiorenza, S. L. TI A MULTIWAVELENGTH STUDY OF A SAMPLE OF 70 mu m SELECTED GALAXIES IN THE COSMOS FIELD. II. THE ROLE OF MERGERS IN GALAXY EVOLUTION SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; galaxies: active; galaxies: evolution; galaxies: high-redshift; infrared: galaxies; surveys ID ACTIVE GALACTIC NUCLEI; ULTRALUMINOUS INFRARED GALAXIES; DUST-OBSCURED GALAXIES; STAR-FORMATION RATES; DIGITAL SKY SURVEY; SPECTRAL ENERGY-DISTRIBUTIONS; COLOR-MAGNITUDE RELATION; MEDIUM DEEP SURVEY; LUMINOSITY FUNCTION; REDSHIFT SURVEY AB We analyze the morphological properties of a large sample of 1503 70 mu m selected galaxies in the COSMOS field spanning the redshift range 0.01 < z < 3.5 with a median redshift of 0.5 and an infrared luminosity range of 10(8) < L-IR(8-1000 mu m) < 10(14) L-circle dot with a median luminosity of 10(11.4) L-circle dot. In general, these galaxies are massive, with a stellar mass range of 10(10)-10(12) M-circle dot, and luminous, with -25 < M-K < -20. We find a strong correlation between the fraction of major mergers and L-IR, with the fraction at the highest luminosity (L-IR > 10(12) L-circle dot) being up to similar to 50%. We also find that the fraction of spirals drops dramatically with LIR. Minor mergers likely play a role in boosting the infrared luminosity for sources with low luminosities (L-IR < 10(11.5) L-circle dot). The precise fraction of mergers in any given L-IR bin varies by redshift due to sources at z > 1 being difficult to classify and subject to the effects of bandpass shifting; therefore, these numbers can only be considered lower limits. At z < 1, where the morphological classifications are most robust, major mergers clearly dominate the ULIRG population (similar to 50%-80%) and are important for the LIRG population (similar to 25%-40%). At z > 1, the fraction of major mergers is lower, but is at least 30%-40% for ULIRGs. In a comparison of our visual classifications with several automated classification techniques we find general agreement; however, the fraction of identified mergers is underestimated due to automated classification methods being sensitive to only certain timescales of a major merger. Although the general morphological trends agree with what has been observed for local (U) LIRGs, the fraction of major mergers is slightly lower than seen locally. This is in part due to the difficulty of identifying merger signatures at high redshift. The distribution of the U-V color of the galaxies in our sample peaks in the green valley (< U - V > = 1.1) with a large spread at bluer and redder colors and with the major mergers peaking more strongly in the green valley than the rest of the morphological classes. We argue that, given the number of major gas-rich mergers observed and the relatively short timescale that they would be observable in the (U) LIRG phase, it is plausible for the observed red sequence of massive ellipticals (< 10(12) M-circle dot) to have been formed entirely by gas-rich major mergers. C1 [Kartaltepe, Jeyhan S.; Sanders, D. B.; Le Floc'h, E.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Kartaltepe, Jeyhan S.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Le Floc'h, E.; Aussel, H.] Univ Paris 07, CNRS, AIM Unite Mixte Rech, CEA CNRS,UMR 7158, F-91191 Gif Sur Yvette, France. [Frayer, D. T.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Arnouts, S.] Canada France Hawaii Telescope Corp, Kamuela, HI 96743 USA. [Ilbert, O.; Cassata, P.; Le Fevre, O.] Lab Astrophys Marseille, F-13376 Marseille 12, France. [Salvato, M.; Scoville, N. Z.; Capak, P.; Smolcic, V.] CALTECH, MC 105 24, Pasadena, CA 91125 USA. [Surace, J.; Yan, L.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Caputi, K.; Carollo, C. M.; Lilly, S.] ETH, Dept Phys, CH-8093 Zurich, Switzerland. [Civano, F.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hasinger, G.] Max Planck Inst Extraterr Phys, D-85478 Garching, Germany. [Koekemoer, A. M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Liu, C. T.; Fiorenza, S. L.] CUNY, Coll Staten Isl, Astrophys Observ, Staten Isl, NY 10314 USA. [McCracken, H. J.] Univ Paris 06, Inst Astrophys Paris, CNRS, UMR 7095, F-75014 Paris, France. [Schinnerer, E.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Taniguchi, Y.] Ehime Univ, Dept Phys, Grad Sch Sci, Matsuyama, Ehime 7908577, Japan. [Thompson, D. J.] Univ Arizona, Large Binocular Telescope Observ, Tucson, AZ 85721 USA. [Trump, J.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Baldassare, V. F.] CUNY, Dept Phys & Astron, Hunter Coll, New York, NY 10065 USA. RP Kartaltepe, JS (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. EM jeyhan@noao.edu RI Le Fevre, Olivier/G-7389-2011; OI Koekemoer, Anton/0000-0002-6610-2048 FU NASA [NAS 5-26555, 1282612, 1298213, 1344920]; European Southern Observatory, Chile [175.A-0839]; CFHT Corporation; CEA/DAPNIA; National Research Council of Canada; Canadian Astronomy Data Centre; Centre National de la Recherche Scientifique de France; TERAPIX; University of Hawaii; City University of New York; NSF [AST-0071048]; National Aeronautics and Space Administration; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England FX Based on observations with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by AURA Inc, under NASA contract NAS 5-26555; also based on data collected at the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan; the XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA; the European Southern Observatory under Large Program 175.A-0839, Chile; the National Radio Astronomy Observatory which is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc; the Canada-France-Hawaii Telescope with MegaPrime/MegaCam operated as a joint project by the CFHT Corporation, CEA/DAPNIA, the National Research Council of Canada, the Canadian Astronomy Data Centre, the Centre National de la Recherche Scientifique de France, TERAPIX and the University of Hawaii.; Support for this work was provided in part by NASA through contracts 1282612, 1298213, and 1344920 issued by the Jet Propulsion Laboratory. This work was supported in part by a grant from The City University of New York PSC-CUNY Research Award Program. We would also like to recognize the contributions from all of the members of the COSMOS Team who helped in obtaining and reducing the large amount of multi-wavelength data that are now publicly available through the NASA Infrared Science Archive (IRSA) at http://irsa.ipac.caltech.edu/Missions/cosmos.html. The analysis pipeline used to reduce the DEIMOS data was developed at UC Berkeley with support from NSF grant AST-0071048. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research has also made use of data from the Sloan Digital Sky Survey (SDSS-DR7). Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web site is http://www.sdss.org/. We thank the anonymous referee for their thorough comments, which greatly improved the paper. We also thank Marco Barden and Knud Jhanke for the use of the FERENGI redshifting code as well as their help with using it. NR 103 TC 78 Z9 78 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 2010 VL 721 IS 1 BP 98 EP 123 DI 10.1088/0004-637X/721/1/98 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 654TI UT WOS:000282192900008 ER PT J AU Romita, KA Carlson, LR Meixner, M Sewilo, M Whitney, B Babler, B Indebetouw, R Hora, JL Meade, M Shiao, B AF Romita, Krista Alexandra Carlson, Lynn Redding Meixner, M. Sewilo, M. Whitney, B. Babler, B. Indebetouw, R. Hora, J. L. Meade, M. Shiao, B. TI YOUNG STELLAR OBJECTS IN THE LARGE MAGELLANIC CLOUD STAR-FORMING REGION N206 SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared: stars; ISM: individual objects (N206); Magellanic Clouds; stars: formation; stars: pre-main sequence ID 2-DIMENSIONAL RADIATIVE-TRANSFER; SPECTRAL ENERGY-DISTRIBUTIONS; PROTOSTELLAR ENVELOPES; SUPERNOVA-REMNANTS; SPITZER ANALYSIS; MASSIVE STARS; SAGE; SEQUENCE; 2MASS; EVOLUTION AB We present analysis of the energetic star-forming region Henize 206 (N206) located near the southern edge of the Large Magellanic Cloud (LMC) based on photometric data from the Spitzer Surveying the Agents of Galaxy Evolution (SAGE-LMC; IRAC 3.6, 4.5, 5.8, 8.0 mu m and MIPS 24 mu m), Infrared Survey Facility near-infrared survey (J, H, K(s)), and the Magellanic Clouds Photometric Survey (MCPS UBVI) covering a wavelength range of 0.36-24 mu m. Young stellar object (YSO) candidates are identified based upon their location in infrared color-magnitude space and classified by the shapes of their spectral energy distributions in comparison with a pre-computed grid of YSO models. We identify 116 YSO candidates: 102 are well characterized by the YSO models, predominately Stage I, and 14 may be multiple sources or young sources with transition disks. Careful examination of the individual sources and their surrounding environment allows us to identify a factor of similar to 14.5 more YSO candidates than have already been identified. The total mass of these well-fit YSO candidates is similar to 520 M(circle dot). We calculate a current star formation rate of 0.27 x 10(-1) M(circle dot) yr(-1) kpc(-2). The distribution of YSO candidates appears to follow shells of neutral material in the interstellar medium. C1 [Romita, Krista Alexandra; Meixner, M.; Sewilo, M.; Shiao, B.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Carlson, Lynn Redding] Johns Hopkins Univ, Baltimore, MD USA. [Whitney, B.] Space Sci Inst, Boulder, CO USA. [Babler, B.; Meade, M.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Indebetouw, R.] Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. [Hora, J. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Romita, KA (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. EM k.a.romita@gmail.com; carlson@stsci.edu; bwhitney@spacescience.org; brian@sal.wisc.edu; remy@virginia.edu; jhora@cfa.harvard.edu OI Babler, Brian/0000-0002-6984-5752; Hora, Joseph/0000-0002-5599-4650 NR 41 TC 7 Z9 7 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 2010 VL 721 IS 1 BP 357 EP 368 DI 10.1088/0004-637X/721/1/357 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 654TI UT WOS:000282192900023 ER PT J AU Broderick, AE Keto, E AF Broderick, Avery E. Keto, Eric TI THE EVOLUTION OF CLOUD CORES AND THE FORMATION OF STARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE hydrodynamics; ISM: clouds; ISM: kinematics and dynamics; stars: formation ID PRE-STELLAR CORES; OSCILLATING STARLESS CORES; CARLO RADIATIVE-TRANSFER; INITIAL CONDITIONS; DARK CLOUDS; DENSE CORES; PRESTELLAR CORES; DYNAMICAL STATE; TEMPERATURE; EXTINCTION AB For a number of starless cores, self-absorbed molecular line and column density observations have implied the presence of large-amplitude oscillations. We examine the consequences of these oscillations on the evolution of the cores and the interpretation of their observations. We find that the pulsation energy helps support the cores and that the dissipation of this energy can lead toward instability and star formation. In this picture, the core lifetimes are limited by the pulsation-decay timescales, dominated by non-linear mode-mode coupling, and on the order of similar or equal to few x 10(5)-10(6) yr. Notably, this is similar to what is required to explain the relatively low rate of conversion of cores into stars. For cores with large-amplitude oscillations, dust continuum observations may appear asymmetric or irregular. As a consequence, some of the cores that would be classified as super-critical may be dynamically stable when oscillations are taken into account. Thus, our investigation motivates a simple hydrodynamic picture, capable of reproducing many of the features of the progenitors of stars without the inclusion of additional physical processes, such as large-scale magnetic fields. C1 [Broderick, Avery E.] Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Keto, Eric] Smithsonian Observ, Cambridge, MA 02138 USA. RP Broderick, AE (reprint author), Canadian Inst Theoret Astrophys, 60 St George St, Toronto, ON M5S 3H8, Canada. EM aeb@cita.utoronto.ca; keto@cfa.harvard.edu NR 48 TC 8 Z9 8 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 2010 VL 721 IS 1 BP 493 EP 504 DI 10.1088/0004-637X/721/1/493 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 654TI UT WOS:000282192900033 ER PT J AU Koch, PM Tang, YW Ho, PTP AF Koch, Patrick M. Tang, Ya-Wen Ho, Paul T. P. TI MAGNETIC FIELD PROPERTIES IN HIGH-MASS STAR FORMATION FROM LARGE TO SMALL SCALES: A STATISTICAL ANALYSIS FROM POLARIZATION DATA SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: clouds; ISM: individual objects (W51 e2/e8, Orion BN/KL); ISM: magnetic fields; methods: statistical; polarization; turbulence ID FAR-INFRARED POLARIMETRY; MOLECULAR CLOUDS; SUBMILLIMETER POLARIZATION; RADIATIVE TORQUES; GRAIN ALIGNMENT; FORMING REGIONS; INTERSTELLAR GRAINS; CORES; ORION; DISPERSION AB Polarization data from high-mass star formation regions (W51 e2/e8, Orion BN/KL) are used to derive statistical properties of the plane of sky projected magnetic field. Structure function and auto-correlation function are calculated for observations with various resolutions from the BIMA and SMA interferometers, covering a range in physical scales from similar to 70 mpc to similar to 2.1 mpc. Results for the magnetic field turbulent dispersion, its turbulent-to-mean field strength ratio, and the large-scale polarization angle correlation length are presented as a function of the physical scale at the star formation sites. Power-law scaling relations emerge for some of these physical quantities. The turbulent-to-mean field strength ratio is found to be close to constant over the sampled observing range, with a hint of a decrease toward smaller scales, indicating that the role of the magnetic field and turbulence is evolving with the physical scale. A statistical method is proposed to separate large-and small-scale correlations from an initial ensemble of polarization segments. This also leads to a definition of a turbulent polarization angle correlation length. C1 [Koch, Patrick M.; Tang, Ya-Wen; Ho, Paul T. P.] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan. [Ho, Paul T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Koch, PM (reprint author), Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan. EM pmkoch@asiaa.sinica.edu.tw OI Tang, Ya-Wen/0000-0002-0675-276X FU NSC [NSC98-2119-M-001-024-MY4] FX The authors thank the referees, Roger H. Hildebrand, Martin Houde, and John E. Vaillancourt for their comments and explanations which provided important further insight. Y.-W.T. and P. T. P. H. are supported by NSC grant NSC98-2119-M-001-024-MY4. NR 48 TC 14 Z9 14 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 2010 VL 721 IS 1 BP 815 EP 827 DI 10.1088/0004-637X/721/1/815 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 654TI UT WOS:000282192900061 ER PT J AU Su, YN van Ballegooijen, A Golub, L AF Su, Yingna van Ballegooijen, Adriaan Golub, Leon TI STRUCTURE AND DYNAMICS OF QUIESCENT FILAMENT CHANNELS OBSERVED BY HINODE/XRT AND STEREO/EUVI SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: activity; Sun: corona; Sun: filaments, prominences; Sun: magnetic topology; Sun: UV radiation; Sun: X-rays, gamma rays ID GLOBAL SOLAR CORONA; ACTIVE-REGION 10953; RAY TELESCOPE XRT; MAGNETIC-FIELDS; H-ALPHA; FLUX ROPE; PROMINENCES; EVOLUTION; SUN; SIMULATIONS AB We present a study of the structure and dynamics of quiescent filament channels observed by Hinode/XRT and STEREO/EUVI at the solar minimum 23/24 from 2006 November to 2008 December. For 12 channels identified on the solar disk (Group I channels), we find that the morphology of the structure on the two sides of the channel is asymmetric in bothX-rays and EUV: the eastern side has curved features while the western side has straight features. We interpret the results in terms of a magnetic flux rope model. The asymmetry in the morphology is due to the variation in axial flux of the flux rope along the channel, which causes the field lines from one polarity to turn into the flux rope (curved feature), while the field lines from the other polarity are connected to very distant sources (straight). For most of the 68 channels identified by cavities at the east and west limbs (Group II channels), the asymmetry cannot be clearly identified, which is likely due to the fact that the axial flux may be relatively constant along such channels. Corresponding cavities are identified only for 5 of the 12 Group I channels, while Group II channels are identified for all of the 68 cavity pairs. The studied filament channels are often observed as dark channels in X-rays and EUV. Sheared loops within Group I channels are often seen in X-rays, but are rarely seen in Group II channels as shown in the X-ray Telescope daily synoptic observations. A survey of the dynamics of studied filament channels shows that filament eruptions occur at an average rate of 1.4 filament eruptions per channel per solar rotation. C1 [Su, Yingna; van Ballegooijen, Adriaan; Golub, Leon] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Su, YN (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM ynsu@head.cfa.harvard.edu RI Su, Yingna/J-1674-2012; OI van Ballegooijen, Adriaan/0000-0002-5622-3540; Golub, Leon/0000-0001-9638-3082 FU NASA [NNM07AB07C]; International Space Science Institute (Bern) FX We thank the referee for helpful comments to improve this paper. Hinode is a Japanese mission developed and launched by ISAS/JAXA, with NAOJ as domestic partner and NASA and STFC (UK) as international partners. It is operated by these agencies in cooperation with ESA and the NSC (Norway). The authors thank the teams of Hinode/XRT, STEREO/SECCHI, Yohkoh/SXT, TRACE, SOLIS, SOHO/LASCO, KSO, MLSO, BBSO for providing the valuable data. US members of the XRT team are supported by NASA contract NNM07AB07C to Smithsonian Astrophysical Observatory (SAO). Y.S. acknowledges Dr. Kathy Reeves and Dr. David McKenzie for providing observational information on cavities and filament channels by Hinode/XRT and Yohkoh/SXT. The authors acknowledge the International Space Science Institute (Bern) for supporting the international team on Prominence Cavities. They also thank the team members for lively discussions. NR 53 TC 9 Z9 9 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 2010 VL 721 IS 1 BP 901 EP 910 DI 10.1088/0004-637X/721/1/901 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 654TI UT WOS:000282192900069 ER PT J AU Kewley, LJ Rupke, D Zahid, HJ Geller, MJ Barton, EJ AF Kewley, Lisa J. Rupke, David Zahid, H. Jabran Geller, Margaret J. Barton, Elizabeth J. TI METALLICITY GRADIENTS AND GAS FLOWS IN GALAXY PAIRS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: abundances; galaxies: fundamental parameters; galaxies: interactions; galaxies: starburst ID TRIGGERED STAR-FORMATION; ULTRALUMINOUS INFRARED GALAXIES; GEMINI SPECTROSCOPIC SURVEY; EXTRAGALACTIC HII-REGIONS; CLOSE PAIRS; ABUNDANCE GRADIENT; STARBURST GALAXIES; MOLECULAR GAS; H-II; CLUSTERS AB We present the first systematic investigation into the metallicity gradients in galaxy close pairs. We determine the metallicity gradients for eight galaxies in close pairs using H II region metallicities obtained with high signal-to-noise multi-slit observations with the Keck LRIS Spectrograph. We show that the metallicity gradients in close pairs are significantly shallower than gradients in isolated spiral galaxies such as the Milky Way, M83, and M101. These observations provide the first solid evidence that metallicity gradients in interacting galaxies are systematically different from metallicity gradients in isolated spiral galaxies. Our results suggest that there is a strong relationship between metallicity gradients and the gas dynamics in galaxy interactions and mergers. C1 [Kewley, Lisa J.; Rupke, David; Zahid, H. Jabran] Univ Hawaii, Inst Astron, Hilo, HI 96822 USA. [Geller, Margaret J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Barton, Elizabeth J.] Univ Calif Irvine, Irvine, CA 92697 USA. RP Kewley, LJ (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Hilo, HI 96822 USA. EM kewley@ifa.hawaii.edu NR 50 TC 87 Z9 87 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD SEP 20 PY 2010 VL 721 IS 1 BP L48 EP L52 DI 10.1088/2041-8205/721/1/L48 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 647HY UT WOS:000281610300011 ER PT J AU Horton, BM Yoon, J Ghalambor, CK Moore, IT Sillett, TS AF Horton, Brent M. Yoon, Jongmin Ghalambor, Cameron K. Moore, Ignacio T. Sillett, T. Scott TI Seasonal and population variation in male testosterone levels in breeding orange-crowned warblers (Vermivora celata) SO GENERAL AND COMPARATIVE ENDOCRINOLOGY LA English DT Article DE Breeding density; Life history; Mating effort; Parental investment; Testosterone Trade-offs ID DARK-EYED JUNCOS; EXPERIMENTALLY ELEVATED TESTOSTERONE; IMMUNOCOMPETENCE HANDICAP HYPOTHESIS; AVIAN LIFE HISTORIES; BASAL METABOLIC-RATE; MALE HOUSE SPARROWS; MALE GREAT TITS; TRADE-OFFS; BEHAVIORAL INSENSITIVITY; TERRITORIAL BEHAVIOR AB Comparative hormone studies can reveal how physiology underlies life history variation. Here, we examined seasonal variation in plasma testosterone concentration between populations of male orangecrowned warblers (Vermivora celata) breeding in Fairbanks, Alaska (V. c. celata) and on Santa Catalina Island, California (V. c. sordida). These populations face different ecological constraints and exhibit different life histories. Alaska birds have a short breeding season, low annual adult survival, and high reproductive rates. In contrast, Catalina Island birds exhibit high adult survival and low reproductive rates despite having a long breeding season. We examined seasonal variation in male testosterone concentrations as a potential mechanism underlying differences in male reproductive strategies between populations. From 2006 to 2008, we sampled males during the pre-incubation, incubation, and nestling stages. Alaska males exhibited a seasonal testosterone pattern typical of northern passerines: testosterone levels were high during pre-incubation and declined during incubation to low levels during nestling provisioning. Testosterone concentrations in Catalina Island males, however, did not vary consistently with breeding stage, remained elevated throughout the breeding season, and were higher than in Alaska males during the nestling stage. We hypothesize that in Alaska, where short seasons and high adult mortality limit breeding opportunities, the seasonal testosterone pattern facilitates high mating effort prior to incubation, but high parental investment during the nestling stage. On Catalina Island, elevated testosterone levels may reflect the extended mating opportunities and high population density facing males in this population. Our results suggest that population variation in seasonal testosterone patterns in orange-crowned warblers may be a function of differences in life history strategy and the social environment. Published by Elsevier Inc. C1 [Horton, Brent M.; Sillett, T. Scott] Smithsonian Migratory Bird Ctr, Washington, DC 20013 USA. [Yoon, Jongmin; Ghalambor, Cameron K.] Colorado State Univ, Dept Biol, Ft Collins, CO 80523 USA. [Moore, Ignacio T.] Virginia Tech, Dept Biol Sci, Blacksburg, VA 24061 USA. RP Horton, BM (reprint author), Smithsonian Migratory Bird Ctr, Natl Zool Pk,POB 37012 MRC 5503, Washington, DC 20013 USA. EM hortonb@si.edu OI Moore, Ignacio/0000-0001-8875-8913 NR 74 TC 15 Z9 15 U1 0 U2 18 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0016-6480 J9 GEN COMP ENDOCR JI Gen. Comp. Endocrinol. PD SEP 15 PY 2010 VL 168 IS 3 BP 333 EP 339 DI 10.1016/j.ygcen.2010.04.019 PG 7 WC Endocrinology & Metabolism SC Endocrinology & Metabolism GA 641LF UT WOS:000281126700005 PM 20420840 ER PT J AU Aplin, KP Helgen, KM Lunde, DP AF Aplin, Kenneth P. Helgen, Kristofer M. Lunde, Darrin P. TI A Review of Peroryctes broadbenti, the Giant Bandicoot of Papua New Guinea SO AMERICAN MUSEUM NOVITATES LA English DT Review ID SEXUAL-DIMORPHISM; CANINE SIZE; MARSUPIALIA; MAMMALS; PERAMELEMORPHIA; THYLACOMYIDAE; POPULATIONS; SELECTION; BEHAVIOR; MURIDAE AB The giant bandicoot, Peroryctes broadbenti (Ramsay, 1879), is represented in museum collections by 23 specimens collected at 12 localities in the lowlands of the southeastern peninsula (the "Papuan Peninsula") of Papua New Guinea. Available data on P broadbenti are reviewed, including its comparative anatomy and morphological variability, taxonomic relationships, geographic and elevational distribution, dietary and reproductive traits, and conservation status. Despite previous confusion between this species and P. raffrayana (Milne-Edwards, 1878), the two species are readily distinguished by a suite of external, cranial, and dental characters. Diagnostic characters are enumerated and illustrated, and comparisons drawn with other New Guinean bandicoots. Generic distinction of Peroryctes Thomas, 1906, in cranial morphology from other New Guinean bandicoots is also reviewed. A striking degree of sexual dimorphism is documented in both body size and dentition for P broadbenti; these comparisons are set in context by a review of sexual dimorphism among bandicoots in general. C1 [Aplin, Kenneth P.] CSIRO, Div Sustainable Ecosyst, Canberra, ACT 2601, Australia. [Aplin, Kenneth P.; Helgen, Kristofer M.; Lunde, Darrin P.] Amer Museum Nat Hist, Div Vertebrate Zool Mammal, New York, NY 10024 USA. [Helgen, Kristofer M.] Smithsonian Inst, Div Mammals, Natl Museum Nat Hist, MRC 108, Washington, DC 20013 USA. RP Aplin, KP (reprint author), CSIRO, Div Sustainable Ecosyst, Canberra, ACT 2601, Australia. EM ken.aplin@csiro.au; helgenk@si.edu; lunde@amnh.org FU Smithsonian Institution; National Science Foundation; Bernice P. Bishop Museum; American Society of Mammalogists FX The second author's studies of New Guinean mammals were supported by grants from the Smithsonian Institution, National Science Foundation, the Bernice P. Bishop Museum, and the American Society of Mammalogists. NR 86 TC 16 Z9 16 U1 0 U2 5 PU AMER MUSEUM NATURAL HISTORY PI NEW YORK PA ATTN: LIBRARY-SCIENTIFIC PUBLICATIONS DISTRIBUTION, CENTRAL PK WEST AT 79TH ST, NEW YORK, NY 10024-5192 USA SN 0003-0082 EI 1937-352X J9 AM MUS NOVIT JI Am. Mus. Novit. PD SEP 14 PY 2010 IS 3696 BP 1 EP 41 PG 41 WC Biodiversity Conservation; Zoology SC Biodiversity & Conservation; Zoology GA 650QU UT WOS:000281866700001 ER PT J AU Garcia-Robledo, C Horvitz, CC Staines, CL AF Garcia-Robledo, Carlos Horvitz, Carol C. Staines, Charles L. TI Larval morphology, development, and notes on the natural history of Cephaloleia "rolled-leaf" beetles (Coleoptera: Chrysomelidae: Cassidinae) SO ZOOTAXA LA English DT Article DE Cannaceae; Cephaloleia; Costaceae; Heliconiaceae; Larval development; life cycle; Marantaceae; sexual dimorphism; Zingiberaceae; Zingiberales ID HELICONIA INSECT COMMUNITIES; HISPINE BEETLES; HERBIVORES; EVOLUTION; GINGERS; FOREST; ZINGIBERALES; IMBRICATA; CHEMISTRY AB The Neotropical genus Cephaloleia Chevrolat, 1837 is comprised of 209 described species. Adults usually feed and mate within the scrolls formed by the young rolled leaves of plants of Neotropical Zingiberales. This paper reports for populations of Cephaloleia belti Baly, C. dilaticollis Baly, C. dorsalis Baly and C. placida Baly at La Selva Biological Station (Costa Rica, Central America) detailed descriptions of: 1. larval and adult diets and diet breadth; 2. egg, larval and pupal morphology; 3. larval development times; 4. dimorphic sexual characteristics; 5. adult longevity; and 6. differences in lifespan between genders. Cephaloleia belti displays the broader diet breadth, feeding on 14 species of three families of Zingiberales. Cephaloleia dilaticollis feeds on nine species of three families of Zingiberales. Cephaloleia dorsalis and C. placida feed on four species of Costaceae and two species of Zingiberaceae, respectively. Time to pupation ranges among species from 32.8 to 59.1 days. In the four Cephaloleia species, adult females are larger than males. Genders display marked sexual dimorphism in the shape of their last abdominal sternite and the pygidium. Longevity of adults ranged from ca. 300 to 390 days. Life expectancy estimates for adult beetles reared in the laboratory ranged from 111.5 to 187.2 days. Male and female adults of C. belti and C. dilaticollis have equivalent life expectancies. However, life expectancy is longer for male C. dorsalis and C. placida. C1 [Garcia-Robledo, Carlos; Horvitz, Carol C.] Univ Miami, Dept Biol, Coral Gables, FL 33124 USA. [Staines, Charles L.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. RP Garcia-Robledo, C (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, POB 37012, Washington, DC 20013 USA. EM garciac@si.edu FU University of Miami; OTS (Organization for Tropical Studies); College of Arts and Sciences, University of Miami FX The authors thank the staff of La Selva Biological Station - Organization for Tropical Studies. We want to thank G. Frias, J.G. Huertas, G. Huertas and R. Sanchez, for assistance in the field and laboratory. SEM images were provided by P. Blackwelder, H. Al Sayegh, and X. Vial - University of Miami Center for Advanced Microscopy (UMCAM). The illustrations included in this paper were made by E. K. Kuprewicz. This research was funded by the J. McLamore Fellowship - University of Miami and the OTS (Organization for Tropical Studies) - Donald and Beverly Stone Fellowship and the OTS-Christiane and Christopher Tyson Fellowship to C. Garcia-Robledo and the Cooper Fellowship, College of Arts and Sciences, University of Miami to C. C. Horvitz. Comments by M. L. Chamorro-Lacayo, T. H. Fleming, D. J. Futuyma, J. Gomez-Zurita, E. K. Kuprewicz, K. D. Waddington, B. A. Whitlock and two anonymous reviewers improved this manuscript substantially. This is contribution No. 663 of the Program in Tropical Biology, Evolution and Behavior, Department of Biology, University of Miami. NR 53 TC 14 Z9 14 U1 0 U2 1 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD SEP 13 PY 2010 IS 2610 BP 50 EP 68 PG 19 WC Zoology SC Zoology GA 648TZ UT WOS:000281718500003 ER PT J AU Younger, JD Fazio, GG Ashby, MLN Civano, F Gurwell, MA Huang, JS Iono, D Peck, AB Petitpas, GR Scott, KS Wilner, DJ Wilson, GW Yun, MS AF Younger, Joshua D. Fazio, Giovanni G. Ashby, Matthew L. N. Civano, Francesca Gurwell, Mark A. Huang, Jia-Sheng Iono, Daisuke Peck, Alison B. Petitpas, Glen R. Scott, Kimberly S. Wilner, David J. Wilson, Grant W. Yun, Min S. TI The physical scale of the far-infrared emission in the most luminous submillimetre galaxies - II. Evidence for merger-driven star formation SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Review DE instrumentation: interferometers; galaxies: high-redshift; galaxies: interactions; galaxies: starburst; infrared: galaxies; submillimetre: general ID SUPERMASSIVE BLACK-HOLES; ACTIVE GALACTIC NUCLEI; HIGH-REDSHIFT GALAXIES; INITIAL MASS FUNCTION; PHASE CALIBRATION SOURCES; EVOLUTION SURVEY COSMOS; LAMBDA-CDM UNIVERSE; MU-M OBSERVATIONS; FORMING GALAXIES; RADIO CORRELATION AB We present high-resolution 345-GHz interferometric observations of two extremely luminous (L(ir) greater than or similar to 1013 L(circle dot)), submillimetre-selected galaxies (SMGs) in the Cosmic Evolution Survey (COSMOS) field with the Submillimeter Array (SMA). Both targets were previously detected as unresolved point sources by the SMA in its compact configuration, also at 345 GHz. These new data, which provide a factor of greater than or similar to 3 improvement in resolution, allow us to measure the physical scale of the far-infrared in the submillimetre directly. The visibility functions of both targets show significant evidence for structure on similar to 0.5-1-arcsec scales, which at z greater than or similar to 1.5 translates into a physical scale of similar to 5-8 kpc. Our results are consistent with the angular and physical scales of two comparably luminous objects with high-resolution SMA follow-up, as well as radio continuum and CO sizes of other SMGs. These relatively compact sizes (less than or similar to 5-10 kpc) argue strongly for merger-driven starbursts, rather than extended gas-rich discs, as the preferred channel for forming SMGs. C1 [Younger, Joshua D.] Inst Adv Study, Sch Nat Sci, Princeton, NJ 08540 USA. [Fazio, Giovanni G.; Ashby, Matthew L. N.; Civano, Francesca; Gurwell, Mark A.; Huang, Jia-Sheng; Petitpas, Glen R.; Wilner, David J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Iono, Daisuke] Nobeyama Radio Observ, Minamisa Ku, Nagano 3841805, Japan. [Peck, Alison B.] Joint ALMA Off, Santiago 7550108, Chile. [Scott, Kimberly S.; Wilson, Grant W.; Yun, Min S.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Scott, Kimberly S.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. RP Younger, JD (reprint author), Inst Adv Study, Sch Nat Sci, Einstein Dr, Princeton, NJ 08540 USA. EM jyounger@ias.edu FU Smithsonian Institution; Academia Sinica; NASA [HF-51266.01, NAS 5-26555, HST-GO-09822]; NSF [AST 0828222, AST 0907952] FX We are thankful to the referee for his helpful comments. The Sub-millimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. This research has made use of data obtained from the Chandra Data Archive and software provided by the Chandra X-ray Center (CXC) in the application packages CIAO and SHERPA. This research was based in part on data collected at Subaru Telescope, which is operated by the National Astronomical Observatory of Japan, as well as observations obtained with WIRCam, a joint project of Canada-France-Hawaii Telescope (CFHT), Taiwan, Korea, Canada, France and the CFHT which is operated by the National Research Council (NRC) of Canada, the Institute National des Sciences de l'Univers of the Centre National de la Recherche Scientifique of France and the University of Hawaii. We furthermore utilize observations made with the NASA/ESA HST. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc., and the James Clerk Maxwell Telescope is operated by The Joint Astronomy Centre on behalf of the Science and Technology Facilities Council of the United Kingdom, the Netherlands Organisation for Scientific Research and the National Research Council of Canada. JDY acknowledges support from NASA through Hubble Fellowship grant HF-51266.01 awarded by the Space Telescope Science Institute (STScI), which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. STScI is operated by the association of Universities for Research in Astronomy, Inc., under the NASA contract NAS 5-26555. The HST COSMOS Treasury programme was supported through NASA grant HST-GO-09822. Work with the AzTEC data is supported, in part, by NSF grants AST 0828222 and AST 0907952. NR 156 TC 25 Z9 25 U1 0 U2 0 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD SEP 11 PY 2010 VL 407 IS 2 BP 1268 EP 1276 DI 10.1111/j.1365-2966.2010.16984.x PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 646OG UT WOS:000281551300045 ER PT J AU Sato, M Reid, MJ Brunthaler, A Menten, KM AF Sato, M. Reid, M. J. Brunthaler, A. Menten, K. M. TI TRIGONOMETRIC PARALLAX OF W51 MAIN/SOUTH SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrometry; Galaxy: fundamental parameters; Galaxy: kinematics and dynamics; Galaxy: structure; ISM: individual objects (W51); masers ID H2O MASER SOURCES; STAR-FORMING REGION; CELESTIAL REFERENCE FRAME; GHZ METHANOL MASERS; PROPER MOTIONS; MASSIVE CORES; ORION-KL; DYNAMICAL COLLAPSE; STELLAR ORBITS; SPIRAL ARM AB We report measurement of the trigonometric parallax of W51 Main/South using the Very Long Baseline Array. We measure a value of 0.185 +/- 0.010 mas corresponding to a distance of 5.41(-0.28)(+0.31) kpc. W51 Main/South is a well-known massive star-forming region near the tangent point of the Sagittarius spiral arm of the Milky Way. Our distance to W51 yields an estimate of the distance to the Galactic center of R(0) = 8.3 +/- 0.46 (statistical) +/-1.0 (systematic) kpc by simple geometry. Combining the parallax and proper motion measurements for W51, we obtained the full-space motion of thismassive star-forming region. We find W51 is in a nearly circular orbit about the Galactic center. The H(2)O masers used for our parallax measurements trace four powerful bipolar outflows within a 0.4 pc size region, some of which are associated with dusty molecular hot cores and/or hyper- or ultra-compact HII regions. C1 [Sato, M.] Univ Tokyo, Grad Sch Sci, Dept Astron, Tokyo 1130033, Japan. [Sato, M.; Reid, M. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Sato, M.] Natl Inst Nat Sci, Natl Astron Observ Japan, VERA Project, Mitaka, Tokyo 1818588, Japan. [Brunthaler, A.; Menten, K. M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. RP Sato, M (reprint author), Univ Tokyo, Grad Sch Sci, Dept Astron, Tokyo 1130033, Japan. FU JSPS FX The authors thank an anonymous referee for many valuable comments. M. S. acknowledges financial support from the JSPS Research Fellowships for Young Scientists. This work was supported by a Grant-in-Aid for JSPS Fellows and conducted as part of her visiting research at Harvard-Smithsonian Center for Astrophysics through Smithsonian Astrophysical Observatory Predoctoral Program and the JSPS Excellent Young Researchers Overseas Visit Program. NR 60 TC 85 Z9 85 U1 1 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 2010 VL 720 IS 2 BP 1055 EP 1065 DI 10.1088/0004-637X/720/2/1055 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 647ND UT WOS:000281624300009 ER PT J AU Cavagnolo, KW McNamara, BR Nulsen, PEJ Carilli, CL Jones, C Birzan, L AF Cavagnolo, K. W. McNamara, B. R. Nulsen, P. E. J. Carilli, C. L. Jones, C. Birzan, L. TI A RELATIONSHIP BETWEEN AGN JET POWER AND RADIO POWER SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: clusters: general; radio continuum: galaxies; X-rays: galaxies ID ACTIVE GALACTIC NUCLEUS; EARLY-TYPE GALAXIES; HOT INTERSTELLAR-MEDIUM; X-RAY BINARIES; CHANDRA OBSERVATIONS; BLACK-HOLES; SKY-SURVEY; ELLIPTIC GALAXIES; SCALING RELATION; BUOYANT BUBBLES AB Using Chandra X-ray and Very Large Array radio data, we investigate the scaling relationship between jet power, P(jet), and synchrotron luminosity, P(radio). We expand the sample presented in Birzan et al. to lower radio power by incorporating measurements for 21 giant elliptical galaxies (gEs) to determine if the Birzan et al. P(jet)-P(radio) scaling relations are continuous in form and scatter from gEs up to brightest cluster galaxies. We find a mean scaling relation of P(jet) approximate to 5.8 x 10(43) (P(radio)/10(40))(0.70) erg s(-1) which is continuous over similar to 6-8 decades in P(jet) and P(radio) with a scatter of approximate to 0.7 dex. Our mean scaling relationship is consistent with the model presented in Willott et al. if the typical fraction of lobe energy in non-radiating particles to that in relativistic electrons is greater than or similar to 100. We identify several gEs whose radio luminosities are unusually large for their jet powers and have radio sources which extend well beyond the densest parts of their X-ray halos. We suggest that these radio sources are unusually luminous because they were unable to entrain appreciable amounts of gas. C1 [Cavagnolo, K. W.; McNamara, B. R.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [McNamara, B. R.] Perimeter Inst Theoret Phys, Waterloo, ON N2L 2Y5, Canada. [McNamara, B. R.; Nulsen, P. E. J.; Jones, C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Carilli, C. L.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Birzan, L.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. RP Cavagnolo, KW (reprint author), Univ Waterloo, Dept Phys & Astron, 200 Univ Ave W, Waterloo, ON N2L 3G1, Canada. EM kcavagno@uwaterloo.ca OI Nulsen, Paul/0000-0003-0297-4493 FU CXO; CXO Center; NASA [NAS8-03060] FX K. W. C. and B. R. M. acknowledge generous support from the Natural Sciences and Engineering Research Council of Canada and grants from the CXO. C.J. thanks the Smithsonian Institution for generous support. P.N. thanks the CXO Center for supporting this work. K. W. C. thanks Judith Croston, David Rafferty, Lorant Sjouwerman, and Chris Willott for helpful discussions. We also thank the anonymous referee for a prompt and helpful review. The CXO Center is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8-03060. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. NR 71 TC 137 Z9 137 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 2010 VL 720 IS 2 BP 1066 EP 1072 DI 10.1088/0004-637X/720/2/1066 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 647ND UT WOS:000281624300010 ER PT J AU Buchhave, LA Bakos, GA Hartman, JD Torres, G Kovacs, G Latham, DW Noyes, RW Esquerdo, GA Everett, M Howard, AW Marcy, GW Fischer, DA Johnson, JA Andersen, J Furesz, G Perumpilly, G Sasselov, DD Stefanik, RP Beky, B Lazar, J Papp, I Sari, P AF Buchhave, L. A. Bakos, G. A. Hartman, J. D. Torres, G. Kovacs, G. Latham, D. W. Noyes, R. W. Esquerdo, G. A. Everett, M. Howard, A. W. Marcy, G. W. Fischer, D. A. Johnson, J. A. Andersen, J. Furesz, G. Perumpilly, G. Sasselov, D. D. Stefanik, R. P. Beky, B. Lazar, J. Papp, I. Sari, P. TI HAT-P-16b: A 4 M-J PLANET TRANSITING A BRIGHT STAR ON AN ECCENTRIC ORBIT SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars: individual (HAT-P-16, GSC 2792-01700); techniques: photometric; techniques: spectroscopic ID COROT SPACE MISSION; EXTRASOLAR PLANETS; TIDAL EVOLUTION; PERIOD PLANETS; K STAR; STELLAR; ALGORITHM; FIELD; SPECTROSCOPY; EXOPLANETS AB We report the discovery of HAT-P-16b, a transiting extrasolar planet orbiting the V = 10.8mag F8 dwarf GSC 279201700, with a period P = 2.775960 +/- 0.000003 days, transit epoch T-c = 2455027.59293 +/- 0.00031 (BJD10), and transit duration 0.1276 +/- 0.0013 days. The host star has a mass of 1.22 +/- 0.04 (M)circle dot, radius of 1.24 +/- 0.05 R-circle dot, effective temperature 6158 +/- 80 K, and metallicity [Fe/H] = + 0.17 +/- 0.08. The planetary companion has a mass of 4.193 +/- 0.094 M-J and radius of 1.289 +/- 0.066 R-J, yielding a mean density of 2.42 +/- 0.35 g cm(-3). Comparing these observed characteristics with recent theoretical models, we find that HAT-P-16b is consistent with a 1 Gyr H/He-dominated gas giant planet. HAT-P-16b resides in a sparsely populated region of the mass-radius diagram and has a non-zero eccentricity of e = 0.036 with a significance of 10s. C1 [Buchhave, L. A.; Bakos, G. A.; Hartman, J. D.; Torres, G.; Latham, D. W.; Noyes, R. W.; Esquerdo, G. A.; Everett, M.; Furesz, G.; Perumpilly, G.; Sasselov, D. D.; Stefanik, R. P.; Beky, B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Buchhave, L. A.; Andersen, J.] Univ Copenhagen, Niels Bohr Inst, DK-1168 Copenhagen, Denmark. [Kovacs, G.] Konkoly Observ Budapest, Budapest, Hungary. [Howard, A. W.; Marcy, G. W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Fischer, D. A.] Yale Univ, Dept Astron, New Haven, CT 06511 USA. [Johnson, J. A.] CALTECH, Dept Astrophys, Pasadena, CA 91125 USA. [Andersen, J.] Nord Opt Telescope Sci Assoc, La Palma, Canary Islands, Spain. [Lazar, J.; Papp, I.; Sari, P.] Hungarian Astron Assoc, Budapest, Hungary. RP Buchhave, LA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Howard, Andrew/D-4148-2015; OI Howard, Andrew/0000-0001-8638-0320; Buchhave, Lars A./0000-0003-1605-5666; Hartman, Joel/0000-0001-8732-6166; Fischer, Debra/0000-0003-2221-0861 FU NASA [NNG04GN74G, NNX08AF23G, NNX09AF59G, NCC2-1390, N018Hr]; SAO IRD; NSF [AST-0702843, AST-0702821]; Hungarian Scientific Research Foundation (OTKA) [K-81373] FX HATNet operations have been funded by NASA grants NNG04GN74G, NNX08AF23G, and SAO IR&D grants. The work of G.A.B. and J.A.J. were supported by the Postdoctoral Fellowship of the NSF Astronomy and Astrophysics Program (AST-0702843 and AST-0702821, respectively). G. T. acknowledges partial support from NASA grant NNX09AF59G. We acknowledge partial support also from the Kepler Mission under NASA Cooperative Agreement NCC2-1390 ( D. W. L., PI). G. K. thanks the Hungarian Scientific Research Foundation (OTKA) for support through grant K-81373. Based in part 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. This research has made use of Keck telescope time granted through NASA (N018Hr). NR 48 TC 101 Z9 101 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 2010 VL 720 IS 2 BP 1118 EP 1125 DI 10.1088/0004-637X/720/2/1118 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 647ND UT WOS:000281624300015 ER PT J AU Acciari, VA Arlen, T Aune, T Beilicke, M Benbow, W Boltuch, D Bradbury, SM Buckley, JH Bugaev, V Byrum, K Cannon, A Cesarini, A Christiansen, JL Ciupik, L Cui, W Dickherber, R Duke, C Finley, JP Finnegan, G Furniss, A Galante, N Godambe, S Grube, J Guenette, R Gyuk, G Hanna, D Holder, J Hui, CM Humensky, TB Imran, A Kaaret, P Karlsson, N Kertzman, M Kieda, D Konopelko, A Krawczynski, H Krennrich, F Maier, G McArthur, S McCann, A McCutcheon, M Moriarty, P Ong, RA Otte, AN Pandel, D Perkins, JS Pohl, M Quinn, J Ragan, K Reyes, LC Reynolds, PT Roache, E Rose, HJ Schroedter, M Sembroski, GH Senturk, GD Smith, AW Steele, D Swordy, SP Tesic, G Theiling, M Thibadeau, S Varlotta, A Vassiliev, VV Vincent, S Wagner, RG Wakely, SP Ward, JE Weekes, TC Weinstein, A Weisgarber, T Williams, DA Wissel, S Zitzer, B AF Acciari, V. A. Arlen, T. Aune, T. Beilicke, M. Benbow, W. Boltuch, D. Bradbury, S. M. Buckley, J. H. Bugaev, V. Byrum, K. Cannon, A. Cesarini, A. Christiansen, J. L. Ciupik, L. Cui, W. Dickherber, R. Duke, C. Finley, J. P. Finnegan, G. Furniss, A. Galante, N. Godambe, S. Grube, J. Guenette, R. Gyuk, G. Hanna, D. Holder, J. Hui, C. M. Humensky, T. B. Imran, A. Kaaret, P. Karlsson, N. Kertzman, M. Kieda, D. Konopelko, A. Krawczynski, H. Krennrich, F. Maier, G. McArthur, S. McCann, A. McCutcheon, M. Moriarty, P. Ong, R. A. Otte, A. N. Pandel, D. Perkins, J. S. Pohl, M. Quinn, J. Ragan, K. Reyes, L. C. Reynolds, P. T. Roache, E. Rose, H. J. Schroedter, M. Sembroski, G. H. Senturk, G. Demet Smith, A. W. Steele, D. Swordy, S. P. Tesic, G. Theiling, M. Thibadeau, S. Varlotta, A. Vassiliev, V. V. Vincent, S. Wagner, R. G. Wakely, S. P. Ward, J. E. Weekes, T. C. Weinstein, A. Weisgarber, T. Williams, D. A. Wissel, S. Zitzer, B. TI VERITAS SEARCH FOR VHE GAMMA-RAY EMISSION FROM DWARF SPHEROIDAL GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE dark matter; galaxies: dwarf; gamma rays: galaxies ID EXPLORING HALO SUBSTRUCTURE; DARK-MATTER SUBSTRUCTURE; VELOCITY DISPERSION PROFILES; MILKY-WAY HALO; URSA-MINOR; GIANT STARS; DENSITY PROFILES; GALACTIC-CENTER; DRACO; TELESCOPE AB Indirect dark matter searches with ground-based gamma-ray observatories provide an alternative for identifying the particle nature of dark matter that is complementary to that of direct search or accelerator production experiments. We present the results of observations of the dwarf spheroidal galaxies Draco, Ursa Minor, Bootes 1, and Willman 1 conducted by the Very Energetic Radiation Imaging Telescope Array System (VERITAS). These galaxies are nearby dark matter dominated objects located at a typical distance of several tens of kiloparsecs for which there are good measurements of the dark matter density profile from stellar velocity measurements. Since the conventional astrophysical background of very high energy gamma rays from these objects appears to be negligible, they are good targets to search for the secondary gamma-ray photons produced by interacting or decaying dark matter particles. No significant gamma-ray flux above 200 GeV was detected from these four dwarf galaxies for a typical exposure of similar to 20 hr. The 95% confidence upper limits on the integral gamma-ray flux are in the range (0.4-2.2) x 10(-12) photons cm(-2) s(-1). We interpret this limiting flux in the context of pair annihilation of weakly interacting massive particles (WIMPs) and derive constraints on the thermally averaged product of the total self-annihilation cross section and the relative velocity of the WIMPs ( less than or similar to 10(-23) cm(3) s(-1) for m(chi) greater than or similar to 300 GeV c(-2)). This limit is obtained under conservative assumptions regarding the dark matter distribution in dwarf galaxies and is approximately 3 orders of magnitude above the generic theoretical prediction for WIMPs in the minimal supersymmetric standard model framework. However, significant uncertainty exists in the dark matter distribution as well as the neutralino cross sections which under favorable assumptions could further lower this limit. C1 [Acciari, V. A.; Benbow, W.; Galante, N.; Perkins, J. S.; Roache, E.; Theiling, M.; Weekes, T. C.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Arlen, T.; Ong, R. A.; Vassiliev, V. V.; Weinstein, A.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Aune, T.; Furniss, A.; Otte, A. N.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Aune, T.; Furniss, A.; Otte, A. N.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Beilicke, M.; Buckley, J. H.; Bugaev, V.; Dickherber, R.; Krawczynski, H.; McArthur, S.; Thibadeau, S.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Boltuch, D.; Holder, J.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Boltuch, D.; Holder, J.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Bradbury, S. M.; Rose, H. J.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Byrum, K.; Smith, A. W.; Wagner, R. G.] Argonne Natl Lab, Argonne, IL 60439 USA. [Cannon, A.; Quinn, J.; Ward, J. E.] Natl Univ Ireland Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Cesarini, A.] Natl Univ Ireland Galway, Sch Phys, Galway, Ireland. [Christiansen, J. L.] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 94307 USA. [Ciupik, L.; Grube, J.; Gyuk, G.; Karlsson, N.; Steele, D.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA. [Cui, W.; Finley, J. P.; Sembroski, G. H.; Varlotta, A.; Zitzer, B.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Duke, C.] Grinnell Coll, Dept Phys, Grinnell, IA 50112 USA. [Finnegan, G.; Godambe, S.; Hui, C. M.; Kieda, D.; Vincent, S.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Guenette, R.; Hanna, D.; Maier, G.; McCann, A.; McCutcheon, M.; Ragan, K.; Tesic, G.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Humensky, T. B.; Swordy, S. P.; Wakely, S. P.; Weisgarber, T.; Wissel, S.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Imran, A.; Krennrich, F.; Pohl, M.; Schroedter, M.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Kaaret, P.; Pandel, D.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. [Konopelko, A.] Pittsburg State Univ, Dept Phys, Pittsburg, KS 66762 USA. [Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland. [Reyes, L. C.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland. [Senturk, G. Demet] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. RP Acciari, VA (reprint author), Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. EM rgwcdf@hep.anl.gov OI Cui, Wei/0000-0002-6324-5772; Cesarini, Andrea/0000-0002-8611-8610; Ward, John E/0000-0003-1973-0794; Pandel, Dirk/0000-0003-2085-5586 FU US National Science Foundation; US Department of Energy; Smithsonian Institution; NSERC in Canada; Science Foundation Ireland; STFC in the UK; U.S. National Science Foundation [0422093] FX This research is supported by grants from the US National Science Foundation, the US Department of Energy, and the Smithsonian Institution, by NSERC in Canada, by Science Foundation Ireland, and by STFC in the UK. We acknowledge the excellent work of the technical support staff at the FLWO and the collaborating institutions in the construction and operation of the instrument. V. V. V. acknowledges the support of the U.S. National Science Foundation under CAREER program (Grant No. 0422093). NR 71 TC 59 Z9 59 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 SEP 10 PY 2010 VL 720 IS 2 BP 1174 EP 1180 DI 10.1088/0004-637X/720/2/1174 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 647ND UT WOS:000281624300021 ER PT J AU Hung, LW Hickox, RC Boroson, BS Vrtilek, SD AF Hung, Li-Wei Hickox, Ryan C. Boroson, Bram S. Vrtilek, Saeqa D. TI SUZAKU X-RAY SPECTRA AND PULSE PROFILE VARIATIONS DURING THE SUPERORBITAL CYCLE OF LMC X-4 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; pulsars: individual (LMC X-4); stars: neutron; X-rays: binaries ID PHASE RESOLVED-SPECTROSCOPY; NEUTRON-STAR; XMM-NEWTON; TIMING-EXPLORER; ORBITAL DECAY; SMC X-1; PERIOD; ACCRETION; DISCOVERY; HERCULES-X-1 AB We present results from spectral and temporal analyses of Suzaku and RXTE observations of the high-mass X-ray binary LMC X-4. Using the full 13 years of available RXTE/all-sky monitor data, we apply the ANOVA and Lomb Normalized Periodogram methods to obtain an improved superorbital period measurement of 30.32 +/- 0.04 days. The phase-averaged X-ray spectra from Suzaku observations during the high state of the superorbital period can be modeled in the 0.6-50 keV band as the combination of a power law with Gamma similar to 0.6 and a highenergy cutoff at similar to 25 keV, a blackbody with kT(BB) similar to 0.18 keV, and emission lines from Fe K-alpha, OVIII, and NeIX (x Ly alpha). Assuming a distance of 50 kpc, the source has luminosity L-X similar to 3 x 10(38) erg s(-1) in the 2-50 keV band, and the luminosity of the soft (blackbody) component is L-BB similar to 1.5 x 10(37) erg s-1. The energy-resolved pulse profiles show single-peaked soft (0.5-1 keV) and hard (6-10 keV) pulses but a more complex pattern of medium (2-10 keV) pulses; cross-correlation of the hard with the soft pulses shows a phase shift that varies between observations. We interpret these results in terms of a picture in which a precessing disk reprocesses the hard X-rays and produces the observed soft spectral component, as has been suggested for the similar sources Her X-1 and SMC X-1. C1 [Hung, Li-Wei] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Hung, Li-Wei; Hickox, Ryan C.; Boroson, Bram S.; Vrtilek, Saeqa D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hickox, Ryan C.] Univ Durham, Dept Phys, Durham DH1 3LE, England. RP Hung, LW (reprint author), Ohio State Univ, Dept Astron, McPherson Lab 140 W 18th Ave, Columbus, OH 43210 USA. EM hung.88@buckeyemail.osu.edu; rhickox@cfa.harvard.edu; bboroson@cfa.harvard.edu; svrtilek@cfa.harvard.edu RI XRAY, SUZAKU/A-1808-2009 FU National Science Foundation; Department of Defense [0754568]; Suzaku [NNX08AI17G]; ADP [NNX08AJ61G]; Smithsonian Institution FX We are grateful to Joseph Neilsen for his contribution to the data analysis, and to Chris Done, Christine Jones, Jonathan McDowell, and Marie Machacek for helpful discussions. We also thank the Suzaku Helpdesk for their valuable advice on the data analysis. The work was supported in part by the National Science Foundation Research Experiences for Undergraduates (REU) and Department of Defense Awards to Stimulate and Support Undergraduate Research Experiences (ASSURE) programs under grant 0754568, Suzaku grant NNX08AI17G, ADP grant NNX08AJ61G, and by the Smithsonian Institution. R. C. H. was supported by an SAO Postdoctoral Fellowship and an STFC Postdoctoral Fellowship. NR 48 TC 8 Z9 8 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 2010 VL 720 IS 2 BP 1202 EP 1214 DI 10.1088/0004-637X/720/2/1202 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 647ND UT WOS:000281624300023 ER PT J AU Rodriguez, DR Kastner, JH Wilner, D Qi, CH AF Rodriguez, David R. Kastner, Joel H. Wilner, David Qi, Chunhua TI IMAGING THE MOLECULAR DISK ORBITING THE TWIN YOUNG SUNS OF V4046 Sgr SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: spectroscopic; circumstellar matter; planetary systems; radio lines: stars; stars: individual (V4046 Sgr); stars: pre-main sequence ID PROTOPLANETARY DISKS; CIRCUMSTELLAR DISKS; H-2 EMISSION; SUBMILLIMETER ARRAY; STELLAR COMPANIONS; ORGANIC-MOLECULES; PLANET FORMATION; KEPLERIAN DISK; BINARY-SYSTEMS; STAR-FORMATION AB We have imaged the disk surrounding the nearby (D similar to 73 pc), similar to 12 Myr, classical T Tauri binary system V4046 Sgr with the Submillimeter Array (SMA) at an angular resolution of similar to 2 ''. We detect a rotating disk in (12)CO(2-1) and (13)CO(2-1) emission and resolve the continuum emission at 1.3 mm. We infer disk gas and dust masses of similar to 110 and similar to 40 Earth masses, respectively. Fits to a power-law disk model indicate that the molecular disk extends to similar to 370 AU and is viewed at an inclination of between similar to 33 degrees and similar to 39 degrees for dynamical stellar masses ranging from 1.8 M(circle dot) down to 1.5 M(circle dot) (the range of the total mass previously determined for the central, 2.4 day spectroscopic binary). This range of disk inclination is consistent with that assumed in deducing the central binary mass (i.e., 35 degrees), suggesting that the V4046 Sgr binary system and its circumbinary, molecular disk are coplanar. In light of the system's age and binarity, the presence of an extensive molecular disk orbiting V4046 Sgr provides constraints on the timescales of processes related to Jovian planet formation and demonstrates that circumbinary Jovian planets potentially could form around close binary systems. C1 [Rodriguez, David R.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Kastner, Joel H.] Rochester Inst Technol, Ctr Imaging Sci, Rochester, NY 14623 USA. [Wilner, David; Qi, Chunhua] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Rodriguez, DR (reprint author), Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. EM drodrigu@astro.ucla.edu; jhk@cis.rit.edu; dwilner@cfa.harvard.edu; cqi@cfa.harvard.edu FU Smithsonian Institution; Academia Sinica; NASA [NNX09AC96G] FX We thank Ben Zuckerman for useful discussions and comments and Meredith Hughes for lending us her deprojected visibility code. We are grateful to Michiel Hogerheijde for providing access to the two-dimensional version of RATRAN used in this work. We appreciate the suggestions and comments of the anonymous referee. The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. This research was supported by NASA Astrophysics Data Analysis Program grant NNX09AC96G to RIT and UCLA. NR 51 TC 31 Z9 31 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 2010 VL 720 IS 2 BP 1684 EP 1690 DI 10.1088/0004-637X/720/2/1684 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 647ND UT WOS:000281624300061 ER PT J AU Schwamb, ME Brown, ME Rabinowitz, DL Ragozzine, D AF Schwamb, Megan E. Brown, Michael E. Rabinowitz, David L. Ragozzine, Darin TI PROPERTIES OF THE DISTANT KUIPER BELT: RESULTS FROM THE PALOMAR DISTANT SOLAR SYSTEM SURVEY SO ASTROPHYSICAL JOURNAL LA English DT Article DE Kuiper Belt: general; Oort Cloud ID TRANS-NEPTUNIAN OBJECTS; EMBEDDED STAR-CLUSTERS; OORT CLOUD; CANDIDATE MEMBERS; SIZE DISTRIBUTION; STELLAR CLUSTERS; MOLECULAR CLOUDS; INFRARED IMAGES; SCATTERED DISK; PERIOD COMETS AB We present the results of a wide-field survey using the 1.2 m Samuel Oschin Telescope at Palomar Observatory. This survey was designed to find the most distant members of the Kuiper Belt and beyond. We searched similar to 12,000 deg(2) down to a mean limiting magnitude of 21.3 in R. A total number of 52 Kuiper Belt objects and Centaurs have been detected, 25 of which were discovered in this survey. Except for the redetection of Sedna, no additional Sedna-like bodies with perihelia greater than 45 AU were detected despite sensitivity out to distances of 1000 AU. We discuss the implications for a distant Sedna-like population beyond the Kuiper Belt, focusing on the constraints we can place on the embedded stellar cluster environment the early Sun may be have been born in, where the location and distribution of Sedna-like orbits sculpted by multiple stellar encounters is indicative of the birth cluster size. We also report our observed latitude distribution and implications for the size of the plutino population. C1 [Schwamb, Megan E.; Brown, Michael E.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Rabinowitz, David L.] Yale Univ, Dept Phys, New Haven, CT 06520 USA. [Ragozzine, Darin] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Schwamb, ME (reprint author), CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. EM mschwamb@gps.caltech.edu RI Ragozzine, Darin/C-4926-2013; OI Schwamb, Megan/0000-0003-4365-1455 FU NASA [NNG05GI02G] FX This research is supported by NASA Origins of Solar Systems Program grant NNG05GI02G. M. E. S. is supported by a NASA Earth and Space Science Fellowship. We are indebted to Ramon Brasser and Nathan Kaib for sharing the results of their cluster integrations and to J. J. Kavellaars, Brett Gladman, and Samantha Lawler for providing us with the nominal CFEPS plutino model. We thank the staff at Palomar Observatory for their dedicated support of the robotic operation of the Samuel Oschin Telescope and QUEST camera. The authors also thank Greg Aldering for his help in scheduling the observations. We acknowledge Mansi Kasliwal, Henry Roe, John Subasavage, Emily Schaller, and Richard Walters for their assistance with recovery observations of our new discoveries. We recognize the work of Christian Clanton for support in developing the dynamical integration tools. We also thank Wes Fraser, Ramon Brasser, and Nathan Kaib for insightful conversations. NR 79 TC 35 Z9 35 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 2010 VL 720 IS 2 BP 1691 EP 1707 DI 10.1088/0004-637X/720/2/1691 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 647ND UT WOS:000281624300062 ER PT J AU Lattanzi, V Gottlieb, CA Thaddeus, P Thorwirth, S McCarthy, MC AF Lattanzi, V. Gottlieb, C. A. Thaddeus, P. Thorwirth, S. McCarthy, M. C. TI THE ROTATIONAL SPECTRUM OF THE NCO- ANION SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual objects (Sgr B2); ISM: molecules; line: identification; molecular data; molecular processes; radio lines: ISM ID NEGATIVE-IONS; ASTRONOMICAL IDENTIFICATION; AUTODETACHMENT SPECTROSCOPY; LASER SPECTROSCOPY; COUPLED-CLUSTER; INTERSTELLAR; ACID; HNCO; CN; DYNAMICS AB The rotational spectrum of the negative molecular ion NCO- has been observed both in a supersonic molecular beam and in a low-pressure glow discharge. The identification is ironclad because of the previous infrared detection of NCO-, the presence of well-resolved nitrogen quadrupole hyperfine structure, and the observation of nine harmonically related transitions in the millimeter band. The spectroscopic constants B and D are three orders of magnitude more accurate than those derived from the earlier IR measurements, and the theoretical eQq is in good agreement with that measured. The entire rotational spectrum can now be calculated well into the THz region to 1 km s(-1) in equivalent radial velocity or better. NCO- is an excellent candidate for radio astronomical detection because of its high stability, polarity, and favorable partition function. The fairly high concentration of NCO- in our laboratory source implies that other molecular anions containing the NCO group may be detectable in the radio band. C1 [Lattanzi, V.; Gottlieb, C. A.; Thaddeus, P.; McCarthy, M. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lattanzi, V.; Gottlieb, C. A.; Thaddeus, P.; McCarthy, M. C.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. [Thorwirth, S.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Thorwirth, S.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. RP Lattanzi, V (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM vlattanzi@cfa.harvard.edu; cgottlieb@cfa.harvard.edu; pthaddeus@cfa.harvard.edu; sthorwirth@ph1.uni-koeln.de; mccarthy@cfa.harvard.edu RI Thorwirth, Sven/C-6217-2011; OI Thorwirth, Sven/0000-0001-8200-6710; McCarthy, Michael/0000-0001-9142-0008 FU NSF [CHE-0701204]; NASA [NNX08AE05G]; Deutsche Forschungsgemeinschaft [TH 1301/3-1] FX It is a pleasure to acknowledge R. Saykally for illuminating discussions on the production and detection of ions in the laboratory. The authors thank V. Bierbaum, E. Herbst, and A. Viggiano for comments on ion chemistry, and K. Oberg on interstellar ices; and M. Guelin for helpful discussions on the astronomical observations of negative ions. The work in Cambridge is supported by the NSF grant CHE-0701204 and NASA grant NNX08AE05G. S. T. is grateful to the Deutsche Forschungsgemeinschaft for a research grant (TH 1301/3-1). NR 39 TC 12 Z9 12 U1 5 U2 11 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 2010 VL 720 IS 2 BP 1717 EP 1720 DI 10.1088/0004-637X/720/2/1717 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 647ND UT WOS:000281624300064 ER PT J AU Luhman, KL Mamajek, EE Allen, PR Muench, AA Finkbeiner, DP AF Luhman, K. L. Mamajek, E. E. Allen, P. R. Muench, A. A. Finkbeiner, D. P. TI DISCOVERY OF A WIDE BINARY BROWN DWARF BORN IN ISOLATION (vol 691, pg 1265, 2009) SO ASTROPHYSICAL JOURNAL LA English DT Correction C1 [Luhman, K. L.; Allen, P. R.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Mamajek, E. E.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. [Muench, A. A.; Finkbeiner, D. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Luhman, KL (reprint author), Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. EM kluhman@astro.psu.edu NR 7 TC 3 Z9 3 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 2010 VL 720 IS 2 BP 1781 EP 1781 DI 10.1088/0004-637X/720/2/1781 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 647ND UT WOS:000281624300071 ER PT J AU Drake, JJ Orlando, S AF Drake, J. J. Orlando, S. TI THE EARLY BLAST WAVE OF THE 2010 EXPLOSION OF U SCORPII SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE methods: numerical; novae, cataclysmic variables; shock waves; stars: individual (U Sco); X-rays: binaries ID NOVA RS-OPHIUCHI; X-RAY-EMISSION; 2006 OUTBURST; RECURRENT NOVAE; SUPERNOVA-REMNANTS; WHITE-DWARF; SPECTROSCOPY; HYDRODYNAMICS; SIMULATIONS; ACCRETION AB Three-dimensional hydrodynamic simulations exploring the first 18 hr of the 2010 January 28 outburst of the recurrent nova U Scorpii have been performed. Special emphasis was placed on capturing the enormous range in spatial scales in the blast. The pre-explosion system conditions included the secondary star and a flared accretion disk. These conditions can have a profound influence on the evolving blast wave. The blast itself is shadowed by the secondary star, which itself gives rise to a low-temperature bow shock. The accretion disk is completely destroyed in the explosion. A model with a disk gas density of 10(15) cm(-3) produced a blast wave that is collimated and with clear bipolar structures, including a bipolar X-ray emitting shell. The degree of collimation depends on the initial mass of ejecta, energy of explosion, and circumstellar gas density distribution. It is most pronounced for a model with the lowest explosion energy (10(43) erg) and mass of ejecta (10(-8) M(circle dot)). The X-ray luminosities of three of six models computed are close to, but consistent with, an upper limit to the early blast X-ray emission obtained by the Swift satellite, the X-ray luminosity being larger for higher circumstellar gas density and higher ejecta mass. The latter consideration, together with estimates of the blast energy from previous outbursts, suggests that the mass of ejecta in the 2010 outburst was not larger than 10(-7) M(circle dot). C1 [Drake, J. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Orlando, S.] INAF Osservatorio Astron Palermo GS Vaiana, I-90134 Palermo, Italy. RP Drake, JJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Orlando, Salvatore/0000-0003-2836-540X FU NASA [NAS8-39073]; DOE FX J.J.D. was funded by NASA contract NAS8-39073 to the Chandra X-ray Center. FLASH was developed by the DOE-supported ASC/Alliance Center for Astrophysical Thermonuclear Flashes, University of Chicago. Simulations were executed at the HPC SCAN facility of INAF-OAPA. NR 47 TC 19 Z9 19 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD SEP 10 PY 2010 VL 720 IS 2 BP L195 EP L200 DI 10.1088/2041-8205/720/2/L195 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 647HX UT WOS:000281610200014 ER PT J AU Magdis, GE Elbaz, D Hwang, HS Daddi, E Rigopoulou, D Altieri, B Andreani, P Aussel, H Berta, S Cava, A Bongiovanni, A Cepa, J Cimatti, A Dickinson, M Dominguez, H Schreiber, NF Genzel, R Huang, JS Lutz, D Maiolino, R Magnelli, B Morrison, GE Nordon, R Garcia, AMP Poglitsch, A Popesso, P Pozzi, F Riguccini, L Rodighiero, G Saintonge, A Santini, P Sanchez-Portal, M Shao, L Sturm, E Tacconi, L Valtchanov, I AF Magdis, G. E. Elbaz, D. Hwang, H. S. Daddi, E. Rigopoulou, D. Altieri, B. Andreani, P. Aussel, H. Berta, S. Cava, A. Bongiovanni, A. Cepa, J. Cimatti, A. Dickinson, M. Dominguez, H. Schreiber, N. Foerster Genzel, R. Huang, J. -S. Lutz, D. Maiolino, R. Magnelli, B. Morrison, G. E. Nordon, R. Garcia, A. M. Perez Poglitsch, A. Popesso, P. Pozzi, F. Riguccini, L. Rodighiero, G. Saintonge, A. Santini, P. Sanchez-Portal, M. Shao, L. Sturm, E. Tacconi, L. Valtchanov, I. TI A FIRST GLIMPSE INTO THE FAR-IR PROPERTIES OF HIGH-z UV-SELECTED GALAXIES: HERSCHEL/PACS OBSERVATIONS OF z similar to 3 LBGS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE cosmology: observations; galaxies: evolution; galaxies: formation; galaxies: general; galaxies: high-redshift; infrared: galaxies ID LYMAN-BREAK GALAXIES; ULTRALUMINOUS INFRARED GALAXIES; STAR-FORMATION; STELLAR MASSES; DUST; MULTIWAVELENGTH; Z-SIMILAR-TO-3; POPULATION; SPECTRA AB We present first insights into the far-IR properties for a sample of IRAC and MIPS 24 mu m detected Lyman break galaxies (LBGs) at z similar to 3, as derived from observations in the northern field of the Great Observatories Origins Survey (GOODS-N) carried out with the PACS instrument on board the Herschel Space Observatory. Although none of our galaxies are detected by Herschel, we employ a stacking technique to construct, for the first time, the average spectral energy distribution (SED) of infrared luminous LBGs from UV to radio wavelengths. We derive a median IR luminosity of L(IR) = 1.6 x 10(12) L(circle dot), placing the population in the class of ultra-luminous infrared galaxies (ULIRGs). Complementing our study with existing multi-wavelength data, we put constraints on the dust temperature of the population and find that for their L(IR), MIPS-LBGs are warmer than submillimeter-luminous galaxies while they fall in the locus of the L(IR)-T(d) relation of the local ULIRGs. This, along with estimates based on the average SED, explains the marginal detection of LBGs in current submillimeter surveys and suggests that these latter studies introduce a bias toward the detection of colder ULIRGs in the high-z universe, while missing high-z ULIRGS with warmer dust. C1 [Magdis, G. E.; Elbaz, D.; Hwang, H. S.; Daddi, E.; Aussel, H.; Riguccini, L.] CEA, Lab AIM, Irfu SAp, F-91191 Gif Sur Yvette, France. [Rigopoulou, D.] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England. European Space Astron Ctr, Villafrance del Castillo, Spain. [Andreani, P.] ESO, D-85748 Garching, Germany. [Berta, S.; Schreiber, N. Foerster; Genzel, R.; Lutz, D.; Magnelli, B.; Nordon, R.; Poglitsch, A.; Popesso, P.; Saintonge, A.; Sanchez-Portal, M.; Shao, L.; Sturm, E.; Tacconi, L.] Max Planck Inst Extraterr Phys MPE, D-85741 Garching, Germany. [Cava, A.; Bongiovanni, A.; Cepa, J.; Garcia, A. M. Perez] Inst Astrofis Canarias, San Cristobal la Laguna 38205, Spain. [Cimatti, A.; Rodighiero, G.] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy. [Dickinson, M.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Dominguez, H.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy. [Huang, J. -S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Maiolino, R.; Pozzi, F.; Santini, P.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy. [Morrison, G. E.] Univ Hawaii, Inst Astron, Honolulu, HI USA. [Morrison, G. E.] Canada France Hawaii Telescope Corp, Kamuela, HI 96743 USA. [Valtchanov, I.] European Space Astron Ctr, Herschel Sci Ctr, Villafranca Castillo Satellite Tracking Stn, Madrid, Spain. RP Magdis, GE (reprint author), CEA, Lab AIM, Irfu SAp, F-91191 Gif Sur Yvette, France. RI Daddi, Emanuele/D-1649-2012; Magdis, Georgios/C-7295-2014; Bongiovanni, Angel/J-6176-2012; Cava, Antonio/C-5274-2017; OI Daddi, Emanuele/0000-0002-3331-9590; Magdis, Georgios/0000-0002-4872-2294; Cava, Antonio/0000-0002-4821-1275; Santini, Paola/0000-0002-9334-8705; Altieri, Bruno/0000-0003-3936-0284 FU BMVIT (Austria); ESA-PRODEX (Belgium); CEA/CNES (France); DLR (Germany); ASI (Italy); CICT/MCT (Spain) FX PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KUL, CSL, IMEC (Belgium); CEA, OAMP (France); MPIA (Germany); IFSI, OAP/AOT, OAA/CAISMI, LENS, SISSA (Italy); and IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI (Italy), and CICT/MCT (Spain). NR 33 TC 30 Z9 30 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD SEP 10 PY 2010 VL 720 IS 2 BP L185 EP L189 DI 10.1088/2041-8205/720/2/L185 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 647HX UT WOS:000281610200012 ER PT J AU Matranga, M Drake, JJ Kashyap, VL Marengo, M Kuchner, MJ AF Matranga, M. Drake, J. J. Kashyap, V. L. Marengo, M. Kuchner, M. J. TI CLOSE BINARIES WITH INFRARED EXCESS: DESTROYERS OF WORLDS? SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE binaries: close; circumstellar matter; infrared: stars; stars: individual (AR Psc, II Peg, UX Ari) ID RS CANUM-VENATICORUM; SUN-LIKE; DEBRIS DISKS; PHOTOMETRIC-OBSERVATIONS; RESONANT SIGNATURES; PLANETARY SYSTEMS; ACTIVE STARS; SPITZER MIPS; WARM DUST; II PEGASI AB We present the results of a Spitzer photometric investigation into the IR excesses of close binary systems. In a sample of 10 objects, excesses in Infrared Array Camera and MIPS24 bands implying the presence of warm dust are found for 3. For two objects, we do not find excesses reported in earlier IRAS studies. We discuss the results in the context of the scenario suggested by Rhee and co-workers, in which warm dust is continuously created by destructive collisions between planetary bodies. A simple numerical model for the steady-state distribution of dust in one IR excess system shows a central clearing of radius 0.22 AU caused by dynamical perturbations from the binary star. This is consistent with the size of the central clearing derived from the Spitzer spectral energy distribution. We conclude that close binaries could be efficient "destroyers of worlds" and lead to destabilization of the orbits of their planetary progeny by magnetically driven angular momentum loss and secular shrinkage of the binary separation. C1 [Matranga, M.; Drake, J. J.; Kashyap, V. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Marengo, M.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Kuchner, M. J.] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab Greenbelt, Greenbelt, MD 20771 USA. RP Matranga, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Kuchner, Marc/E-2288-2012 FU Spitzer [1279130]; NASA [NAS8-39073, 1407] FX M. Matranga was supported by Spitzer contract 1279130. J.J.D. and V. L. K. were funded by the NASA contract NAS8-39073 to the Chandra X-ray Center. Observations were made with Spitzer, operated by JPL under the NASA contract 1407. NR 47 TC 5 Z9 6 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD SEP 10 PY 2010 VL 720 IS 2 BP L164 EP L168 DI 10.1088/2041-8205/720/2/L164 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 647HX UT WOS:000281610200008 ER PT J AU Mueller, UG Scott, JJ Ishak, HD Cooper, M Rodrigues, A AF Mueller, Ulrich G. Scott, Jarrod J. Ishak, Heather D. Cooper, Michael Rodrigues, Andre TI Monoculture of Leafcutter Ant Gardens SO PLOS ONE LA English DT Article ID FUNGUS-GROWING ANTS; LEAF-CUTTER ANTS; ATTINE ANT; DISEASE MANAGEMENT; SYMBIONT CHOICE; ATTA-SEXDENS; EVOLUTION; FORMICIDAE; COOPERATION; CONFLICT AB Background: Leafcutter ants depend on the cultivation of symbiotic Attamyces fungi for food, which are thought to be grown by the ants in single-strain, clonal monoculture throughout the hundreds to thousands of gardens within a leafcutter nest. Monoculture eliminates cultivar-cultivar competition that would select for competitive fungal traits that are detrimental to the ants, whereas polyculture of several fungi could increase nutritional diversity and disease resistance of genetically variable gardens. Methodology/Principal Findings: Using three experimental approaches, we assessed cultivar diversity within nests of Atta leafcutter ants, which are most likely among all fungus-growing ants to cultivate distinct cultivar genotypes per nest because of the nests' enormous sizes (up to 5000 gardens) and extended lifespans (10-20 years). In Atta texana and in A. cephalotes, we resampled nests over a 5-year period to test for persistence of resident cultivar genotypes within each nest, and we tested for genetic differences between fungi from different nest sectors accessed through excavation. In A. texana, we also determined the number of Attamyces cells carried as a starter inoculum by a dispersing queens (minimally several thousand Attamyces cells), and we tested for genetic differences between Attamyces carried by sister queens dispersing from the same nest. Except for mutational variation arising during clonal Attamyces propagation, DNA fingerprinting revealed no evidence for fungal polyculture and no genotype turnover during the 5-year surveys. Conclusions/Significance: Atta leafcutter ants can achieve stable, fungal monoculture over many years. Mutational variation emerging within an Attamyces monoculture could provide genetic diversity for symbiont choice (gardening biases of the ants favoring specific mutational variants), an analog of artificial selection. C1 [Mueller, Ulrich G.; Scott, Jarrod J.; Ishak, Heather D.; Cooper, Michael; Rodrigues, Andre] Univ Texas Austin, Sect Integrat Biol, Austin, TX 78712 USA. [Mueller, Ulrich G.; Scott, Jarrod J.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Scott, Jarrod J.] Univ Wisconsin, Dept Bacteriol, Madison, WI 53706 USA. [Rodrigues, Andre] State Univ Sao Paulo UNESP, Ctr Study Social Insects, Sao Paulo, Brazil. [Rodrigues, Andre] Santa Cruz State Univ UESC, Dept Biol Sci, Ilheus, BA, Brazil. RP Mueller, UG (reprint author), Univ Texas Austin, Sect Integrat Biol, Austin, TX 78712 USA. EM umueller@mail.utexas.edu RI Rodrigues, Andre/B-8148-2012 OI Rodrigues, Andre/0000-0002-4164-9362 FU National Science Foundation [DEB-0920138, DEB-0639879, DEB-0110073, DEB-0949689]; Conselho Nacional de Desenvolvimento Cientifico e Tecnologico [02/05] FX The research was supported by National Science Foundation awards DEB-0920138, DEB-0639879, and DEB-0110073 to UGM; DEB-0949689 to T. R. Schultz, N. Mehdiabadi, and UGM; and a Fellowship (02/05) from the Conselho Nacional de Desenvolvimento Cientifico e Tecnologico to AR. The funding agencies had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 71 TC 18 Z9 18 U1 3 U2 23 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD SEP 10 PY 2010 VL 5 IS 9 AR e12668 DI 10.1371/journal.pone.0012668 PG 7 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 648IX UT WOS:000281687300012 ER PT J AU Onofrio, R AF Onofrio, Roberto TI Higgs-induced spectroscopic shifts near strong gravity sources SO PHYSICAL REVIEW D LA English DT Article ID GALACTIC-CENTER REGION; SAGITTARIUS A-ASTERISK; ENERGY-MOMENTUM TENSOR; GAUGE FIELD-THEORIES; BLACK-HOLE; MASSLESS PARTICLES; MOLECULAR CLOUD; CARBON-MONOXIDE; PROPER-MOTION; GALAXY AB We explore the consequences of the mass generation due to the Higgs field in strong gravity astrophysical environments. The vacuum expectation value of the Higgs field is predicted to depend on the curvature of spacetime, potentially giving rise to peculiar spectroscopic shifts, named hereafter "Higgs shifts." Higgs shifts could be searched through dedicated multiwavelength and multispecies surveys with high spatial and spectral resolution near strong gravity sources such as Sagittarius A* or broad searches for signals due to primordial black holes. The possible absence of Higgs shifts in these surveys should provide limits to the coupling between the Higgs particle and the curvature of spacetime, a topic of interest for a recently proposed Higgs-driven inflationary model. We discuss some conceptual issues regarding the coexistence between the Higgs mechanism and gravity, especially for their different handling of fundamental and composite particles. C1 [Onofrio, Roberto] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy. [Onofrio, Roberto] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Onofrio, R (reprint author), Univ Padua, Dipartimento Fis G Galilei, Via Marzolo 8, I-35131 Padua, Italy. EM onofrior@gmail.com FU Julian Schwinger Foundation [JSF 08070000] FX We are grateful to F. de Felice for fruitful discussions, and H. R. Sadeghpour and L. Viola for a critical reading of the manuscript. Partial support from the Julian Schwinger Foundation through grant JSF 08070000 on Astrophysics of Quantum Vacuum is also acknowledged. NR 51 TC 9 Z9 9 U1 0 U2 2 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1550-7998 J9 PHYS REV D JI Phys. Rev. D PD SEP 9 PY 2010 VL 82 IS 6 AR 065008 DI 10.1103/PhysRevD.82.065008 PG 5 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 647ZI UT WOS:000281659000004 ER PT J AU O'Byrne, G Martin, RV van Donkelaar, A Joiner, J Celarier, EA AF O'Byrne, G. Martin, R. V. van Donkelaar, A. Joiner, J. Celarier, E. A. TI Surface reflectivity from the Ozone Monitoring Instrument using the Moderate Resolution Imaging Spectroradiometer to eliminate clouds: Effects of snow on ultraviolet and visible trace gas retrievals SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID NORTHERN-HEMISPHERE; SPECTRAL ALBEDO; GOME MEASUREMENTS; TROPOSPHERIC NO2; COVERED SURFACES; MODIS; PRODUCTS; SPACE; UV; ALGORITHM AB Satellite retrievals of tropospheric composition from measurements of solar backscatter require accurate information about surface reflectivity. We use clear-sky data from the Ozone Monitoring Instrument (OMI) to determine global surface reflectivity under both snow-covered and snow-free conditions at 354 nm. Clear-sky scenes are determined using cloud and aerosol data from the Moderate Resolution Imaging Spectroradiometer/Aqua satellite instrument that flies 12 min ahead of OMI/Aura. The result is a database of OMI-observed Lambertian equivalent reflectivity (LER) that does not rely on statistical methods to eliminate cloud and aerosol contamination. We apply this database to evaluate previous climatologies of surface reflectivity. Except for regions of seasonal snow cover, agreement is best with a climatology from OMI, which selects the surface reflectivity from a histogram of observed LER (mean difference, 0.0002; standard deviation, 0.011). Three other climatologies of surface reflectivity from Total Ozone Mapping Spectrometer, Global Ozone Monitoring Experiment, and OMI, based on minimum observed LER, are less consistent with our cloud-and aerosol-filtered data set (mean difference, -0.008, 0.012, and -0.002; standard deviation, 0.022, 0.026, and 0.033). Snow increases the sensitivity of solar backscatter measurements at ultraviolet and visible wavelengths to trace gases in the lower troposphere. However, all four existing LER climatologies poorly represent seasonal snow. Surface reflectivity over snow-covered lands depends strongly on the vegetation type covering the surface. The monthly variation of snow-covered reflectivity varies by less than 0.1 in fall and winter. Applying our snow-covered surface reflectivity database to OMI NO2 retrievals could change the retrieved NO2 column by 20%-50% over large regions with seasonal snow cover. C1 [O'Byrne, G.; Martin, R. V.; van Donkelaar, A.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 3J5, Canada. [Martin, R. V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Joiner, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Celarier, E. A.] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. RP O'Byrne, G (reprint author), Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 3J5, Canada. EM randall.martin@dal.ca RI Joiner, Joanna/D-6264-2012; Martin, Randall/C-1205-2014 OI Martin, Randall/0000-0003-2632-8402 FU NASA; Canadian Foundation for Climate and Atmospheric Science FX Terry O'Byrne and two anonymous reviewers provided helpful comments that improved this manuscript. We thank the OMI and MODIS teams as well as Environment Canada for making their data publicly available. This research was supported by NASA and the Canadian Foundation for Climate and Atmospheric Science. NR 57 TC 10 Z9 10 U1 0 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD SEP 8 PY 2010 VL 115 AR D17305 DI 10.1029/2009JD013079 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 649GF UT WOS:000281755400002 ER PT J AU Chesser, RT Yeung, CKL Yao, CT Tian, XH Li, SH AF Chesser, R. Terry Yeung, Carol K. L. Yao, Cheng-Te Tian, Xiu-Hua Li, Shou-Hsien TI Molecular phylogeny of the spoonbills (Aves: Threskiornithidae) based on mitochondrial DNA SO ZOOTAXA LA English DT Article DE spoonbills; Platalea; Threskiornithidae; mitochondrial DNA ID LIKELIHOOD; ACCURATE; MODELS; BIRDS AB Spoonbills (genus Platalea) are a small group of wading birds, generally considered to constitute the subfamily Plataleinae (Aves: Threskiornithidae). We reconstructed phylogenetic relationships among the six species of spoonbills using variation in sequences of the mitochondrial genes ND2 and cytochrome b (total 1796 bp). Topologies of phylogenetic trees reconstructed using maximum likelihood, maximum parsimony, and Bayesian analyses were virtually identical and supported monophyly of the spoonbills. Most relationships within Platalea received strong support: P. minor and P. regia were closely related sister species, P. leucorodia was sister to the minor-regia clade, and P. alba was sister to the minor-regia-leucorodia clade. Relationships of P. flavipes and P. ajaja were less well resolved: these species either formed a clade that was sister to the four-species clade, or were successive sisters to this clade. This phylogeny is consistent with ideas of relatedness derived from spoonbill morphology. Our limited sampling of the Threskiornithinae (ibises), the putative sister group to the spoonbills, indicated that this group is paraphyletic, in agreement with previous molecular data; this suggests that separation of the Threskiornithidae into subfamilies Plataleinae and Threskiornithinae may not be warranted. C1 [Chesser, R. Terry] Smithsonian Inst, Natl Museum Nat Hist, Patuxent Wildlife Res Ctr, US Geol Survey, Washington, DC 20560 USA. [Yeung, Carol K. L.; Li, Shou-Hsien] Natl Taiwan Normal Univ, Dept Life Sci, Taipei 11677, Taiwan. [Yao, Cheng-Te] Endem Species Res Inst, Chi Chi 552, Nantou, Taiwan. [Yao, Cheng-Te] Natl Cheng Kung Univ, Dept Life Sci, Tainan 701, Taiwan. [Tian, Xiu-Hua] NE Forestry Univ, Coll Wildlife, Harbin 150040, Peoples R China. RP Chesser, RT (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Patuxent Wildlife Res Ctr, US Geol Survey, Washington, DC 20560 USA. FU National Science Council, Taiwan, R.O.C. FX We thank the American Museum of Natural History, New York, and the Australian National Wildlife Collection, Canberra, for providing samples, and two anonymous reviewers for comments on the manuscript. This work was supported by grants to S.-H.L. from the National Science Council, Taiwan, R.O.C. Use of trade, product, or firm names does not imply endorsement by the U.S. Government. NR 23 TC 8 Z9 8 U1 3 U2 8 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD SEP 6 PY 2010 IS 2603 BP 53 EP 60 PG 8 WC Zoology SC Zoology GA 646GD UT WOS:000281525600002 ER PT J AU Murphy, NA Sovinec, CR Cassak, PA AF Murphy, N. A. Sovinec, C. R. Cassak, P. A. TI Magnetic reconnection with asymmetry in the outflow direction SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID CORONAL MASS EJECTION; TIME-DEPENDENT RECONNECTION; DRIVEN STELLAR WINDS; CME CURRENT SHEETS; X-LINE; DENSITY ASYMMETRY; GEOMAGNETIC TAIL; MHD SIMULATIONS; ACTIVE-REGION; SOLAR-FLARES AB Magnetic reconnection with asymmetry in the outflow direction occurs in the Earth's magnetotail, coronal mass ejections, flux cancellation events, astrophysical disks, spheromak merging experiments, and elsewhere in nature and the laboratory. A control volume analysis is performed for the case of steady antiparallel magnetic reconnection with asymmetric downstream pressure to derive scaling relations for the outflow velocity from each side of the current sheet and the reconnection rate. Simple relationships for outflow velocity are presented for the incompressible case and the case of symmetric downstream pressure but asymmetric downstream density. Asymmetry alone is not found to greatly affect the reconnection rate. The flow stagnation point and magnetic field null do not coincide in a steady state unless the pressure gradient is negligible at the flow stagnation point. The predictions of the model are compared with resistive MHD simulations of driven reconnection with asymmetry in the outflow direction. C1 [Murphy, N. A.; Sovinec, C. R.] Univ Wisconsin, Ctr Magnet Self Org Lab & Astrophys Plasmas, Madison, WI 53706 USA. [Murphy, N. A.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Sovinec, C. R.] Univ Wisconsin, Dept Engn Phys, Madison, WI 53706 USA. [Cassak, P. A.] W Virginia Univ, Dept Phys, Morgantown, WV 26506 USA. RP Murphy, NA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 16, Cambridge, MA 02138 USA. EM namurphy@cfa.harvard.edu OI Murphy, Nicholas/0000-0001-6628-8033 FU NSF, through the Center for Magnetic Self-Organization in Laboratory and Astrophysical Plasmas [PHY-0821899]; NASA [NNX09AB17G]; NSF [PHY-0902479] FX The authors thank Ellen Zweibel, Jennifer Stone, Michiaki Inomoto, John Raymond, Ping Zhu, Yi-Min Huang, Michael Shay, Clare Parnell, Dmitri Uzdensky, Mitsuo Oka, Joseph Cassinelli, Richard Townsend, K. Tabetha Hole, John Everett, Seth Dorfman, and Samuel Friedman for useful discussions. N. A. M. and C. R. S. acknowledge support from NSF grant PHY-0821899 through the Center for Magnetic Self-Organization in Laboratory and Astrophysical Plasmas. N. A. M. acknowledges additional support from NASA grant NNX09AB17G to the Smithsonian Astrophysical Observatory. P. A. C. acknowledges support from NSF grant PHY-0902479. This research has benefited from use of NASA's Astrophysics Data System Bibliographic Services. NR 95 TC 21 Z9 21 U1 1 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD SEP 4 PY 2010 VL 115 AR A09206 DI 10.1029/2009JA015183 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 647QM UT WOS:000281633700003 ER PT J AU Zatwarnicki, T Mathis, WN AF Zatwarnicki, Tadeusz Mathis, Wayne N. TI A Revision of the nivea Group of the Shore-fly Genus Ditrichophora Cresson (Diptera: Ephydridae) SO TRANSACTIONS OF THE AMERICAN ENTOMOLOGICAL SOCIETY LA English DT Article DE Revision; Diptera; Ephydridae; shore flies; Ditrichophora; Holarctic Region AB Species of the nivea group (genus Ditrichophora Cresson) are revised. The group now includes four species of which one, D. gulkana (Alaska and Mongolia), is newly described. The group is now known to have a Holarctic distribution with two species, D. gulkana and D. nivea, being the first reported from the Nearctic Region. Another Asian species, D. brunnicosa, previously placed in Diclasiopa, is transferred to this group (genus Ditrichophora) and is also reported from Mongolia. To facilitate identification of these rare species, we have included diagnoses of the tribe, genus, and species group and have also provided an annotated key to Holarctic genera of the tribe Discocerinini and to species of the nivea group within Ditrichophora. We also provide the first illustrations of male terminalia for all included species. C1 [Zatwarnicki, Tadeusz] Opole Univ, Dept Biosystemat, PL-45052 Opole, Poland. [Mathis, Wayne N.] Dept Entomol, Washington, DC 20013 USA. Smithsonian Inst, Washington, DC 20013 USA. RP Zatwarnicki, T (reprint author), Opole Univ, Dept Biosystemat, Ul Oleska 22, PL-45052 Opole, Poland. EM zatwar@uni.opole.pl; mathisw@si.edu OI Zatwarnicki, Tadeusz/0000-0003-2163-0143 FU Altai and Hangai Mountains' drainages, Mongolia; United States National Science Foundation [DEB-0743732] FX Field work in Mongolia was generously supported by a grant entitled "Survey and Inventory of the Aquatic Insects of the Altai and Hangai Mountains' drainages, Mongolia" awarded to J. Gelhaus, J. Morse, C. R. Nelson. United States National Science Foundation: Biodiversity Inventories Program (DEB-0743732), awarded for 2008-2011. We are especially indebted to the principal investigators, Jon K. Gelhaus in particular, for inviting us to participate in the program and field work in the summer of 2009. NR 28 TC 0 Z9 0 U1 0 U2 1 PU AMER ENTOMOL SOC PI PHILADELPHIA PA 1900 BENJ FRANKLIN PARKWAY, PHILADELPHIA, PA 19103-1195 USA SN 0002-8320 J9 T AM ENTOMOL SOC JI Trans. Am. Entomol. Soc. PD SEP-DEC PY 2010 VL 136 IS 3-4 BP 199 EP 215 PG 17 WC Entomology SC Entomology GA 716EF UT WOS:000286951200001 ER PT J AU Fornshell, JA Tesei, A Fox, PD AF Fornshell, John A. Tesei, Alessandra Fox, Paul D. TI Acoustic Signatures of Three Marine Arthropods, Squilla mantis (Linnaeus, 1758), Homarus americanus (H. Milne Edwards, 1837), and Nephrops norvegicus (Linnaeus, 1758) (Arthropoda, Malacostraca) SO MARINE TECHNOLOGY SOCIETY JOURNAL LA English DT Article ID ZOOPLANKTON GROUPS; SOUND-SCATTERING; LOBSTER; MECHANISMS AB The acoustic signatures of three marine crustaceans, Squilla mantis (Linnaeus, 1758), Homarus americanus (H. Milne Edwards, 1837), and Nephrops norvegicus (Linnaeus 1758) (Arthropoda, Malacostraca), were experimetally determined in measurements using the calibration tank at the NATO Undersea Research Center, Le Spezia, Italy. The specimens were insonified at 45 rotational intervals with a sound source emitting pings from 30 to 120 kHz. For all three species, the value of the nondimensional parameter ka (where k is the acoustic wave number and a is the characteristic dimension of the object) was 5. The absorption specta, defined as the frequencies at which the intensity of the reflected sound was less than 5% of the incident intensity, were determined. These sepctra changed with the changing aspects and were unique for each animal in this study. Two of the species were in the same infraorder. Astacidea, Our reults contribute to the development of an acoustic identification system for surveys of marine animals. C1 [Fornshell, John A.] Smithsonian Inst, NATO Undersea Res Ctr NURC, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. [Tesei, Alessandra; Fox, Paul D.] Univ Southampton, Inst Sound & Vibrat Res, Southampton, Hants, England. RP Fornshell, JA (reprint author), Smithsonian Inst, NATO Undersea Res Ctr NURC, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. EM johnfornshell@hotmail.com FU NATO Undersea Research Centre (Italy) FX The NATO Undersea Research Centre (Italy) is gratefully acknowledged for having hosted John Fornshell and Paul Fox as Visiting Scientists during the period of the experimental work undertaken under the NURC Visiting Researchers Program 2009 and for providing all related facilities, support, and finance during that period. The Smithsonian Institution (USA) and the Institute of Sound and Vibration Research (UK) are also thanked for their affiliated support during the completion of the work. NR 28 TC 0 Z9 0 U1 0 U2 3 PU MARINE TECHNOLOGY SOC INC PI COLUMBIA PA 5565 STERRETT PLACE, STE 108, COLUMBIA, MD 21044 USA SN 0025-3324 J9 MAR TECHNOL SOC J JI Mar. Technol. Soc. J. PD SEP-OCT PY 2010 VL 44 IS 5 BP 67 EP 80 PG 14 WC Engineering, Ocean; Oceanography SC Engineering; Oceanography GA 679TP UT WOS:000284184000008 ER PT J AU Mawdsley, JR Sithole, H AF Mawdsley, Jonathan R. Sithole, Hendrik TI Diversity and abundance of insect visitors to flowers of trees and shrubs in a South African savannah SO AFRICAN JOURNAL OF ECOLOGY LA English DT Article DE landscape ecology; pollination; savannah; South Africa ID ACACIA-NIGRESCENS; POLLINATION; FABACEAE AB This study presents the results of a landscape-scale survey for insect floral visitors in the Skukuza Ranger District, Kruger National Park, South Africa. Floral visitors were sampled from flowering trees and shrubs along linear transects spanning the entire district. Six plant species were sampled in the late dry season (Acacia grandicornuta Gerstner, A. nigrescens Oliver, Cassia abbreviata Oliver, Combretum hereroense Schinz, Combretum zeyheri Sonder, Euclea divonorum Hiern), and eleven plant species were sampled during the rainy season (Acacia exuvialis Verdcourt, A. grandicornuta Gerstner, A. nilotica (L.) Willdenow, A. tortilis (Forsskal) Hayne, Dichrostachys cinerea Miquel, Flueggea virosa (Roxburgh) Baillon, Grewia bicolor Jussieu, G. flava De Candolle, G. flavescens Jussieu, G. monticola Sonder, and Peltophorum africanum Sonder). Coleoptera, Hymenoptera and Lepidoptera comprised the majority of floral visitors, while species of Blattodea, Diptera, Hemiptera and Neuroptera also occurred on flowers. Known or likely pollinators include bees (Hymenoptera: Apidae, Halictidae and Megachilidae) and scarab beetles (Coleoptera: Scarabaeidae). These plant species appear to have generalist pollination systems, with the exception of species of Grewia L., which appear to be pollinated primarily by bees. A provisional plant-pollinator food web is presented for the eleven species of trees and shrubs which flower during the rainy season.Resume Cet article presente les resultats d'une etude, realisee a l'echelle du paysage, des insectes qui visitent les fleurs dans le Skukuza Ranger District, dans le Parc National Kruger, en Afrique du Sud. Les insectes butineurs ont ete preleves dans des arbres et des arbustes en fleurs le long de transects lineaires qui traversent tout le district. On a echantillonne six especes vegetales en fin de saison seche (Acacia grandicornuta Gerstner, A. nigrescens Oliver, Cassia abbreviata Oliver, Combretum hereroense Schinz, Combretum zeyheri Sonder et Euclea divonorum Hiern), et 11 pendant la saison des pluies (Acacia exuvialis Verdcourt, A. grandicornuta Gerstner, A. nilotica (L.) Willdenow, A. tortilis (Forsskal) Hayne, Dichrostachys cinerea Miquel, Flueggea virosa (Roxburgh) Baillon, Grewia bicolor Jussieu, G. flava De Candolle, G. flavescens Jussieu, G. monticola Sonder, et Peltophorum africanum Sonder). Coleopteres, hymenopteres et lepidopteres composaient la majorite des insectes qui visitaient les fleurs et l'on voyait aussi sur les fleurs des especes de blattodees, de dipteres, d'hemipteres et de neuropteres. Les pollinisateurs connus ou supposes incluent des abeilles (Hymenopteres : Apides, Halictides et Megachilides) et des scarabees (Coleopteres : Scarabeides). Ces especes vegetales semblent avoir des systemes de pollinisation generalistes, a l'exception d'especes de Grewia L. qui semblent etre fertilises d'abord par les abeilles. Un reseau alimentaire provisoire plantes-pollinisateurs est presente pour les 11 especes d'arbres et d'arbustes qui fleurissent pendant la saison des pluies. C1 [Mawdsley, Jonathan R.] Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, MRC 187, Washington, DC 20013 USA. [Sithole, Hendrik] Kruger Natl Pk, ZA-1350 Skukuza, South Africa. RP Mawdsley, JR (reprint author), Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, MRC 187, POB 37012, Washington, DC 20013 USA. EM mawdsley@heinzctr.org NR 21 TC 4 Z9 4 U1 2 U2 23 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0141-6707 J9 AFR J ECOL JI Afr. J. Ecol. PD SEP PY 2010 VL 48 IS 3 BP 691 EP 698 DI 10.1111/j.1365-2028.2009.01166.x PG 8 WC Ecology SC Environmental Sciences & Ecology GA 634WV UT WOS:000280617600014 ER PT J AU Arnoldi, MJ AF Arnoldi, Mary Jo TI Surfaces: Color, Substances, and Ritual Applications on African Sculpture SO AFRICAN STUDIES REVIEW LA English DT Book Review C1 [Arnoldi, Mary Jo] Smithsonian Inst, Washington, DC 20560 USA. RP Arnoldi, MJ (reprint author), Smithsonian Inst, Washington, DC 20560 USA. EM arnoldim@si.edu NR 1 TC 0 Z9 0 U1 0 U2 0 PU AFRICAN STUDIES REVIEW PI NEW BRUNSWICK PA RUTGERS, THE STATE UNIV NEW JERSEY, DOUGLAS CAMPUS, 132 GEORGE ST, NEW BRUNSWICK, NJ 08901-1400 USA SN 0002-0206 J9 AFR STUD REV JI Afr. Stud. Rev. PD SEP PY 2010 VL 53 IS 2 BP 221 EP 222 PG 2 WC Area Studies SC Area Studies GA 654HZ UT WOS:000282160400036 ER PT J AU Peterson, PM Romaschenko, K Johnson, G AF Peterson, Paul M. Romaschenko, Konstantin Johnson, Gabriel TI A PHYLOGENY AND CLASSIFICATION OF THE MUHLENBERGIINAE (POACEAE: CHLORIDOIDEAE: CYNODONTEAE) BASED ON PLASTID AND NUCLEAR DNA SEQUENCES SO AMERICAN JOURNAL OF BOTANY LA English DT Article DE biogeography; Chloridoideae; classification; ITS; Muhlenbergia; Muhlenbergiinae; phylogeny; plastid DNA sequences; Poaceae ID C-4 GRASSES; NORTH; EVOLUTION; ERAGROSTIDEAE; PLANTS; DISJUNCTIONS; GRAMINEAE; TORTOISE; AMERICA; ANATOMY AB Premise of the study : To understand the origins of C(4) grasslands, we must have a better interpretation of plant traits via phylogenetic reconstruction. Muhlenbergiinae, the largest subtribe of C(4) grasses in Mexico and the southwestern United States (with 176 species), is taxonomically poorly understood. Methods : We conducted a phylogenetic analysis of 47 genera and 174 species using six plastid regions (ndhA intron, ndhF, rps16-trnK, rps16 intron, rps3, and rpl32-trnL) and the nuclear ITS 1 and 2 (ribosomal internal transcribed spacer) regions to infer evolutionary relationships and revise the classification. Key results : In our analyses, Muhlenbergia (ca. 153 species) is paraphyletic, with nine genera (Aegopogon, Bealia, Blepharoneuron, Chaboissaea, Lycurus, Muhlenbergia, Pereilema, Redfieldia, Schaffnerella, and Schedonnardus) found nested within. We recognized the following five well-supported monophyletic lineages within Muhlenbergia : subg. Muhlenbergia, with species that have phosphoenolpyruvate carboxykinase-like leaf anatomy and long, scaly rhizomes; subg. Trichochloa with long-lived species that are relatively tall (up to 3 m); subg. Clomena with 3-nerved upper glumes; sect. Pseudosporobolus species with narrow panicles and plumbeous spikelets; and sect. Bealia species with lemmas with hairy margins and midveins. Conclusions: We propose expanding the circumscription of Muhlenbergia to include the other nine genera in this subtribe and make the following new combinations: Muhlenbergia subg. Bealia, M. diandra, M. geminiflora, M. paniculata, M. phleoides, M. subg. Pseudosporobolus (also lectotipified), M. solisii, M. tricholepis. We also propose several new names: M. ammophila, M. columbi, M. plumosa. Our phylograms suggest that Muhlenbergia originated in North America because the sister (Sohnsia filifolia and Scleropogoninae) is composed of predominantly North American species. C1 [Peterson, Paul M.; Romaschenko, Konstantin] Smithsonian Inst, Dept Bot MRC 166, Natl Museum Nat Hist, Washington, DC 20013 USA. [Romaschenko, Konstantin] Bot Inst Barcelona CSIC ICUB, Lab Mol Systemat, Barcelona 08038, Spain. [Johnson, Gabriel] Smithsonian Inst, Dept Bot, Suitland, MD 20746 USA. [Johnson, Gabriel] Smithsonian Inst, Labs Analyt Biol, Suitland, MD 20746 USA. RP Peterson, PM (reprint author), Smithsonian Inst, Dept Bot MRC 166, Natl Museum Nat Hist, Washington, DC 20013 USA. EM peterson@si.edu RI Romaschenko, Konstantin/K-3096-2014 OI Romaschenko, Konstantin/0000-0002-7248-4193 FU Smithsonian Institution; National Museum of Natural History; Scholarly Studies Program; Research Opportunities, Atherton Seidell Foundation; Biodiversity Surveys and Inventories Program FX The authors thank the National Geographic Society Committee for Research and Exploration, grant number 8087-06 for field support, the Smithsonian Institution's Restricted Endowments Fund, National Museum of Natural History Small Grants Fund, the Scholarly Studies Program, Research Opportunities, Atherton Seidell Foundation, and Biodiversity Surveys and Inventories Program for financial support, J. H. Kirkbride, Jr. for translating German, A. Touwaide for correcting the Latin, and two anonymous reviewers for suggesting improvements. NR 93 TC 21 Z9 23 U1 0 U2 7 PU BOTANICAL SOC AMER INC PI ST LOUIS PA PO BOX 299, ST LOUIS, MO 63166-0299 USA SN 0002-9122 J9 AM J BOT JI Am. J. Bot. PD SEP PY 2010 VL 97 IS 9 BP 1532 EP 1554 DI 10.3732/ajb.0900359 PG 23 WC Plant Sciences SC Plant Sciences GA 646KN UT WOS:000281539000012 PM 21616906 ER PT J AU Williams, EM Gordon, AD Richmond, BG AF Williams, E. M. Gordon, A. D. Richmond, B. G. TI Upper Limb Kinematics and the Role of the Wrist During Stone Tool Production SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Article DE extension; flexion; kinematics; mechanical work; stone tool production ID KNUCKLE-WALKING ANCESTOR; HUMAN-EVOLUTION; OVERARM THROWS; EARLY HOMINID; FOSSIL EVIDENCE; MOMENT ARMS; HUMAN HAND; JOINT; TECHNOLOGY; PATTERNS AB ated the shoulder joint from the elbow and wrist joints, suggesting a shared strategy employed in other contexts (e.g., throwing) to increase target accuracy. The knapping strategy included moving the wrist into peak extension (subject peak grand mean = 47.30 degrees) at the beginning of the downswing phase, which facilitated rapid wrist flexion and accelerated the hammerstone toward the nodule. This sequence resulted in the production of significantly more mechanical work, and therefore greater strike forces, than would otherwise be produced. Together these results represent a strategy for increasing knapping efficiency in Homo sapiens and point to aspects of skeletal anatomy that might be examined to assess potential knapping ability and efficiency in fossil hominin taxa. Am J Phys Anthropol 143:134-145, 2010. (C) 2010 Wiley-Liss, Inc.Past studies have hypothesized that aspects of hominin upper limb morphology are linked to the ability to produce stone tools. However, we lack the data on upper limb motions needed to evaluate the biomechanical context of stone tool production. This study seeks to better understand the biomechanics of stone tool-making by investigating upper limb joint kinematics, focusing on the role of the wrist joint, during simple flake production. We test the hypotheses, based on studies of other upper limb activities (e.g., throwing), that upper limb movements will occur in a proximal-to-distal sequence, culminating in rapid wrist flexion just prior to strike. Data were captured from four amateur knappers during simple flake production using a VICON motion analysis system (50 Hz). Results show that subjects utilized a proximal-to-distal joint sequence and disassoci C1 [Williams, E. M.] George Washington Univ, Hominid Paleobiol Doctoral Program, Dept Anthropol, Ctr Adv Study Hominid Paleobiol, Washington, DC 20052 USA. [Gordon, A. D.] SUNY Albany, Dept Anthropol, Albany, NY 12222 USA. [Richmond, B. G.] Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20560 USA. RP Williams, EM (reprint author), George Washington Univ, Hominid Paleobiol Doctoral Program, Dept Anthropol, Ctr Adv Study Hominid Paleobiol, 2110 G St NW, Washington, DC 20052 USA. EM emswill@gwmail.gwu.edu OI Gordon, Adam/0000-0002-1807-4644 FU National Science Foundation [IGERT DGE 9987590, DGE 0801634]; George Washington University; The George Washington University's Sigma Xi chapter FX Grant sponsor: National Science Foundation's Integrative Graduate Education and Research Traineeship; Grant numbers: IGERT DGE 9987590; Grant numbers: DGE 0801634. Grant sponsor: The George Washington University's Research Enhancement Fund. Grant sponsor: The George Washington University's Sigma Xi chapter. NR 69 TC 16 Z9 16 U1 4 U2 23 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0002-9483 EI 1096-8644 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PD SEP PY 2010 VL 143 IS 1 BP 134 EP 145 DI 10.1002/ajpa.21302 PG 12 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 643PE UT WOS:000281309500013 PM 20734439 ER PT J AU Wang, QA Smith, AL Strait, DS Wright, BW Richmond, BG Grosse, IR Byron, CD Zapata, U AF Wang, Qian Smith, Amanda L. Strait, David S. Wright, Barth W. Richmond, Brian G. Grosse, Ian R. Byron, Craig D. Zapata, Uriel TI The Global Impact of Sutures Assessed in a Finite Element Model of a Macaque Cranium SO ANATOMICAL RECORD-ADVANCES IN INTEGRATIVE ANATOMY AND EVOLUTIONARY BIOLOGY LA English DT Article DE elastic properties; structural stiffness; static loading; suture fusion; bone biomechanics ID RHESUS-MONKEY SKULLS; ELASTIC PROPERTIES; HUMAN-EVOLUTION; BONE STRAIN; CRANIOFACIAL SKELETON; MECHANICAL-PROPERTIES; COMPUTER-SIMULATION; SAGITTAL SUTURE; FACIAL SUTURES; ZYGOMATIC ARCH AB The biomechanical significance of cranial sutures in primates is an open question because their global impact is unclear, and their material properties are difficult to measure. In this study, eight suture-bone functional units representing eight facial sutures were created in a finite element model of a monkey cranium. All the sutures were assumed to have identical isotropic linear elastic material behavior that varied in different modeling experiments, representing either fused or unfused sutures. The values of elastic moduli employed in these trials ranged over several orders of magnitude. Each model was evaluated under incisor, premolar, and molar biting conditions. Results demonstrate that skulls with unfused sutures permitted more deformations and experienced higher total strain energy. However, strain patterns remained relatively unaffected away from the suture sites, and bite reaction force was likewise barely affected. These findings suggest that suture elasticity does not substantially alter load paths through the macaque skull or its underlying rigid body kinematics. An implication is that, for the purposes of finite element analysis, omitting or fusing sutures is a reasonable modeling approximation for skulls with small suture volume fraction if the research objective is to observe general patterns of craniofacial biomechanics under static loading conditions. The manner in which suture morphology and ossification affect the mechanical integrity of skulls and their ontogeny and evolution awaits further investigation,and their viscoelastic properties call for dynamic simulations. Anat Rec, 293:1477-1491, 2010. (C) 2010 Wiley-Liss, Inc. C1 [Wang, Qian; Zapata, Uriel] Mercer Univ, Sch Med, Div Basic Med Sci, Macon, GA 31207 USA. [Smith, Amanda L.; Strait, David S.] SUNY Albany, Dept Anthropol, Albany, NY 12222 USA. [Wright, Barth W.] Kansas City Univ Med & Biosci, Dept Anat, Kansas City, MO USA. [Richmond, Brian G.] George Washington Univ, Dept Anthropol, Ctr Adv Study Hominid Paleobiol, Washington, DC USA. [Richmond, Brian G.] Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20560 USA. [Grosse, Ian R.] Univ Massachusetts, Dept Mech & Ind Engn, Amherst, MA 01003 USA. [Byron, Craig D.] Mercer Univ, Dept Biol, Macon, GA 31207 USA. [Zapata, Uriel] EAFIT Univ, Dept Mech Engn, Medellin, Colombia. RP Wang, QA (reprint author), Mercer Univ, Sch Med, Div Basic Med Sci, 1550 Coll St, Macon, GA 31207 USA. EM wang_q2@mercer.edu RI Zapata M, Uriel/G-5411-2011 OI Zapata M, Uriel/0000-0002-9309-7571 FU National Science Foundation HOMINID [0725183, 0725126, 0725136, 0725078, 0725122] FX Grant sponsor: National Science Foundation HOMINID; Grant numbers: 0725183, 0725126, 0725136, 0725078, 0725122. NR 83 TC 32 Z9 34 U1 4 U2 10 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 1932-8486 J9 ANAT REC JI Anat. Rec. PD SEP PY 2010 VL 293 IS 9 BP 1477 EP 1491 DI 10.1002/ar.21203 PG 15 WC Anatomy & Morphology SC Anatomy & Morphology GA 645XC UT WOS:000281498500003 PM 20652940 ER PT J AU Crofoot, MC Lambert, TD Kays, R Wikelski, MC AF Crofoot, Margaret C. Lambert, Thomas D. Kays, Roland Wikelski, Martin C. TI Does watching a monkey change its behaviour? Quantifying observer effects in habituated wild primates using automated radiotelemetry SO ANIMAL BEHAVIOUR LA English DT Article DE Barro Colorado Island, Panama; Cebus capucinus; habituation; telemetry ID CAPUCHINS CEBUS-CAPUCINUS; FEMALE SOCIAL RELATIONSHIPS; LONG-TERM; FOREST; CHIMPANZEES; PREDATION; RESPONSES; PENGUINS; LOCATION; SURVIVAL AB In studies of animal behaviour, researchers have long been concerned that their presence may change the conduct of their study subjects. To minimize observer effects, researchers often habituate their study animals. The premise of this method is that, with sufficient neutral exposure, animals will stop reacting to humans. While numerous studies demonstrate that negative responses to humans decrease over time, the fact that an animal does not flee from or behave aggressively towards observers cannot be taken as evidence that it is not altering its behaviour in other, more subtle ways. Because remotely monitoring the behaviour of wild animals is difficult, it has not been possible to answer the critical question: do habituated animals change their behaviour when researchers are present? Here, we use data from an automated radiotelemetry system that remotely monitored the movement and activity of radiocollared animals to test whether observers affected the behaviour of seven habituated white-faced capuchins, Cebus capucinus. We found no evidence that observers influenced the ranging behaviour or activity patterns of their study subjects. Capuchins did not move faster, stop to rest less frequently, or display higher levels of activity when they were being followed compared to when they were alone. It has been suggested that researchers may embolden habituated study subjects, artificially increasing their relative dominance, but we found no relationship between observer presence and proximity to neighbouring social groups. Although it remains possible that observer effects existed but were too subtle to be detected with the remote sensing technology we used, the results of this study nevertheless provide reassuring evidence that humans can observe habituated wild animals without overly influencing the animals' activity and movement patterns. (C) 2010 The Association for the Study of Animal Behaviour. Published by Elsevier Ltd. All rights reserved. C1 [Crofoot, Margaret C.; Wikelski, Martin C.] Max Planck Inst Ornithol, Div Migrat & Immunoecol, Radolfzell am Bodensee, Germany. [Crofoot, Margaret C.; Kays, Roland; Wikelski, Martin C.] Smithsonian Trop Res Inst, Ancon, Panama. [Crofoot, Margaret C.] Princeton Univ, Dept Ecol & Evolutionary Biol, Princeton, NJ USA. [Lambert, Thomas D.] Frostburg State Univ, Dept Biol, Frostburg, MD 21532 USA. [Kays, Roland] New York State Museum & Sci Serv, Albany, NY USA. RP Crofoot, MC (reprint author), Smithsonian Trop Res Inst, Unit 9100, Box 0948, Dpo, AA 34002 USA. EM crofootm@si.edu FU Frederik Sheldon Travel Grant; American Society of Primatologists; Smithsonian Tropical Research Institute; Sigma Xi; Department of Biology at Armstrong Atlantic State University; Program in Biological Anthropology, Harvard University FX We thank the Autoridad Nacional del Ambiente (ANAM) and the government of Panama for permission to conduct research in Panama, and the Smithsonian Tropical Research Institute, and especially Oris Acevedo for logistical support. Technical support was provided by the Automated Radio Telemetry System Initiative, particularly Daniel Obando, Pablo Flores, Alejandro Ortega and Kevin Sallee. We also thank Vilma Fernandez for her help collecting data, Michelle Brown, Robyn Hoing, Jennifer Boothby, Robert Horan, Vilma Fernandez and George Middleton for help with darting, Nicanor Obaldia, DVM, Claudia Brandariz, DVM and Terry Norton, DVM for veterinary support and Ben Hirsch, Scott Mangan, Ian Gilby, Susy Cote, Michelle Brown and two anonymous referees for their comments on this paper. Financial support for this work was provided by the Frederik Sheldon Travel Grant, the American Society of Primatologists, the Smithsonian Tropical Research Institute, Sigma Xi, the Department of Biology at Armstrong Atlantic State University, and the Program in Biological Anthropology, Harvard University. Required permits for the work described in this paper were obtained from the Autoridad Nacional del Ambiente, Panama, and the Smithsonian Tropical Research Institute. All research complied with the laws of the Republic of Panama and the United States of America. NR 46 TC 17 Z9 18 U1 2 U2 41 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0003-3472 J9 ANIM BEHAV JI Anim. Behav. PD SEP PY 2010 VL 80 IS 3 BP 475 EP 480 DI 10.1016/j.anbehav.2010.06.006 PG 6 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA 637VM UT WOS:000280846800017 ER PT J AU Winkler, U Zotz, G AF Winkler, Uwe Zotz, Gerhard TI 'And then there were three': highly efficient uptake of potassium by foliar trichomes of epiphytic bromeliads SO ANNALS OF BOTANY LA English DT Article DE Epiphytic bromeliads; potassium uptake; luxury consumption; plant nutrition; Vriesea splenriet ID MONTANE FOREST; SPANISH MOSS; PHOSPHORUS; NITROGEN; PLANTS; TRANSPORT; NUTRITION; ROOTS AB Background and ilium Vascular epiphytes have to acquire nutrients from atmospheric wash out, stem-flow, canopy soils and trapped litter. Physiological studies on the adaptations to nutrient acquisition and plant utilization of nutrients have focused on phosphorus and nitrogen; potassium, as a third highly abundant nutrient element, has received minor attention. In the present study, potassium uptake kinetics by leaves, within-plant distribution and nutrient accumulation were analysed to gain an improved understanding of physiological adaptations to non-terrestrial nutrient supply of plants. Methods Radioactively labelled (86)RbCl was used as an analogue to study uptake kinetics of potassium absorbed from tanks of epiphytes, its plant distribution and the correlation between uptake efficiency and abundance of trichomes, functioning as uptake organs of leaves. Potassium in leaves was additionally analysed by atomic absorption spectroscopy to assess plant responses to potassium deficiency. Key Results Labelled rubidium was taken up from tanks over a wide range of concentrations, 0-01-90 mM, which was achieved by two uptake systems. In four tank epiphytes, the high-affinity transporters had average K(m) values of 41-2 mu m, and the low-affinity transporters average K(m) values of 44-8 mM. Further analysis in Vriesea splenriet showed that high-affinity uptake of rubidium was an ATP-dependent process, while low-affinity uptake was mediated by a K(+)-channel. The kinetic properties of both types of transporters are comparable with those of potassium transporters in roots of terrestrial plants. Specific differences in uptake velocities of epiphytes are correlated with the abundance of trichomes on their leaf surfaces. The main sinks for potassium were fully grown leaves. These leaves thus function as internal potassium sources, which allow growth to be maintained during periods of low external potassium availability. Conclusions Vascular epiphytes possess effective mechanisms to take up potassium from both highly diluted and highly concentrated solutions, enabling the plant to incorporate this nutrient element quickly and almost quantitatively from tank solutions. A surplus not needed for current metabolism is stored, i.e. plants show luxury consumption. C1 [Winkler, Uwe; Zotz, Gerhard] Carl von Ossietzky Univ Oldenburg, Funct Ecol Grp, D-26111 Oldenburg, Germany. [Zotz, Gerhard] Smithsonian Trop Res Inst, Balboa, Panama. RP Winkler, U (reprint author), Carl von Ossietzky Univ Oldenburg, Funct Ecol Grp, D-26111 Oldenburg, Germany. EM u.winkler@uni-oldenburg.de NR 35 TC 8 Z9 8 U1 2 U2 32 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0305-7364 J9 ANN BOT-LONDON JI Ann. Bot. PD SEP PY 2010 VL 106 IS 3 BP 421 EP 427 DI 10.1093/aob/mcq120 PG 7 WC Plant Sciences SC Plant Sciences GA 648ZJ UT WOS:000281733900005 PM 20542886 ER PT J AU Uchoa, MA Nicacio, J AF Uchoa, Manoel A. Nicacio, Jose TI New Records of Neotropical Fruit Flies (Tephritidae), Lance Flies (Lonchaeidae) (Diptera: Tephritoidea), and Their Host Plants in the South Pantanal and Adjacent Areas, Brazil SO ANNALS OF THE ENTOMOLOGICAL SOCIETY OF AMERICA LA English DT Article DE Anastrepha spp; Ceratitis cantata; host fruit; Neosilba spp.; taxonomy ID NEOSILBA DIPTERA; STATE; REVISION; MCALPINE AB Fruit flies (Tephritidae) and lance flies (Lonchaeidae) (Diptera) include pests of highest economic importance to horticulture around the world, because various species damage high value fruit crops. These Tephritoidea are the reason for quarantine barriers among many countries, limiting the commerce of fresh fruits and vegetables Knowledge of frugivorous tephritoid species richness and their interactions with the host plants are extremely important to Integrated Pest Management This paper presents the interactions of 15 species of Anastrepha Schiner, Ceratitis capitata (Wiedemann) (Tephritidae), and eight species of Neosilba McAlpine (Lonchaeidae) with 40 host fruit species We discovered that Pouteria glomerata (Miguel) Radlkofer (Sapotaceae) is the host fruit of Anastrepha undosa Stone. A. zernyi Ulna was associated with fruit of Anacardium othonianum Rizzini (Anacardiaceae) This is the first record of A. zernyi from the State of Mato Grosso do Sul, and of A hastata Stone from Central Brazil A sorocula Zucchi and A. zenildae Zucchi were the tephritids that infested the highest number of host fruits A alveatoides Blanchard, A. distincta Greene, A macrura Hendel, A. rheediae Stone and A. undosa Stone were recovered from only one species of host, and all of these associations are new records. Also established for the first time are the associations among eight species of Neosilba with 38 host species. N. zadolicha McAlpine and Steyskal, N. pendula (Bezzi), N glaberrima (Wiedemann) and N. mesperata Strikis and Prado were the most polyphagous Lonchaeidae C1 [Uchoa, Manoel A.; Nicacio, Jose] UFGD, Lab Insetos Frugivoros, FCBA, BR-79804970 Dourados, MS, Brazil. [Uchoa, Manoel A.] Natl Museum Nat Hist, Dept Entomol, Smithsonian Inst, Washington, DC 20013 USA. RP Uchoa, MA (reprint author), UFGD, Lab Insetos Frugivoros, FCBA, Caixa Postal 241, BR-79804970 Dourados, MS, Brazil. FU Fundacao de Apoio ao Desenvolvimento do Ensino. Ciencia e Tecnologia do Estado de Mato Grosso do Sul (FUNDECT, MS, Brazil); Conselho Nacional de Desenvolvimento Cientifico c Tecnologico (CNPq); Coodenacao de Aperfeicoamento de Pessoal de Nivel Superior (CAPES) FX We thank the botanists Ubirazailda Maria Rezende from the Herbarium of the Universidade Federal de Mato Grosso do Sul (UFMS), Campo Grande-MS and Jose Rubens Pirani from the Herbarium of the Universidade de Sao Paulo (USP) Sao Paulo, Brazil, for the identification of the plant species, Pedro Carlos Strikis (UNICAMP, Campinas-SP, Brazil) for identification and mounting the Lonchaeodae, Fundacao de Apoio ao Desenvolvimento do Ensino. Ciencia e Tecnologia do Estado de Mato Grosso do Sul (FUNDECT, MS, Brazil) for the financial support to the project 'Biodiversidade de insetos frugivoros, seus hospedeiros and e immigos naturais no Brasil Central" and Conselho Nacional de Desenvolvimento Cientifico c Tecnologico (CNPq) for the grant to J N N, Coodenacao de Aperfeicoamento de Pessoal de Nivel Superior (CAPES) for the Postdoctoral fellowship to M A U, and Allen L Norrboin (Systematic Entomology Laboratory, USDA-ARS) for his valuable suggestions on the manuscript, making it more comprehensive NR 46 TC 16 Z9 17 U1 0 U2 4 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 0013-8746 EI 1938-2901 J9 ANN ENTOMOL SOC AM JI Ann. Entomol. Soc. Am. PD SEP PY 2010 VL 103 IS 5 BP 723 EP 733 PG 11 WC Entomology SC Entomology GA 647XY UT WOS:000281655300005 ER PT J AU Grant, JA Westall, F Beaty, DW Vago, JL AF Grant, John A. Westall, Frances Beaty, David W. Vago, Jorge L. TI Two Rovers to the Same Site on Mars, 2018: Possibilities for Cooperative Science SO ASTROBIOLOGY LA English DT Article ID SAMPLE RETURN; MISSION; EXPLORATION; SURFACE; LIFE C1 [Grant, John A.] Smithsonian Inst, Ctr Earth & Planetary Studies, Natl Air & Space Museum, MRC 315, Washington, DC 20013 USA. [Westall, Frances] CNRS, Ctr Biophys Mol, F-45071 Orleans 2, France. [Beaty, David W.] CALTECH, Mars Program Off, Jet Prop Lab, Pasadena, CA 91109 USA. [Vago, Jorge L.] European Space Agcy, ESA ESTEC HME ME, NL-2201 AZ Noordwijk, Netherlands. RP Grant, JA (reprint author), Smithsonian Inst, Ctr Earth & Planetary Studies, Natl Air & Space Museum, MRC 315, POB 37012, Washington, DC 20013 USA. EM grantj@si.edu; frances.westall@cnrs-orleans.fr; David.Beaty@jpl.nasa.gov; Jorge.Vago@esa.int FU National Aeronautics and Space Administration FX An early draft of the list of possible options for collaborative science and their priorities (Table 2 of this report) was discussed with multiple colleagues within the Mars exploration community, including the leaders of MRR-SAG; ExoMars project leadership; the ExoMars Science Working Group; ExoMars instrument science colleagues; the JPL Mars Program Office science team; similar to 8-10 MER scientists; and professional colleagues of several team members. This resulted in the addition of several new ideas, valuable clarification of others, and refinement of our perception of their relative priorities. Chad Edwards (Chief Telecommunications Engineer, Mars Program Office, JPL) provided extensive input to the telecommunications analysis. Gerhard Kminek (Planetary Protection Officer, ESA) provided input to the section on planetary protection. An early draft of this report was presented orally on March 17, 2010, at the MEPAG meeting in Monrovia, and the ensuing discussion was very helpful in refining the ideas contained in this report. A portion of this work was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 40 TC 4 Z9 4 U1 0 U2 7 PU MARY ANN LIEBERT, INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 EI 1557-8070 J9 ASTROBIOLOGY JI Astrobiology PD SEP PY 2010 VL 10 IS 7 BP 663 EP 685 DI 10.1089/ast.2010.0526 PG 23 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 671EM UT WOS:000283483100001 ER PT J AU Laine, S Appleton, PN Gottesman, ST Ashby, MLN Garland, CA AF Laine, Seppo Appleton, Philip N. Gottesman, Stephen T. Ashby, Matthew L. N. Garland, Catherine A. TI WARM MOLECULAR HYDROGEN EMISSION IN NORMAL EDGE-ON GALAXIES NGC 4565 AND NGC 5907 SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: individual (NGC 4565, NGC 5907); galaxies: ISM; galaxies: structure ID SPITZER-SPACE-TELESCOPE; INFRARED SPECTROGRAPH IRS; SPIRAL GALAXIES; ROTATION CURVES; STEPHANS QUINTET; NEUTRAL HYDROGEN; CO OBSERVATIONS; DARK-MATTER; SWS SURVEY; DUST AB We have observed warm molecular hydrogen in two nearby edge-on disk galaxies, NGC 4565 and NGC 5907, using the Spitzer high-resolution infrared spectrograph. The 0-0 S(0) 28.2 mu m and 0-0 S(1) 17.0 mu m pure rotational lines were detected out to 10 kpc from the center of each galaxy on both sides of the major axis, and in NGC 4565 the S(0) line was detected at r = 15 kpc on one side. This location is beyond the transition zone where diffuse neutral atomic hydrogen starts to dominate over cold molecular gas and marks a transition from a disk dominated by high surface-brightness far-infrared (far-IR) emission to that of a more quiescent disk. It also lies beyond a steep drop in the radio continuum emission from cosmic rays (CRs) in the disk. Despite indications that star formation activity decreases with radius, the H(2) excitation temperature and the ratio of the H(2) line and the far-IR luminosity surface densities, Sigma(L(H2))/Sigma(L(TIR)), change very little as a function of radius, even into the diffuse outer region of the disk of NGC 4565. This suggests that the source of excitation of the H(2) operates over a large range of radii and is broadly independent of the strength and relative location of UV emission from young stars. Although excitation in photodissociation regions is the most common explanation for the widespread H(2) emission, CR heating or shocks cannot be ruled out. At r = 15 kpc in NGC 4565, outside the main UV-and radio-continuum-dominated disk, we derived a higher than normal H(2) to 7.7 mu m polycyclic aromatic hydrocarbon (PAH) emission ratio, but this is likely due to a transition from mainly ionized PAH molecules in the inner disk to mainly neutral PAH molecules in the outer disk. The inferred mass surface densities of warm molecular hydrogen in both edge-on galaxies differ substantially, being 4(-60) M(circle dot)pc(-2) and 3(-50) M(circle dot)pc(-2) at r = 10 kpc for NGC 4565 and NGC 5907, respectively. The higher values represent very unlikely point-source upper limits. The point-source case is not supported by the observed emission distribution in the spectral slits. These mass surface densities cannot support the observed rotation velocities in excess of 200 km s(-1). Therefore, warm molecular hydrogen cannot account for dark matter in these disk galaxies, contrary to what was implied by a previous Infrared Space Observatory study of the nearby edge-on galaxy NGC 891. C1 [Laine, Seppo] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Appleton, Philip N.] CALTECH, NASA Herschel Sci Ctr, Pasadena, CA 91125 USA. [Gottesman, Stephen T.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Ashby, Matthew L. N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Garland, Catherine A.] Castleton State Coll, Dept Nat Sci, Castleton, VT 05735 USA. RP Laine, S (reprint author), CALTECH, Spitzer Sci Ctr, MS 220-6, Pasadena, CA 91125 USA. EM seppo@ipac.caltech.edu; apple@ipac.caltech.edu; gott@astro.ufl.edu; mashby@cfa.harvard.edu; catherine.garland@castleton.edu OI Appleton, Philip/0000-0002-7607-8766 FU NASA FX We are grateful to Tom Jarrett at IPAC for helping us to correct the rogue pixels with his custom-made IRAF script. We thank the anonymous referee for very helpful and detailed comments. We acknowledge stimulating discussions with Eric Murphy on the mid-IR and far-IR properties of nearby galaxies. 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. SMART was developed by the IRS Team at Cornell University and is available through the Spitzer Science Center at Caltech. The IRS was a collaborative venture between Cornell University and Ball Aerospace Corporation funded by NASA through the Jet Propulsion Laboratory and Ames Research Center. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. NR 48 TC 8 Z9 8 U1 1 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD SEP PY 2010 VL 140 IS 3 BP 753 EP 769 DI 10.1088/0004-6256/140/3/753 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 638GT UT WOS:000280882300009 ER PT J AU Trilling, DE Mueller, M Hora, JL Harris, AW Bhattacharya, B Bottke, WF Chesley, S Delbo, M Emery, JP Fazio, G Mainzer, A Penprase, B Smith, HA Spahr, TB Stansberry, JA Thomas, CA AF Trilling, D. E. Mueller, M. Hora, J. L. Harris, A. W. Bhattacharya, B. Bottke, W. F. Chesley, S. Delbo, M. Emery, J. P. Fazio, G. Mainzer, A. Penprase, B. Smith, H. A. Spahr, T. B. Stansberry, J. A. Thomas, C. A. TI EXPLORENEOs. I. DESCRIPTION AND FIRST RESULTS FROM THE WARM SPITZER NEAR-EARTH OBJECT SURVEY SO ASTRONOMICAL JOURNAL LA English DT Article DE minor planets, asteroids: general; infrared: planetary systems; surveys ID THERMAL INFRARED SPECTROPHOTOMETRY; KUIPER-BELT OBJECTS; SPACE-TELESCOPE; ASTEROID BELT; ARRAY CAMERA; RA-SHALOM; ORIGIN; POPULATION; MAGNITUDES; YARKOVSKY AB We have begun the ExploreNEOs project in which we observe some 700 Near-Earth Objects (NEOs) at 3.6 and 4.5 mu m with the Spitzer Space Telescope in its Warm Spitzer mode. From these measurements and catalog optical photometry we derive albedos and diameters of the observed targets. The overall goal of our ExploreNEOs program is to study the history of near-Earth space by deriving the physical properties of a large number of NEOs. In this paper, we describe both the scientific and technical construction of our ExploreNEOs program. We present our observational, photometric, and thermal modeling techniques. We present results from the first 101 targets observed in this program. We find that the distribution of albedos in this first sample is quite broad, probably indicating a wide range of compositions within the NEO population. Many objects smaller than 1 km have high albedos (greater than or similar to 0.35), but few objects larger than 1 km have high albedos. This result is consistent with the idea that these larger objects are collisionally older, and therefore possess surfaces that are more space weathered and therefore darker, or are not subject to other surface rejuvenating events as frequently as smaller NEOs. C1 [Trilling, D. E.; Thomas, C. A.] No Arizona Univ, Dept Phys & Astron, Flagstaff, AZ 86001 USA. [Mueller, M.; Delbo, M.] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, F-06304 Nice 4, France. [Hora, J. L.; Fazio, G.; Smith, H. A.; Spahr, T. B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Harris, A. W.] DLR Inst Planetary Res, D-12489 Berlin, Germany. [Bhattacharya, B.] CALTECH, NASA Herschel Sci Ctr, Pasadena, CA 91125 USA. [Bottke, W. F.] SW Res Inst, Boulder, CO 80302 USA. [Chesley, S.; Mainzer, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Emery, J. P.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. [Penprase, B.] Pomona Coll, Dept Phys & Astron, Claremont, CA 91711 USA. [Stansberry, J. A.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Trilling, DE (reprint author), No Arizona Univ, Dept Phys & Astron, Flagstaff, AZ 86001 USA. EM david.trilling@nau.edu OI Mueller, Michael/0000-0003-3217-5385; Hora, Joseph/0000-0002-5599-4650; Thomas, Cristina/0000-0003-3091-5757 FU NASA FX We acknowledge the thorough and prompt hard work of the staff at the Spitzer Science Center, without whom the execution of this program would not be possible. We thank Michael Mommert (DLR) for help in checking the modeling results given in the data tables. We thank an anonymous referee for making a number of useful suggestions. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by JPL/Caltech under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. NR 68 TC 29 Z9 29 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD SEP PY 2010 VL 140 IS 3 BP 770 EP 784 DI 10.1088/0004-6256/140/3/770 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 638GT UT WOS:000280882300010 ER PT J AU Song, LM Tripp, TM Wang, QD Yao, YS Cui, W Xue, YQ Orosz, JA Steeghs, D Steiner, JF Torres, MAP McClintock, JE AF Song, Limin Tripp, Todd M. Wang, Q. Daniel Yao, Yangsen Cui, Wei Xue, Yongquan Orosz, Jerome A. Steeghs, Danny Steiner, James F. Torres, Manuel A. P. McClintock, Jeffrey E. TI VARIABLE O vi AND N v EMISSION FROM THE X-RAY BINARY LMC X-3: HEATING OF THE BLACK HOLE COMPANION SO ASTRONOMICAL JOURNAL LA English DT Article DE stars: individual (LMCX-3) ID ULTRAVIOLET-SPECTROSCOPIC-EXPLORER; INTERSTELLAR-MEDIUM; ACCRETION DISK; STELLAR WINDS; SPECTROGRAPH; LMC-X-3; STARS; MODEL; HALO; OVI AB Based on high-resolution ultraviolet spectroscopy obtained with the Far Ultraviolet Spectroscopic Explorer (FUSE) and the Cosmic Origins Spectrograph, we present new detections of Ovi and Nv emission from the black hole X-ray binary (XRB) system LMCX-3. We also update the ephemeris of the XRB using recent radial velocity measurements obtained with the echelle spectrograph on the Magellan-Clay telescope. We observe significant velocity variability of the UV emission, and we find that the Ovi and Nv emission velocities follow the optical velocity curve of the XRB. Moreover, the Ovi and Nv intensities regularly decrease between binary phase=0.5 and 1.0, which suggests that the source of the UV emission is increasingly occulted as the B star in the XRB moves from superior to inferior conjunction. These trends suggest that illumination of the B star atmosphere by the intense X-ray emission from the accreting black hole creates a hot spot on one side of the B star, and this hot spot is the origin of the Ovi and Nv emission. However, the velocity semiamplitude of the ultraviolet emission, K(UV) approximate to 180 km s(-1), is lower than the optical semiamplitude; this difference could be due to rotation of the B star. Comparison of the FUSE observations taken in 2001 November and 2004 April shows a significant change in the Ovi emission characteristics: in the 2001 data, the Ovi region shows both broad and narrow emission features, while in 2004 only the narrow Ovi emission is clearly present. Rossi X-ray Timing Explorer data show that the XRB was in a high/soft state in the 2001 November epoch but was in a transitional state in 2004 April, so the shape of the X-ray spectrum might change the properties of the region illuminated on the B star and thus change the broad versus narrow characteristics of the UV emission. If our hypothesis about the origin of the highly ionized emission is correct, then careful analysis of the emission occultation could, in principle, constrain the inclination of the XRB and the mass of the black hole. Key words: stars: individual (LMCX-3) C1 [Song, Limin; Tripp, Todd M.; Wang, Q. Daniel] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Yao, Yangsen] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Cui, Wei; Xue, Yongquan] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Xue, Yongquan] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Orosz, Jerome A.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. [Steeghs, Danny] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Steiner, James F.; Torres, Manuel A. P.; McClintock, Jeffrey E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Song, LM (reprint author), Univ Massachusetts, Dept Astron, Lederle Grad Res Tower B 619E,710 N Pleasant St, Amherst, MA 01003 USA. RI Steeghs, Danny/C-5468-2009; OI Steeghs, Danny/0000-0003-0771-4746; Cui, Wei/0000-0002-6324-5772 FU NASA [NNG04GJB83G, HST-GO-11642.01-A, HST-GO-11642.02-A] FX We thank John Raymond, Saku Vrtilek, and Jifeng Liu for their very helpful comments on an early version of the paper. We thank the referee for thoughtful suggestions. The data presented in this paper were obtained for the FUSE GO program E063 and the HST GO program 11642. These programs were funded by NASA through grants NNG04GJB83G, HST-GO-11642.01-A, and HST-GO-11642.02-A, respectively. NR 26 TC 5 Z9 5 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD SEP PY 2010 VL 140 IS 3 BP 794 EP 803 DI 10.1088/0004-6256/140/3/794 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 638GT UT WOS:000280882300012 ER PT J AU Hughes, AM Andrews, SM Wilner, DJ Meyer, MR Carpenter, JM Qi, C Hales, AS Casassus, S Hogerheijde, MR Mamajek, EE Wolf, S Henning, T Silverstone, MD AF Hughes, A. M. Andrews, S. M. Wilner, D. J. Meyer, M. R. Carpenter, J. M. Qi, C. Hales, A. S. Casassus, S. Hogerheijde, M. R. Mamajek, E. E. Wolf, S. Henning, T. Silverstone, M. D. TI STRUCTURE AND COMPOSITION OF TWO TRANSITIONAL CIRCUMSTELLAR DISKS IN CORONA AUSTRALIS SO ASTRONOMICAL JOURNAL LA English DT Article DE circumstellar matter; protoplanetary disks; stars: individual (RX J1842.9-3532, RX J1852.3-3700); stars: pre-main sequence ID T-TAURI STARS; 2-DIMENSIONAL RADIATIVE-TRANSFER; MAIN-SEQUENCE STARS; SUN-LIKE STARS; PROTOPLANETARY DISKS; PLANETARY SYSTEMS; YOUNG STARS; X-RAY; SUBMILLIMETER ARRAY; ACCRETION RATES AB The late stages of evolution of the primordial circumstellar disks surrounding young stars are poorly understood, yet vital to constraining theories of planet formation. We consider basic structural models for the disks around two similar to 10 Myr old members of the nearby RCrA association: RX J1842.9-3532 and RX J1852.3-3700. We present new arc second-resolution maps of their 230 GHz continuum emission from the Submillimeter Array and unresolved CO(3-2) spectra from the Atacama Submillimeter Telescope Experiment. By combining these data with broadband fluxes from the literature and infrared fluxes and spectra from the catalog of the Formation and Evolution of Planetary Systems Legacy program on the Spitzer Space Telescope, we assemble a multiwavelength data set probing the gas and dust disks. Using the Monte Carlo radiative transfer code RADMC to model simultaneously the spectral energy distribution and millimeter continuum visibilities, we derive basic dust disk properties and identify an inner cavity of radius 16 AU in the disk around RX J1852.3-3700. We also identify an optically thin 5 AU cavity in the disk around RX J1842.9-3532, with a small amount of optically thick material close to the star. The molecular line observations suggest an intermediate disk inclination in RX J1842.9-3532, consistent with the continuum emission. In combination with the dust models, the molecular data allow us to derive a lower CO content than expected, suggesting that the process of gas clearing is likely underway in both systems, perhaps simultaneously with planet formation. C1 [Hughes, A. M.; Andrews, S. M.; Wilner, D. J.; Qi, C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Meyer, M. R.] ETH, Inst Astron, Dept Phys, CH-8093 Zurich, Switzerland. [Carpenter, J. M.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Hales, A. S.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Casassus, S.] Univ Chile, Dept Astron, Santiago, Chile. [Hogerheijde, M. R.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Mamajek, E. E.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. [Wolf, S.] Univ Kiel, Inst Theoret Phys & Astrophys, D-24098 Kiel, Germany. [Henning, T.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Silverstone, M. D.] Eureka Sci Inc, Cary, NC 27513 USA. RP Hughes, AM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mhughes@cfa.harvard.edu; sandrews@cfa.harvard.edu; dwilner@cfa.harvard.edu; mmeyer@phys.ethz.ch; jmc@astro.caltech.edu; cqi@cfa.harvard.edu; ahales@alma.cl; simon@das.uchile.cl; michiel@strw.leidenuniv.nl; emamajek@pas.rochester.edu; wolf@astrophysik.uni-kiel.de; henning@mpia-hd.mpg.de; mdsilverstone@att.net RI Casassus, Simon/I-8609-2016 FU NASA [NAG5-11777, NAS 5-26555, NNG06GH25G]; Space Telescope Science Institute FX We thank C. P. Dullemond for access to the two-dimensional version of RADMC. Partial support for this work was provided by NASA Origins of Solar Systems Program Grant NAG5-11777. A. M. H. acknowledges support from a National Science Foundation Graduate Research Fellowship. Support for S. M. A. was provided by NASA through Hubble Fellowship grant HF-01203-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. M. R. M. acknowledges the Harvard Origins of Life Initiative, the Smithsonian Astrophysical Observatory, and a NASA TPF Foundation Science Program grant NNG06GH25G (PI: S. Kenyon) for sabbatical support. NR 66 TC 18 Z9 18 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD SEP PY 2010 VL 140 IS 3 BP 887 EP 896 DI 10.1088/0004-6256/140/3/887 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 638GT UT WOS:000280882300019 ER PT J AU Castelli, F Kurucz, RL AF Castelli, F. Kurucz, R. L. TI New Fe II energy levels from stellar spectra SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE line: identification; atomic data; stars: atmospheres; stars: chemically peculiar; stars: individual: HR 6000 ID SUPERMULTIPLET; LINES AB Aims. The spectra of B-type and early A-type stars show numerous unidentified lines in the whole optical range, especially in the 5100-5400 angstrom interval. Because Fe II transitions to high energy levels should be observed in this region, we used semiempirical predicted wavelengths and gf-values of Fe II to identify unknown lines. Methods. Semiempirical line data for Fe II computed by Kurucz are used to synthesize the spectrum of the slow-rotating, Fe-overabundant CP star HR 6000. Results. We determined a total of 109 new 4f levels for Fe II with energies ranging from 122 324 cm(-1) to 128 110 cm(-1). They belong to the Fe II subconfigurations 3d(6)((3)P)4f (10 levels), 3d(6)((3)H)4f (36 levels), 3d(6)((3)F)4f (37 levels), and 3d(6)((3)G)4f (26 levels). We also found 14 even levels from 4d (3 levels), 5d (7 levels), and 6d (4 levels) configurations. The new levels have allowed us to identify more than 50% of the previously unidentified lines of HR 6000 in the wavelength region 3800-8000 angstrom. Tables listing the new energy levels are given in the paper; tables listing the spectral lines with log gf >= -1.5 that are transitions to the 4f energy levels are given in the Online Material. These new levels produce 18 000 lines throughout the spectrum from the ultraviolet to the infrared. C1 [Castelli, F.] Ist Nazl Astrofis, Osservatorio Astron Trieste, I-34131 Trieste, Italy. [Kurucz, R. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Castelli, F (reprint author), Ist Nazl Astrofis, Osservatorio Astron Trieste, Via Tiepolo 11, I-34131 Trieste, Italy. EM castelli@oats.inaf.it NR 13 TC 16 Z9 16 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD SEP-OCT PY 2010 VL 520 AR A57 DI 10.1051/0004-6361/201015126 PG 30 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 665VQ UT WOS:000283064200117 ER PT J AU Israel, H Erben, T Reiprich, TH Vikhlinin, A Hildebrandt, H Hudson, DS McLeod, BA Sarazin, CL Schneider, P Zhang, YY AF Israel, H. Erben, T. Reiprich, T. H. Vikhlinin, A. Hildebrandt, H. Hudson, D. S. McLeod, B. A. Sarazin, C. L. Schneider, P. Zhang, Y. -Y. TI The 400d Galaxy Cluster Survey weak lensing programme I. MMT/Megacam analysis of CL0030+2618 at z=0.50 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: clusters: general; galaxies: clusters: individuals: CL0030+2618; cosmology: observations gravitational lensing: weak; X-rays: galaxies: clusters ID BONN DEEP SURVEY; COSMIC SHEAR ANALYSIS; LYMAN-BREAK GALAXIES; DARK-MATTER HALOES; DIGITAL SKY SURVEY; X-RAY SOURCES; MASS FUNCTION; PHOTOMETRIC REDSHIFTS; OBSERVED GROWTH; PUBLIC-SURVEY AB Context. Studying cosmological structure formation provides insights into all of the universe's components: baryonic matter, dark matter, and, notably, dark energy. Measuring the mass function of galaxy clusters at high redshifts is particularly useful probe for both learning about the history of structure formation and constraining cosmological parameters. Aims. We attempt to derive reliable masses for a high-redshift, high-luminosity sample of galaxy clusters selected from the 400d X-ray selected cluster survey. Weak gravitational lensing allows us to determine masses that can be compared with those inferred from X-rays, forming an independent test. We focus on a particular object, CL0030+2618 at z = 0.50. Methods. Using deep imaging in three passbands acquired using the Megacam instrument at MMT, we show that Megacam is well-suited to measuring gravitational shear, i.e., the shapes of faint galaxies. A catalogue of background galaxies is constructed by analysing the photometric properties of galaxies in the g'r'i' bands. Results. Using the aperture mass technique, we detect the weak lensing signal of CL0030+2618 at 5.8 sigma significance. We find significant tangential alignment of galaxies out to similar to 10' or a distance of >2 r(200) from the cluster centre. The weak lensing centre of CL0030+2618 agrees with several X-ray measurements and the position of the brightest cluster galaxy. Finally, we infer a weak lensing virial mass of M(200) = 7.2(-2.9-2.5)(+ 3.6+2.3) x 10(14) M(circle dot) for CL0030+2618. Conclusions. Despite complications caused by a tentative foreground galaxy group along the line of sight, the X-ray and weak lensing estimates for CL0030+2618 are in remarkable agreement. C1 [Israel, H.; Erben, T.; Reiprich, T. H.; Hudson, D. S.; Schneider, P.; Zhang, Y. -Y.] Argelander Inst Astron, D-53121 Bonn, Germany. [Vikhlinin, A.; McLeod, B. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hildebrandt, H.] Leiden Univ, Leiden Observ, NL-2333 CA Leiden, Netherlands. [Sarazin, C. L.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. RP Israel, H (reprint author), Argelander Inst Astron, Hugel 71, D-53121 Bonn, Germany. EM hisrael@astro.uni-bonn.de FU Silicon Valley Community Foundation; Smithsonian Astrophysical Observatory; NOAO; NSF FX Observations reported here were obtained at the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona. Our MMT observations were supported in part by a donation from the F. H. Levinson Fund of the Silicon Valley Community Foundation to the University of Virginia. In addition, MMT observations used for this project were granted by the Smithsonian Astrophysical Observatory and by NOAO, through the Telescope System Instrumentation Program (TSIP). TSIP is funded by NSF. NR 92 TC 20 Z9 20 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD SEP-OCT PY 2010 VL 520 AR A58 DI 10.1051/0004-6361/200913667 PG 29 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 665VQ UT WOS:000283064200033 ER PT J AU Kalkofen, W Rossi, P Bodo, G Massaglia, S AF Kalkofen, W. Rossi, P. Bodo, G. Massaglia, S. TI Acoustic waves in a stratified atmosphere IV. Three-dimensional nonlinear hydrodynamics SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE hydrodynamics; stars: late-type; waves; Sun: chromosphere ID SOLAR CHROMOSPHERE; PROPAGATION; INTERNETWORK; OSCILLATIONS; EXCITATION; DYNAMICS; GRAINS; ENERGY; SUMER AB Context. The quiet solar chromosphere in the interior of supergranulation cells is believed to be heated by the dissipation of acoustic waves that originate with a typical period of 3 min in the photosphere. Aims. We investigate how the horizontal expansion with height of acoustic waves traveling upward into an isothermal, gravitationally stratified atmosphere depends on the size of the source region. Methods. We have solved the three-dimensional, nonlinear, time-dependent hydrodynamic equations for impulsively-generated, upward-propagating acoustic waves, assuming cylindrical symmetry. Results. When the diameter of the source of acoustic waves is small, the pattern of the upward-propagating waves is that of a point source, for which the energy travels upward in a vertical cone, qualitatively matching the observed pattern of bright-point expansion with height. For the largest plausible size of a source region, i.e., with granular size of 1 Mm, wave propagation in the low chromosphere is approximately that of plane waves, but in the middle and upper chromosphere it is also that of a point source. The assumption of plane-wave propagation is not a good approximation in the solar chromosphere. The upward-directed energy flux is larger than that of the solar chromosphere, at least in the middle and upper chromosphere, and probably throughout. Conclusions. Simulations of impulsively generated acoustic waves emitted from source regions with diameters that are small compared to the pressure scale height of the atmosphere qualitatively reproduce the upward expansion observed in chromospheric bright points. The emission features in the cores of the H and K lines are predicted to be blueshifted for a pulse and redshifted for the waves in its wake. The contribution of internal gravity waves to the upward energy flux is small and decreases with increasing size of the source region. C1 [Kalkofen, W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kalkofen, W.] Kiepenheuer Inst Solar Phys, D-79104 Freiburg, Germany. [Rossi, P.; Bodo, G.] INAF Osservatorio Astron Torino, I-10025 Pino Torinese, Italy. [Massaglia, S.] Univ Torino, Dipartimento Fis Gen, I-10125 Turin, Italy. RP Kalkofen, W (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM wkalkofen@cfa.harvard.edu; rossi@oato.inaf.it; bodo@oato.inaf.it; massaglia@ph.unito.it RI Bodo, Gianluigi/F-9223-2012; ROSSI, PAOLA/I-7031-2015 OI Bodo, Gianluigi/0000-0002-9265-4081; massaglia, silvano/0000-0003-1779-7426; ROSSI, PAOLA/0000-0002-0840-4726 NR 32 TC 6 Z9 6 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD SEP-OCT PY 2010 VL 520 AR A100 DI 10.1051/0004-6361/200912996 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 665VQ UT WOS:000283064200100 ER PT J AU Robitaille, TP AF Robitaille, T. P. TI On the modified random walk algorithm for Monte-Carlo radiation transfer (Research Note) SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE radiative transfer; diffusion; circumstellar matter; methods: numerical AB Min et al. (2009) presented two complementary techniques that use the diffusion approximation to allow efficient Monte-Carlo radiation transfer in very optically thick regions: a modified random walk and a partial diffusion approximation. In this note, I show that the calculations required for the modified random walk method can be significantly simplified. In particular, the diffusion coefficient and the mass absorption coefficients required for the modified random walk are in fact the same as the standard diffusion coefficient and the Planck mean mass absorption coefficient. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Robitaille, TP (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM trobitaille@cfa.harvard.edu OI Robitaille, Thomas/0000-0002-8642-1329 FU NASA; Jet Propulsion Laboratory, California Institute of Technology FX I wish to thank the referee for a careful review, and for insightful comments that improved this research note. I also wish to thank Barbara Whitney, Kenny Wood, and Katharine Johnston for useful discussions. Support for this work was provided by NASA through the Spitzer Space Telescope Fellowship Program, through a contract issued by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. NR 3 TC 15 Z9 15 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 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD SEP-OCT PY 2010 VL 520 AR A70 DI 10.1051/0004-6361/201015025 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 665VQ UT WOS:000283064200128 ER PT J AU Strassmeier, KG Granzer, T Kopf, M Weber, M Kuker, M Reegen, P Rice, JB Matthews, JM Kuschnig, R Rowe, JF Guenther, DB Moffat, AFJ Rucinski, SM Sasselov, D Weiss, WW AF Strassmeier, K. G. Granzer, T. Kopf, M. Weber, M. Kueker, M. Reegen, P. Rice, J. B. Matthews, J. M. Kuschnig, R. Rowe, J. F. Guenther, D. B. Moffat, A. F. J. Rucinski, S. M. Sasselov, D. Weiss, W. W. TI Rotation and magnetic activity of the Hertzsprung-gap giant 31 Comae SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: activity; stars: atmospheres; stars: individual: 31 Comae; starspots; stars: late-type; stars: rotation ID PRE-MAIN-SEQUENCE; LATE-TYPE STARS; GENEVA-COPENHAGEN SURVEY; TIME-SERIES ANALYSIS; X-RAY ACTIVITY; LATE A-TYPE; G-K GIANTS; STELLAR EVOLUTION; COOL STARS; LUMINOSITY CLASSIFICATION AB Context. The single rapidly-rotating G0 giant 31 Comae has been a puzzle because of the absence of photometric variability despite its strong chromospheric and coronal emissions. As a Hertzsprung-gap giant, it is expected to be at the stage of rearranging its moment of inertia, hence likely also its dynamo action, which could possibly be linked with its missing photospheric activity. Aims. Our aim is to detect photospheric activity, obtain the rotation period, and use it for a first Doppler image of the star's surface. Its morphology could be related to the evolutionary status. Methods. We carried out high-precision, white-light photometry with the MOST satellite, ground-based Stromgren photometry with automated telescopes, and high-resolution optical echelle spectroscopy with the new STELLA robotic facility. Results. The MOST data reveal, for the first time, light variations with a full amplitude of 5 mmag and an average photometric period of 6.80 +/- 0.06 days. Radial-velocity variations with a full amplitude of 270 ms(-1) and a period of 6.76 +/- 0.02 days were detected from our STELLA spectra, which we also interpret as due to stellar rotation. The two-year constancy of the average radial velocity of +0.10 +/- 0.33 km s(-1) confirms the star's single status, as well as the membership in the cluster Melotte 111. A spectrum synthesis gives T-eff = 5660 +/- 42 K, log g = 3.51 +/- 0.09, and [Fe/H] = -0.15 +/- 0.03, which together with the revised Hipparcos distance, suggests a mass of 2.6 +/- 0.1 M-circle dot and an age of approximate to 540 Myr. The surface lithium abundance is measured to be nearly primordial. A detection of a strong He I absorption line indicates nonradiative heating processes in the atmosphere. Our Doppler images show a large, asymmetric polar spot, cooler than Teff by approximate to 1600 K, and several small low-to-mid latitude features that are warmer by approximate to 300-400 K and are possibly of chromospheric origin. We computed the convective turnover time for 31 Com as a function of depth and found on average tau(C) approximate to 5 days. Conclusions. 31 Com appears to be just at the onset of rapid magnetic braking and Li dilution because its age almost exactly coincides with the predicted onset of envelope convection. That we recover a big polar starspot despite the Rossby number being larger than unity, and thus no efficient (envelope) dynamo is expected, leads us to conclude that 31 Com still harbors a fossil predominantly poloidal magnetic field. However, the increasing convective envelope may have just started an interface dynamo that now is the source of the warm surface features and the corresponding UV and X-ray emission. C1 [Strassmeier, K. G.; Granzer, T.; Kopf, M.; Weber, M.; Kueker, M.] AIP, D-14482 Potsdam, Germany. [Reegen, P.; Kuschnig, R.; Weiss, W. W.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. [Rice, J. B.] Brandon Univ, Dept Phys, Brandon, MB R7A 6A9, Canada. [Matthews, J. M.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Rowe, J. F.] NASA Ames Res Ctr, Moffett Field, CA 94035 USA. [Guenther, D. B.] St Marys Univ, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada. [Moffat, A. F. J.] Univ Montreal CP 6128, Dept Phys, Montreal, PQ H3C 3J7, Canada. [Rucinski, S. M.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON OM5S 3H4, Canada. [Sasselov, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Strassmeier, KG (reprint author), AIP, Sternwarte 16, D-14482 Potsdam, Germany. EM kstrassmeier@aip.de; reegen@astro.univie.ac.at; rice@BrandonU.ca FU Natural Sciences and Engineering Research Council (NSERC) Canada; Canadian Space Agency; Austrian Science Promotion Agency (FFG-MOST); Austrian Science Funds [FWF-P17580]; FWF; KGS FX K.G.S. and the AIP coauthors are grateful to the State of Brandenburg and the German federal ministry for education and research (BMBF) for their continuous support of the STELLA and APT activities. It is our pleasure to thank Sydney Barnes and Yong-Cheol Kim for computing the moment-of-inertia models for us. We particularly thank our anonymous referee whose comments resulted in a much improved paper. J.B.R., J.M.M., D.B.G., A.F.J.M., and S.M.R. are supported by funding from the Natural Sciences and Engineering Research Council (NSERC) Canada. R.K. is funded by the Canadian Space Agency. W.W.W. is supported by the Austrian Science Promotion Agency (FFG-MOST) and the Austrian Science Funds (FWF-P17580). The APT operation has been supported by grants from the FWF to M. Breger and KGS. This work has made use of BaSTI web tools, the MESA code and of the many CDS-Strasbourg services. NR 120 TC 10 Z9 10 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD SEP-OCT PY 2010 VL 520 AR A52 DI 10.1051/0004-6361/201015023 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 665VQ UT WOS:000283064200075 ER PT J AU Gunther, HM Matt, SP Schmitt, JHMM Gudel, M Li, ZY Burton, DM AF Guenther, H. M. Matt, S. P. Schmitt, J. H. M. M. Guedel, M. Li, Z. -Y. Burton, D. M. TI The disk-bearing young star IM Lupi X-ray properties and limits on accretion SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: formation; stars: individual: IM Lup; X-rays: stars ID T-TAURI-STARS; MAIN-SEQUENCE STARS; NEWTON EXTENDED SURVEY; LOW-MASS STARS; EMISSION-LINES; BROWN DWARFS; MAGNETOSPHERIC ACCRETION; MOLECULAR CLOUD; ATOMIC DATABASE; HERBIG STAR AB Context. Classical T Tauri stars (CTTS) differ in their X-ray signatures from older pre-main sequence stars, e.g., weak-lined TTS (WTTS). CTTS exhibit a soft excess and deviations from the low-density coronal limit in the He-like triplets. Aims. We test whether these features correlate with either accretion or the presence of a disk by observing IM Lup, a disk-bearing object apparently in transition between CTTS and WTTS without obvious accretion. Methods. We analyse a Chandra grating spectrum and additional XMM-Newton data of IM Lup and accompanying optical spectra, some of which where taken simultaneously with the X-ray observations. We fit the X-ray emission lines and decompose the H alpha emission line into different components. Results. In X-rays, IM Lup has a bright and hot active corona, where elements with low first-ionisation potential are depleted. The He-like Ne IX triplet is in the low-density state, but because of the small number of counts in the data a high-density scenario cannot be excluded at the 90% confidence level. In terms of all its X-ray properties, IM Lup resembles a main-sequence star, but is also compatible with CTTS signatures at the 90% confidence level, thus we cannot decide whether the soft excess and deviations from the low-density coronal limit for the He-like triplets in CTTS are produced by accretion or only the presence of a disk. The star IM Lup is chromospherically active, which accounts for most of its emission in H alpha. Despite its low equivalent width, the complexity of the H alpha line profile is reminiscent of CTTS. We estimate the mass accretion rate to be 10(-11) M(circle dot) yr(-1). C1 [Guenther, H. M.; Schmitt, J. H. M. M.] Univ Hamburg, Hamburger Sternwarte, D-21029 Hamburg, Germany. [Guenther, H. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Matt, S. P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Guedel, M.] ETH, Inst Astron, CH-8093 Zurich, Switzerland. [Guedel, M.] Univ Vienna, Dept Astron, A-1180 Vienna, Austria. [Li, Z. -Y.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Burton, D. M.] Univ So Queensland, Toowoomba, Qld 4350, Australia. RP Gunther, HM (reprint author), Univ Hamburg, Hamburger Sternwarte, Gojenbergsweg 112, D-21029 Hamburg, Germany. EM moritz.guenther@hs.uni-hamburg.de RI Guedel, Manuel/C-8486-2015; OI Guedel, Manuel/0000-0001-9818-0588; Gunther, Hans Moritz/0000-0003-4243-2840; Matt, Sean/0000-0001-9590-2274 FU ESA Member States; NASA; NRL (USA); RAL (UK); MSSL (UK); Universities of Florence (Italy); Cambridge (UK); George Mason University (USA); La Silla Observatory [081.C-0779(A)]; DLR [50OR0105]; Oak Ridge Associated Universities; Chandra [GO9-0007X] FX Based on observations obtained with XMM-Newton, an ESA science mission, and Chandra, a NASA science mission, both with instruments and contributions directly funded by ESA Member States and NASA.; CHIANTI is a collaborative project involving the NRL (USA), RAL (UK), MSSL (UK), the Universities of Florence (Italy) and Cambridge (UK), and George Mason University (USA). We made use of observations made with ESO Telescopes at the La Silla Observatory under programme ID 081.C-0779(A). The authors would like to thank Ian Waite, USQ, for the initial extraction of the IM Lup data from ANU. H.M.G. acknowledges support from DLR under 50OR0105. S.P.M. was supported by an appointment to the NASA Postdoctoral Program at Ames Research Center, administered by Oak Ridge Associated Universities through a contract with NASA. Z.-Y.L. acknowledges support from Chandra grant GO9-0007X. NR 66 TC 5 Z9 5 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD SEP PY 2010 VL 519 AR A97 DI 10.1051/0004-6361/201014386 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 668UQ UT WOS:000283297300097 ER PT J AU Krivonos, R Revnivtsev, M Tsygankov, S Sazonov, S Vikhlinin, A Pavlinsky, M Churazov, E Sunyaev, R AF Krivonos, R. Revnivtsev, M. Tsygankov, S. Sazonov, S. Vikhlinin, A. Pavlinsky, M. Churazov, E. Sunyaev, R. TI INTEGRAL/IBIS 7-year All-Sky Hard X-ray Survey I. Image reconstruction SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE methods: data analysis; methods: observational; techniques: image processing; surveys; X-rays: general; Galaxy: general ID UNIFORMLY REDUNDANT ARRAYS; GALACTIC PLANE SCAN; SURVEY CATALOG; WAVELET TRANSFORM; IBIS TELESCOPE; COMA CLUSTER; REGION; EMISSION; MISSION; RIDGE AB This paper is the first in a series devoted to the hard X-ray whole sky survey performed by the INTEGRAL observatory over seven years. Here we present an improved method for image reconstruction with the IBIS coded mask telescope. The main improvements are related to the suppression of systematic effects that strongly limit sensitivity in the region of the Galactic plane (GP), especially in the crowded field of the Galactic center (GC). We extended the IBIS/ISGRI background model to take into account the Galactic ridge X-ray emission (GRXE). To suppress residual systematic artifacts on a reconstructed sky image, we applied nonparametric sky image filtering based on wavelet decomposition. The implemented modifications of the sky reconstruction method decrease the systematic noise in the similar to 20 Ms deep field of GC by similar to 44%, and practically remove it from the high-latitude sky images. New observational data sets, along with an improved reconstruction algorithm, allow us to conduct the hard X-ray survey with the best currently available minimal sensitivity 3.7 x 10(-12) erg s(-1) cm(-2) similar to 0.26 mCrab in the 17-60 keV band at a 5 sigma detection level. The survey covers 90% of the sky down to the flux limit of 6.2 x 10(-11) erg s(-1) cm(-2) (similar to 4.32 mCrab) and 10% of the sky area down to the flux limit of 8.6 x 10(-12) erg s(-1) cm(-2) (similar to 0.60 mCrab). C1 [Krivonos, R.; Tsygankov, S.; Churazov, E.; Sunyaev, R.] Max Planck Inst Astrophys, D-85740 Garching, Germany. [Krivonos, R.; Revnivtsev, M.; Tsygankov, S.; Sazonov, S.; Vikhlinin, A.; Pavlinsky, M.; Churazov, E.; Sunyaev, R.] Russian Acad Sci, Space Res Inst, Moscow 117997, Russia. [Revnivtsev, M.] Tech Univ Munich, D-85748 Garching, Germany. [Vikhlinin, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Krivonos, R (reprint author), Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85740 Garching, Germany. EM krivonos@mpa-garching.mpg.de RI Churazov, Eugene/A-7783-2013 FU Russian Federation [NSH-5069.2010.2]; Presidium of the Russian Academy of Sciences/RAS; Division of Physical Sciences of the RAS [OFN-17]; Russian Basic Research Foundation [09-02-00867]; Dynasty Foundation; ESA, Denmark; ESA, France; ESA, Germany; ESA, Italy; ESA, Switzerland; ESA, Spain; ESA, Czech Republic; ESA, Poland FX We are grateful to the anonymous referee for the critical remarks that helped us improve the paper. The data used were from the European and Russian INTEGRAL Science Data Centers2,3. The work was supported by the President of the Russian Federation (through the program supporting leading scientific schools, project NSH-5069.2010.2), by the Presidium of the Russian Academy of Sciences/RAS (the program "Origin, Structure, and Evolution of Objects of the Universe"), by the Division of Physical Sciences of the RAS (the program "Extended objects in the Universe", OFN-17), and by the Russian Basic Research Foundation (project 09-02-00867). S. S. acknowledges the support of the Dynasty Foundation. R. K. would like to express his sincere gratitude to Kate O'Shea for her support in the preparation of the paper.; Based on observations with INTEGRAL, an ESA project with the instruments and science data center funded by ESA member states (especially the PI countries: Denmark, France, Germany, Italy, Switzerland, Spain), Czech Republic, and Poland, and with the participation of Russia and the USA. NR 42 TC 32 Z9 32 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 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD SEP PY 2010 VL 519 AR A107 DI 10.1051/0004-6361/200913814 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 668UQ UT WOS:000283297300107 ER PT J AU Lombardi, M Alves, J Lada, CJ AF Lombardi, M. Alves, J. Lada, C. J. TI Larson's third law and the universality of molecular cloud structure SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: clouds; dust, extinction; ISM: structure; methods: statistical ID FIELD EXTINCTION MAPS; DUST; COMPLEXES; MASS; GAS AB Larson (1981) first noted a scaling relation between masses and sizes in molecular clouds that implies that these objects have approximately constant column densities. This original claim, based upon millimeter observations of carbon monoxide lines, has been challenged by many theorists, arguing that the apparent constant column density observed is merely the result of the limited dynamic range of observations, and that in reality clouds have column density variations over two orders of magnitudes. In this letter we investigate a set of nearby molecular clouds with near-infrared excess methods, which guarantee very large dynamic ranges and robust column density measurements, to test the validity of Larson's third law. We verify that different clouds have almost identical average column densities above a given extinction threshold; this holds regardless of the extinction threshold, but the actual average surface mass density is a function of the specific threshold used. We show that a second version of Larson's third law, involving the mass-radius relation for single clouds and cores, does not hold in our sample, indicating that individual clouds are not objects that can be described by constant column density. Our results instead indicate that molecular clouds are characterized by a universal structure. Finally we point out that this universal structure can be linked to the log-normal nature of cloud column density distributions. C1 [Lombardi, M.] Univ Milan, Dept Phys, I-20133 Milan, Italy. [Lombardi, M.] European So Observ, D-85748 Garching, Germany. [Alves, J.] Univ Vienna, A-1180 Vienna, Austria. [Lada, C. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Lombardi, M (reprint author), Univ Milan, Dept Phys, Via Celoria 16, I-20133 Milan, Italy. EM mlombard@eso.org OI LOMBARDI, MARCO/0000-0002-3336-4965; Alves, Joao/0000-0002-4355-0921 NR 26 TC 36 Z9 36 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 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD SEP PY 2010 VL 519 AR L7 DI 10.1051/0004-6361/201015282 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 668UQ UT WOS:000283297300124 ER PT J AU Wagg, J Carilli, CL Wilner, DJ Cox, P De Breuck, C Menten, K Riechers, DA Walter, F AF Wagg, J. Carilli, C. L. Wilner, D. J. Cox, P. De Breuck, C. Menten, K. Riechers, D. A. Walter, F. TI [CII] line emission in BRI 1335-0417 at z=4.4 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: high-redshift; galaxies: ISM ID C-II LINE; FAR-INFRARED SPECTROSCOPY; QUASAR HOST GALAXY; HIGH-REDSHIFT; STAR-FORMATION; MOLECULAR GAS; BIG-BANG; MU-M; STARBURST; QSOS AB Using the 12-m APEX telescope, we have detected redshifted emission from the 157.74 mu m [CII] line in the z = 4.4074 quasar BRI 1335-0417. The linewidth and redshift are in good agreement with previous observations of high-J CO line emission. We measure a [CII] line luminosity, L([CII]) = (16.4 +/- 2.6) x 10(9) L(circle dot), making BRI 1335-0417 the most luminous, unlensed [CII] line emitter known at high-redshift. The [CII]-to-FIR luminosity ratio of (5.3 +/- 0.8) x 10(-4) is similar to 3x higher than expected for an average object with a FIR luminosity L(FIR) = 3.1 x 10(13) L(circle dot), if this ratio were to follow the trend observed in other FIR-bright galaxies that have been detected in [CII] line emission. These new data suggest that the scatter in the [CII]-to-FIR luminosity ratio could be larger than previously expected for high luminosity objects. BR1335-0417 has a similar FIR luminosity and [CII]/CO luminosity compared to local ULIRGS and appears to be a gas-rich merger forming stars at a rate of a few thousand solar masses per year. C1 [Wagg, J.] European So Observ, Santiago 19, Chile. [Carilli, C. L.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Wilner, D. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Cox, P.] Inst Radioastron Millimetr, F-38406 St Martin Dheres, France. [De Breuck, C.] European So Observ, D-85748 Garching, Germany. [Menten, K.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Riechers, D. A.] CALTECH, Pasadena, CA 91125 USA. [Walter, F.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. RP Wagg, J (reprint author), European So Observ, Casilla 19001, Santiago 19, Chile. EM jwagg@eso.org OI De Breuck, Carlos/0000-0002-6637-3315 FU NASA [HST-HF-51235.01, NAS 5-26555] FX We thank the staff of the APEX telescope for help with the observations and data analysis. In particular we thank Thomas Stanke, Andreas Lundgren, Rodrigo Parra, Francisco Montenegro, Giorgio Siringo, and Claudio Agurto. D. R. acknowledges support from from NASA through Hubble Fellowship grant HST-HF-51235.01 awarded by STScI, operated by AURA for NASA, under contract NAS 5-26555. We thank the referee for useful comments and suggestions on the manuscript. NR 27 TC 37 Z9 37 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD SEP PY 2010 VL 519 AR L1 DI 10.1051/0004-6361/201015424 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 668UQ UT WOS:000283297300118 ER PT J AU Gonzalez, AH Papovich, C Bradac, M Jones, C AF Gonzalez, Anthony H. Papovich, Casey Bradac, Marusa Jones, Christine TI SPECTROSCOPIC CONFIRMATION OF A z=2.79 MULTIPLY IMAGED LUMINOUS INFRARED GALAXY BEHIND THE BULLET CLUSTER SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: high-redshift; galaxies: starburst; gravitational lensing: strong ID STAR-FORMING GALAXIES; LYMAN BREAK GALAXY; AROMATIC-HYDROCARBON EMISSION; SPITZER-SPACE-TELESCOPE; INITIAL MASS FUNCTION; MIDINFRARED SPECTROSCOPY; REDSHIFT Z-SIMILAR-TO-2; SUBMILLIMETER GALAXIES; DUST; EVOLUTION AB We report spectroscopic confirmation and high-resolution infrared imaging of a z = 2.79 triply imaged galaxy behind the Bullet Cluster. This source, a Spitzer-selected luminous infrared galaxy, is confirmed via polycyclic aromatic hydrocarbon (PAH) features using the Spitzer Infrared Spectrograph (IRS) and resolved with Hubble Space Telescope Wide Field Camera 3 imaging. In this galaxy, which with a stellar mass M* approximate to 4 x 10(9) M(circle dot) is one of the two least massive ones studied with IRS at z > 2, we also detect H(2) S(4) and H(2) S(5) pure rotational lines (at 3.1 sigma and 2.1 sigma)-the first detection of these molecular hydrogen lines in a high-redshift galaxy. From the molecular hydrogen lines we infer an excitation temperature T = 377(-84)(+68) K. The detection of these lines indicates that the warm molecular gas mass is 6(-4)(+346)% of the stellar mass and implies the likely existence of a substantial reservoir of cold molecular gas in the galaxy. Future spectral observations at longer wavelengths with facilities such as the Herschel Space Observatory, the Large Millimeter Telescope, and the Atacama Pathfinder Experiment thus hold the promise of precisely determining the total molecular gas mass. Given the redshift, and using refined astrometric positions from the high-resolution imaging, we also update the magnification estimate and derived fundamental physical properties of this system. The previously published values for L(IR), star formation rate, and dust temperature are confirmed modulo the revised magnification; however, we find that PAH emission is roughly a factor of 5 stronger than would be predicted by the relations between L(IR) and L(PAH) reported for SMGs and starbursts in Pope et al. C1 [Gonzalez, Anthony H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Papovich, Casey] Texas A&M Univ, Dept Phys, College Stn, TX 77843 USA. [Bradac, Marusa] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Jones, Christine] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gonzalez, AH (reprint author), Univ Florida, Dept Astron, Gainesville, FL 32611 USA. EM anthony@astro.ufl.edu FU NASA; NASA/HST [HST-GO-10200, HST-GO-10863, HST-GO-11099]; NASA/Spitzer [1319141, 1376614] FX A.H.G. and C.P. thank Eiichi Egami, Jane Rigby, and Ranga-Ram Chary for constructive discussions related to this work. The authors also thank the anonymous referee for comments that improved this paper. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. The authors acknowledge support for this work from NASA/HST grants HST-GO-10200, HST-GO-10863, and HST-GO-11099, as well as NASA/Spitzer grants 1319141 and 1376614. NR 46 TC 10 Z9 10 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2010 VL 720 IS 1 BP 245 EP 251 DI 10.1088/0004-637X/720/1/245 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 647DJ UT WOS:000281596000021 ER PT J AU Slane, P Castro, D Funk, S Uchiyama, Y Lemiere, A Gelfand, JD Lemoine-Goumard, M AF Slane, P. Castro, D. Funk, S. Uchiyama, Y. Lemiere, A. Gelfand, J. D. Lemoine-Goumard, M. TI FERMI DETECTION OF THE PULSAR WIND NEBULA HESS J1640-465 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual objects (HESS J1640-465, FGL J1640.8-4634, 3EG J1639-4702, G338.3-0.0); ISM: supernova remnants; pulsars: general ID LARGE-AREA TELESCOPE; GAMMA-RAY EMISSION; SUPERNOVA REMNANT; RX J1713.7-3946; X-RAY; EVOLUTION; ACCELERATION; SPECTRUM; CATALOG; GALAXY AB We present observations of HESS J1640-465 with the Fermi-Large Area Telescope. The source is detected with high confidence as an emitter of high-energy gamma-rays. The spectrum lacks any evidence for the characteristic cutoff associated with emission from pulsars, indicating that the emission arises primarily from the pulsar wind nebula (PWN). Broadband modeling implies an evolved nebula with a low magnetic field resulting in a high gamma-ray to X-ray flux ratio. The Fermi emission exceeds predictions of the broadband model, and has a steeper spectrum, possibly resulting from a distinct excess of low energy electrons similar to what is inferred for both the Vela X and Crab PWNe. C1 [Slane, P.; Castro, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Castro, D.] Univ Simon Bolivar, Dept Fis, Valle De Sartenejas, Venezuela. [Funk, S.; Uchiyama, Y.] Stanford Linear Accelerator Ctr, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94025 USA. [Lemiere, A.] CNRS, IN2P3, Inst Phys Nucl, F-91400 Orsay, France. [Gelfand, J. D.] NYU, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [Lemoine-Goumard, M.] Univ Bordeaux, CNRS, IN2P3, Ctr Etud Nucl Bordeaux Gradignan,UMR 5797, F-33175 Gradignan, France. RP Slane, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM slane@cfa.harvard.edu; dcastro@head.cfa.harvard.edu; funk@slac.stanford.edu; uchiyama@slac.stanford.edu RI Funk, Stefan/B-7629-2015; Gelfand, Joseph/F-1110-2015 OI Funk, Stefan/0000-0002-2012-0080; Gelfand, Joseph/0000-0003-4679-1058 FU NASA [NAS8-39073]; Fermi [NNX09AT68G]; NSF [AST-0702957]; INAF in Italy; CNES in France FX The work presented here was supported in part by NASA Contract NAS8-39073 (P.O.S.) and Fermi Grant NNX09AT68G. J.D.G. is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-0702957. P.O.S., S.F., and Y.U. are grateful to the KITP in Santa Barbara, where elements of the work presented here were first discussed during a KITP program. The authors thank Don Ellison, Luke Drury, Felix Aharonian, and David Smith for helpful discussions during the preparation of this paper.; The Fermi-LAT Collaboration acknowledges support from a number of agencies and institutes for both development and the operation of the LAT as well as scientific data analysis. These include NASA and DOE in the United States, CEA/Irfu and IN2P3/CNRS in France, ASI and INFN in Italy, MEXT, KEK, and JAXA in Japan, and the K. A. Wallenberg Foundation, the Swedish Research Council and the National Space Board in Sweden. Additional support from INAF in Italy and CNES in France for science analysis during the operations phase is also gratefully acknowledged. NR 35 TC 33 Z9 33 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2010 VL 720 IS 1 BP 266 EP 271 DI 10.1088/0004-637X/720/1/266 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 647DJ UT WOS:000281596000024 ER PT J AU Mancone, CL Gonzalez, AH Brodwin, M Stanford, SA Eisenhardt, PRM Stern, D Jones, C AF Mancone, Conor L. Gonzalez, Anthony H. Brodwin, Mark Stanford, Spencer A. Eisenhardt, Peter R. M. Stern, Daniel Jones, Christine TI THE FORMATION OF MASSIVE CLUSTER GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: general; galaxies: evolution galaxies: formation; galaxies: luminosity function, mass function ID IRAC SHALLOW SURVEY; STELLAR POPULATION SYNTHESIS; NEAR-INFRARED PROPERTIES; LUMINOSITY FUNCTION; RED SEQUENCE; STAR-FORMATION; EVOLUTION; SPITZER; 1ST; UNCERTAINTIES AB We present composite 3.6 and 4.5 mu m luminosity functions (LFs) for cluster galaxies measured from the Spitzer Deep, Wide-Field Survey for 0.3 < z < 2. We compare the evolution of m* for these LFs to models for passively evolving stellar populations to constrain the primary epoch of star formation in massive cluster galaxies. At low redshifts (z less than or similar to 1.3), our results agree well with models with no mass assembly and passively evolving stellar populations with a luminosity-weighted mean formation redshift z(f) = 2.4 assuming a Kroupa initial mass function (IMF). We conduct a thorough investigation of systematic biases that might influence our results, and estimate systematic uncertainties of Delta z(f) = (+0.16)(-0.18) (model normalization), Delta z(f) = (+0.40)(-0.05) (a), and Delta z(f) = (+0.30)(-0.45) (choice of stellar population model). For a Salpeter-type IMF, the typical formation epoch is thus strongly constrained to be z similar to 2-3. Higher formation redshifts can only be made consistent with the data if one permits an evolving IMF that is bottom-light at high redshift, as suggested by van Dokkum. At high redshifts (z greater than or similar to 1.3), we also witness a statistically significant (>5 sigma) disagreement between the measured LF and the continuation of the passive evolution model from lower redshifts. After considering potential systematic biases that might influence our highest redshift data points, we interpret the observed deviation as potential evidence for ongoing mass assembly at this epoch. C1 [Mancone, Conor L.; Gonzalez, Anthony H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Brodwin, Mark; Jones, Christine] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Stanford, Spencer A.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Stanford, Spencer A.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94550 USA. [Eisenhardt, Peter R. M.; Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Mancone, CL (reprint author), Univ Florida, Dept Astron, Gainesville, FL 32611 USA. EM cmaneone@astro.ufl.edu; anthony@astro.ufl.edu FU National Science Foundation [AST-0708490]; U.S. Department of Energy by Lawrence Livermore National Laboratory [W-7405-Eng-48, DE-AC52-07NA27344]; NASA FX This paper is based upon work supported by the National Science Foundation under grant AST-0708490. Part of this work was performed under the auspices of the U.S. Department of Energy by Lawrence Livermore National Laboratory in part under Contract W-7405-Eng-48 and in part under Contract DE-AC52-07NA27344. The work of P.R.M.E. and D.S. was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. NR 40 TC 46 Z9 46 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2010 VL 720 IS 1 BP 284 EP 298 DI 10.1088/0004-637X/720/1/284 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 647DJ UT WOS:000281596000026 ER PT J AU Oberg, KI Qi, CH Fogel, JKJ Bergin, EA Andrews, SM Espaillat, C van Kempen, TA Wiener, DJ Pascucci, I AF Oberg, Karin I. Qi, Chunhua Fogel, Jeffrey K. J. Bergin, Edwin A. Andrews, Sean M. Espaillat, Catherine van Kempen, Tim A. Wiener, David J. Pascucci, Ilaria TI THE DISK IMAGING SURVEY OF CHEMISTRY WITH SMA. I. TAURUS PROTOPLANETARY DISK DATA SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; ISM: molecules; protoplanetary disks; radio lines: ISM; stars: formation; techniques: high angular resolution ID HERBIG-AE STARS; INTERMEDIATE-MASS STARS; T-TAURI; CIRCUMSTELLAR DISKS; HIGH-RESOLUTION; GM-AURIGAE; DM-TAURI; DEUTERATED MOLECULES; TRANSITIONAL DISKS; ACCRETION RATES AB Chemistry plays an important role in the structure and evolution of protoplanetary disks, with implications for the composition of comets and planets. This is the first of a series of papers based on data from DISCS, a Submillimeter Array survey of the chemical composition of protoplanetary disks. The six Taurus sources in the program (DM Tau, AA Tau, LkCa 15, GM Aur, CQ Tau, and MWC 480) range in stellar spectral type from M1 to A4 and offer an opportunity to test the effects of stellar luminosity on the disk chemistry. The disks were observed in 10 different lines at similar to 3" resolution and an rms of similar to 100 mJy beam(-1) at similar to 0.5 km s(-1). The four brightest lines are CO 2-1, HCO(+) 3-2, CN 2(33/4/2) - 1(22/3/1), and HCN 3-2, and these are detected toward all sources (except for HCN toward CQ Tau). The weaker lines of CN 2(22)-1(11), DCO(+) 3-2, N(2)H(+) 3-2, H(2)CO 3(03)-2(02), and 4(14)-3(13) are detected toward two to three disks each, and DCN 3-2 only toward LkCa 15. CH(3)OH 4(21)-3(12) and c-C(3)H(2) are not detected. There is no obvious difference between the T Tauri and Herbig Ae sources with regard to CN and HCN intensities. In contrast, DCO(+), DCN, N(2)H(+), and H(2)CO are detected only toward the T Tauri stars, suggesting that the disks around Herbig Ae stars lack cold regions for long enough timescales to allow for efficient deuterium chemistry, CO freeze-out, and grain chemistry. C1 [Oberg, Karin I.; Qi, Chunhua; Andrews, Sean M.; Espaillat, Catherine; van Kempen, Tim A.; Wiener, David J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fogel, Jeffrey K. J.; Bergin, Edwin A.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Pascucci, Ilaria] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP Oberg, KI (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU NASA [NAS 5-26555]; National Science Foundation [0901947, 0707777]; Smithsonian Institution; Academia Sinica FX This work has benefited from discussions with and comments from Ewine van Dishoeck, Geoffrey Blake, and Michiel Hogerheijde, and from a helpful review by an anonymous referee. The SMA is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. Support for K.I.O. and S.M.A. is provided by NASA through Hubble Fellowship grants 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. C.E. was supported by the National Science Foundation under Award No. 0901947. E.A.B. acknowledges support from NSF Grant 0707777. NR 84 TC 60 Z9 60 U1 0 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2010 VL 720 IS 1 BP 480 EP 493 DI 10.1088/0004-637X/720/1/480 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 647DJ UT WOS:000281596000040 ER PT J AU Liu, GC Birkinshaw, M Wu, JHP Ho, PTP Huang, CWL Liao, YW Lin, KY Molnar, SM Nishioka, H Koch, PM Umetsu, K Wang, FC Altamirano, P Chang, CH Chang, SH Chang, SW Chen, MT Han, CC Huang, YD Hwang, YJ Jiang, HM Kesteven, M Kubo, D Li, CT Martin-Cocher, P Oshiro, P Raffin, P Wei, T Wilson, W AF Liu, Guo-Chin Birkinshaw, Mark Wu, Jiun-Huei Proty Ho, Paul T. P. Huang, Chih-Wei Locutus Liao, Yu-Wei Lin, Kai-Yang Molnar, Sandor M. Nishioka, Hiroaki Koch, Patrick M. Umetsu, Keiichi Wang, Fu-Cheng Altamirano, Pablo Chang, Ciia-Hao Chang, Shu-Hao Chang, Su-Wei Chen, Ming-Tang Han, Chih-Chiang Huang, Yau-De Hwang, Yuh-Jing Jiang, Homin Kesteven, Michael Kubo, Derek Li, Chao-Te Martin-Cocher, Pierre Oshiro, Peter Raffin, Philippe Wei, Tashun Wilson, Warwick TI CONTAMINATION OF THE CENTRAL SUNYAEV-ZEL'DOVICH DECREMENTS IN AMiBA GALAXY CLUSTER OBSERVATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic background radiation; cosmology: observations; diffuse radiation; galaxies: clusters: general ID MICROWAVE BACKGROUND ANISOTROPY; RADIO-SOURCES; SCALING RELATIONS; SOURCE CATALOG; X-RAY; ARRAY; MASS; CMB AB We investigate the contamination of the Sunyaev-Zel'dovich (SZ) effect for six galaxy clusters, A1689, A1995, A2142, A2163, A2261, and A2390, observed by the Y. T. Lee Array for Microwave Background Anisotropy in 2007. With the range of baselines used, we find that the largest effect (of order 13%-50% of the central SZ flux density) comes from primary anisotropies in the cosmic microwave background and exceeds the thermal noise in all six cases. Contamination from discrete radio sources is estimated to be at a level of 3%-60% of the central SZ flux density. We use the statistics of these contaminating sources to estimate and correct the errors in the measured SZ effects of these clusters. C1 [Liu, Guo-Chin; Ho, Paul T. P.; Lin, Kai-Yang; Molnar, Sandor M.; Nishioka, Hiroaki; Koch, Patrick M.; Umetsu, Keiichi; Altamirano, Pablo; Chang, Ciia-Hao; Chang, Shu-Hao; Chang, Su-Wei; Chen, Ming-Tang; Han, Chih-Chiang; Huang, Yau-De; Hwang, Yuh-Jing; Jiang, Homin; Kubo, Derek; Li, Chao-Te; Martin-Cocher, Pierre; Oshiro, Peter; Raffin, Philippe; Wei, Tashun] Inst Astron & Astrophys, Acad Sinica, Taipei 106, Taiwan. [Liu, Guo-Chin] Tamkang Univ, Dept Phys, Tamsui 25137, Taipei County, Taiwan. [Birkinshaw, Mark] Univ Bristol, Dept Phys, Bristol BS8 1TL, Avon, England. [Wu, Jiun-Huei Proty; Huang, Chih-Wei Locutus; Liao, Yu-Wei; Lin, Kai-Yang; Wang, Fu-Cheng] Natl Taiwan Univ, Dept Phys, Inst Astrophys, Taipei 10617, Taiwan. [Wu, Jiun-Huei Proty; Huang, Chih-Wei Locutus; Liao, Yu-Wei; Lin, Kai-Yang; Wang, Fu-Cheng] Natl Taiwan Univ, Ctr Theoret Sci, Taipei 10617, Taiwan. [Ho, Paul T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kesteven, Michael; Wilson, Warwick] Australia Telescope Natl Facil, Epping, NSW 1710, Australia. RP Liu, GC (reprint author), Inst Astron & Astrophys, Acad Sinica, POB 23-141, Taipei 106, Taiwan. OI WU, JIUN-HUEI/0000-0001-9608-7662; Umetsu, Keiichi/0000-0002-7196-4822 FU STFC; National Science Council of Taiwan [NSC97-2112-M-032-007-MY3, NSC97-2112-M-001-020-MY3] FX We acknowledge the extensive use we have made of data from the WMAP satellite, and thank Dr. L. Chiang for fruitful discussions on Galactic emission and the WMAP data. We also appreciate discussions with Drs. N. Aghanim and S. Matsushita on radio source properties. Support from the STFC for MB is acknowledged. This work is partially supported by the National Science Council of Taiwan under grants NSC97-2112-M-032-007-MY3 and NSC97-2112-M-001-020-MY3. NR 31 TC 4 Z9 4 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2010 VL 720 IS 1 BP 608 EP 613 DI 10.1088/0004-637X/720/1/608 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 647DJ UT WOS:000281596000052 ER PT J AU Espada, D Peck, AB Matsushita, S Sakamoto, K Henkel, C Iono, D Israel, FP Muller, S Petitpas, G Pihlstrom, Y Taylor, GB Trung, DV AF Espada, D. Peck, A. B. Matsushita, S. Sakamoto, K. Henkel, C. Iono, D. Israel, F. P. Muller, S. Petitpas, G. Pihlstrom, Y. Taylor, G. B. Trung, D. V. TI DISENTANGLING THE CIRCUMNUCLEAR ENVIRONS OF CENTAURUS A. II. ON THE NATURE OF THE BROAD ABSORPTION LINE SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: elliptical and lenticular, cD; galaxies: individual (NGC 5128); galaxies: ISM; galaxies: structure; quasars: absorption lines ID NUCLEAR STARBURST ENVIRONMENT; H-I ABSORPTION; MOLECULAR ABSORPTION; RADIO GALAXY; NEARBY GALAXIES; CARBON-MONOXIDE; SCALE STRUCTURE; DENSE GAS; NGC 5128; EMISSION AB We report on atomic gas (Hi) and molecular gas (as traced by CO(2-1)) redshifted absorption features toward the nuclear regions of the closest powerful radio galaxy, Centaurus A (NGC 5128). Our Hi observations using the Very Long Baseline Array allow us to discern with unprecedented sub-parsec resolution Hi absorption profiles toward different positions along the 21 cm continuum jet in the inner 0 ''.3 (or 5.4 pc). In addition, our CO(2-1) data obtained with the Submillimeter Array probe the bulk of the absorbing molecular gas with little contamination by emission, which was not possible with previous CO single-dish observations. We shed light on the physical properties of the gas in the line of sight with these data, emphasizing the still open debate about the nature of the gas that produces the broad absorption line (similar to 55 km s(-1)). First, the broad Hi line is more prominent toward the central and brightest 21 cm continuum component than toward a region along the jet at a distance similar to 20 mas (or 0.4 pc) further from the nucleus. This indicates that the broad absorption line arises from gas located close to the nucleus, rather than from diffuse and more distant gas. Second, the different velocity components detected in the CO(2-1) absorption spectrum match well with other molecular lines, such as those of HCO(+)(1-0), except the broad absorption line that is detected in HCO(+)(1-0) (and most likely related to that of the HI). Dissociation of molecular hydrogen due to the active galactic nucleus seems to be efficient at distances r less than or similar to 10 pc, which might contribute to the depth of the broad Hi and molecular lines. C1 [Espada, D.; Matsushita, S.; Sakamoto, K.; Trung, D. V.] Inst Astron & Astrophys, Acad Sinica, Taipei 10617, Taiwan. [Espada, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Espada, D.] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. [Peck, A. B.; Matsushita, S.] Joint ALMA Off, Santiago, Chile. [Peck, A. B.; Petitpas, G.] Harvard Smithsonian Ctr Astrophys, Hilo, HI 96720 USA. [Peck, A. B.; Pihlstrom, Y.; Taylor, G. B.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Henkel, C.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Iono, D.] NAOJ, Nobeyama Radio Observ, Minamimaki, Nagano 3841305, Japan. [Israel, F. P.] Leiden Univ, Sterrewacht Leiden, NL-2300 RA Leiden, Netherlands. [Muller, S.] Onsala Space Observ, SE-43992 Onsala, Sweden. [Pihlstrom, Y.; Taylor, G. B.] Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA. [Trung, D. V.] Vietnam Acad Sci & Technol, Ctr Quantum Elect, Inst Phys, Hanoi, Vietnam. RP Espada, D (reprint author), Inst Astron & Astrophys, Acad Sinica, POB 23-141, Taipei 10617, Taiwan. EM despada@cfa.harvard.edu OI /0000-0002-9931-1313 FU National Aeronautics and Space Administration; European Community [MOIF-CT-2006-40298] FX We thank the SMA and NRAO staff members who made the observations reported here possible. We also thank A. Sarma for providing the 21 cm continuum VLA data, and S. Martin and I. Jimenez-Serra for interesting discussions. This research has made use of NASA's Astrophysics Data System Bibliographic Services and has also 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. D.E. was supported by a Marie Curie International Fellowship within the 6th European Community Framework Programme (MOIF-CT-2006-40298). NR 51 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 J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2010 VL 720 IS 1 BP 666 EP 678 DI 10.1088/0004-637X/720/1/666 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 647DJ UT WOS:000281596000058 ER PT J AU Beerer, IM Koenig, XP Hora, JL Gutermuth, RA Bontemps, S Megeath, ST Schneider, N Motte, F Carey, S Simon, R Keto, E Smith, HA Allen, LE Fazio, GG Kraemer, KE Price, S Mizuno, D Adams, JD Hernandez, J Lucas, PW AF Beerer, I. M. Koenig, X. P. Hora, J. L. Gutermuth, R. A. Bontemps, S. Megeath, S. T. Schneider, N. Motte, F. Carey, S. Simon, R. Keto, E. Smith, H. A. Allen, L. E. Fazio, G. G. Kraemer, K. E. Price, S. Mizuno, D. Adams, J. D. Hernandez, J. Lucas, P. W. TI A SPITZER VIEW OF STAR FORMATION IN THE CYGNUS X NORTH COMPLEX SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared: stars; H II regions; stars: early-type; stars: formation; stars: pre-main sequence ID GALACTIC PLANE IPHAS; H-ALPHA SURVEY; MOLECULAR CLOUD; OB ASSOCIATIONS; SPACE-TELESCOPE; CLUSTER; REGION; 2MASS; SKY; SPECTROGRAPH AB We present new images and photometry of the massive star-forming complex Cygnus X obtained with the Infrared Array Camera (IRAC) and the Multiband Imaging Photometer for Spitzer (MIPS) on board the Spitzer Space Telescope. A combination of IRAC, MIPS, UKIRT Deep Infrared Sky Survey, and Two Micron All Sky Survey data are used to identify and classify young stellar objects (YSOs). Of the 8231 sources detected exhibiting infrared excess in Cygnus X North, 670 are classified as class I and 7249 are classified as class II. Using spectra from the FAST Spectrograph at the Fred L. Whipple Observatory and Hectospec on the MMT, we spectrally typed 536 sources in the Cygnus X complex to identify the massive stars. We find that YSOs tend to be grouped in the neighborhoods of massive B stars (spectral types B0 to B9). We present a minimal spanning tree analysis of clusters in two regions in Cygnus X North. The fraction of infrared excess sources that belong to clusters with >= 10 members is found to be 50%-70%. Most class II objects lie in dense clusters within blown out H II regions, while class I sources tend to reside in more filamentary structures along the bright-rimmed clouds, indicating possible triggered star formation. C1 [Beerer, I. M.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Koenig, X. P.; Hora, J. L.; Keto, E.; Smith, H. A.; Fazio, G. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gutermuth, R. A.] Smith Coll, Northampton, MA 01063 USA. [Gutermuth, R. A.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Bontemps, S.; Schneider, N.] Observ Bordeaux, F-33270 Floirac, France. [Megeath, S. T.] Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA. [Motte, F.] CEA Saclay, AIM SAp, F-91191 Gif Sur Yvette, France. [Carey, S.] Spitzer Sci Ctr, Pasadena, CA USA. [Simon, R.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Allen, L. E.] Natl Opt Astron Observ, Tucson, AZ USA. [Kraemer, K. E.; Price, S.] USAF, Res Lab, Hanscom AFB, MA USA. [Mizuno, D.] Boston Coll, Inst Sci Res, Boston, MA USA. [Adams, J. D.] Cornell Univ, Dept Radiophys Space Res, Ithaca, NY USA. [Hernandez, J.] Ctr Invest Astron, Merida 5101 A, Venezuela. [Lucas, P. W.] Univ Hertfordshire, Ctr Astrophys Res, Harefield, Middx, England. [Lucas, P. W.] Univ Hertfordshire, Sci & Technol Res Inst, Harefield, Middx, England. RP Beerer, IM (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. OI Koenig, Xavier/0000-0002-9478-4170; Hora, Joseph/0000-0002-5599-4650; Kraemer, Kathleen/0000-0002-2626-7155 FU NASA; National Science Foundation; Department of Defense [0754568]; Smithsonian Institution 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 NASA. This work was supported in part by the National Science Foundation Research Experiences for Undergraduates (REU) and Department of Defense Awards to Stimulate and Support Undergraduate Research Experiences (ASSURE) programs under grant No. 0754568 and by the Smithsonian Institution. NR 54 TC 22 Z9 22 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2010 VL 720 IS 1 BP 679 EP 693 DI 10.1088/0004-637X/720/1/679 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 647DJ UT WOS:000281596000059 ER PT J AU McClelland, CM Garnavich, PM Galbany, L Miquel, R Foley, RJ Filippenko, AV Bassett, B Wheeler, JC Goobar, A Jha, SW Sako, M Frieman, JA Sollerman, J Vinko, J Schneider, DP AF McClelland, Colin M. Garnavich, Peter M. Galbany, Lluis Miquel, Ramon Foley, Ryan J. Filippenko, Alexei V. Bassett, Bruce Wheeler, J. Craig Goobar, Ariel Jha, Saurabh W. Sako, Masao Frieman, Joshua A. Sollerman, Jesper Vinko, Jozsef Schneider, Donald P. TI THE SUBLUMINOUS SUPERNOVA 2007qd: A MISSING LINK IN A FAMILY OF LOW-LUMINOSITY TYPE Ia SUPERNOVAE SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: individual (SDSS J020932.73-005959.8); supernovae: general; supernovae: individual (SN 2007qd, SN 2008ha, SN 2002cx, SN 2005hk) ID DIGITAL SKY SURVEY; LIGHT-CURVE SHAPES; HUBBLE-SPACE-TELESCOPE; SN 2008HA; MODELS; CONSTANT; CONSTRAINTS; PROGENITOR; DISTANCE; SPECTRA AB We present multi-band photometry and multi-epoch spectroscopy of the peculiar Type Ia supernova (SN la) 2007qd, discovered by the SDSS-II Supernova Survey. It possesses physical properties intermediate to those of the peculiar SN 2002cx and the extremely low-luminosity SN 2008ha. Optical photometry indicates that it had an extraordinarily fast rise time of less than or similar to 10 days and a peak absolute B magnitude of -15.4 +/- 0.2 at most, making it one of the most subluminous SN la ever observed. Follow-up spectroscopy of SN 2007qd near maximum brightness unambiguously shows the presence of intermediate-mass elements which are likely caused by carbon/oxygen nuclear burning. Near maximum brightness, SN 2007qd had a photospheric velocity of only 2800 km s(-1), similar to that of SN 2008ha but about 4000 and 7000 km s(-1) less than that of SN 2002cx and normal SN la, respectively. We show that the peak luminosities of SN 2002cx like objects are highly correlated with both their light-curve stretch and photospheric velocities. Its strong apparent connection to other SN 2002cx like events suggests that SN 2007qd is also a pure deflagration of a white dwarf, although other mechanisms cannot be ruled out. It may be a critical link between SN 2008ha and the other members of the SN 2002cx like class of objects. C1 [McClelland, Colin M.; Garnavich, Peter M.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Galbany, Lluis; Miquel, Ramon] Univ Autonoma Barcelona, Inst Fis Altes Energies, E-08193 Barcelona, Spain. [Miquel, Ramon] Inst Catalana Recerca & Estudis Avancats, E-08010 Barcelona, Spain. [Foley, Ryan J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Filippenko, Alexei V.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Bassett, Bruce] Univ Cape Town, Dept Math & Appl Math, ZA-7701 Rondebosch, South Africa. [Wheeler, J. Craig] Univ Texas Austin, Dept Astron, McDonald Observ, Austin, TX 78712 USA. [Goobar, Ariel] Stockholm Univ, Dept Phys, AlbaNova Univ Ctr, SE-10691 Stockholm, Sweden. [Goobar, Ariel] Stockholm Univ, Dept Phys, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden. [Jha, Saurabh W.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Sako, Masao] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Frieman, Joshua A.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Frieman, Joshua A.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Frieman, Joshua A.] Fermilab Natl Accelerator Lab, Ctr Particle Astrophys, Batavia, IL 60510 USA. [Sollerman, Jesper] Univ Copenhagen, Dark Cosmol Ctr, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Sollerman, Jesper] Stockholm Univ, Dept Astron, Oskar Klein Ctr, S-10691 Stockholm, Sweden. [Vinko, Jozsef] Univ Szeged, Dept Opt & Quantum Elect, Szeged, Hungary. [Schneider, Donald P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. RP McClelland, CM (reprint author), Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. RI Galbany, Lluis/A-8963-2017; OI Galbany, Lluis/0000-0002-1296-6887; Bassett, Bruce/0000-0001-7700-1069; Sollerman, Jesper/0000-0003-1546-6615; Vinko, Jozsef/0000-0001-8764-7832; Miquel, Ramon/0000-0002-6610-4836 FU Alfred P. Sloan Foundation; National Science Foundation (NSF) [AST-0908886, AST-0847157]; U.S. Department of Energy (DOE); National Aeronautics and Space Administration (NASA); Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England; American Museum of Natural History; Astrophysical Institute Potsdam; University of Basel; University of Cambridge; Case Western Reserve University; University of Chicago; Drexel University; Fermilab; Institute for Advanced Study; Japan Participation Group; Johns Hopkins University; Joint Institute for Nuclear Astrophysics; Kavli Institute for Particle Astrophysics and Cosmology; Korean Scientist Group; Chinese Academy of Sciences; 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; W. M. Keck Foundation; University of Notre Dame; NASA/STScI [HST-GO-10893.01-A]; DOE [DE-FG02-08ER41563, DE-FG02-08ER41562] FX Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation (NSF), the U.S. Department of Energy (DOE), the National Aeronautics and Space Administration (NASA), the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England.; The SDSS Web site is http://www.sdss.org/. The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington.; 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; it was made possible by the generous financial support of the W. M. Keck Foundation. The authors recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community; we are most fortunate to have the opportunity to conduct observations from this mountain. We thank the Keck staff for their assistance.; We are grateful for the financial support of the University of Notre Dame, NASA/STScI Grant HST-GO-10893.01-A to C.M.M., the NSF, and the DOE, specifically NSF grant AST-0908886 and DOE grant DE-FG02-08ER41563 to A.V.F. Support for this research at Rutgers University was provided by DOE grant DE-FG02-08ER41562 and NSF award AST-0847157 to S.W.J. We thank Brian Hayden, Joe Gallagher, and Weidong Li for discussions and their help in the production of this paper, Jerod Parrent and the Online Supernova Spectrum Archive (SUSPECT), and David Jeffery along with the SUSPEND database. NR 97 TC 33 Z9 33 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 SEP 1 PY 2010 VL 720 IS 1 BP 704 EP 716 DI 10.1088/0004-637X/720/1/704 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 647DJ UT WOS:000281596000061 ER PT J AU Burke, DL Axelrod, T Blondin, S Claver, C Ivezic, Z Jones, L Saha, A Smith, A Smith, RC Stubbs, CW AF Burke, David L. Axelrod, T. Blondin, Stephane Claver, Chuck Ivezic, Zeljko Jones, Lynne Saha, Abhijit Smith, Allyn Smith, R. Chris Stubbs, Christopher W. TI PRECISION DETERMINATION OF ATMOSPHERIC EXTINCTION AT OPTICAL AND NEAR-INFRARED WAVELENGTHS SO ASTROPHYSICAL JOURNAL LA English DT Article DE atmospheric effects; methods: observational; surveys; techniques: photometric ID DIGITAL SKY SURVEY; STANDARD STARS; CALIBRATION; PHOTOMETRY; CATALOG AB The science goals for future ground-based all-sky surveys, such as the Dark Energy Survey, PanSTARRS, and the Large Synoptic Survey Telescope, require calibration of broadband photometry that is stable in time and uniform over the sky to precisions of 1% or better, and absolute calibration of color measurements that are similarly accurate. This performance will need to be achieved with measurements made from multiple images taken over the course of many years, and these surveys will observe in less than ideal conditions. This paper describes a technique to implement a new strategy to directly measure variations of atmospheric transmittance at optical wavelengths and application of these measurements to calibration of ground-based observations. This strategy makes use of measurements of the spectra of a small catalog of bright "probe" stars as they progress across the sky and back-light the atmosphere. The signatures of optical absorption by different atmospheric constituents are recognized in these spectra by their characteristic dependences on wavelength and airmass. State-of-the-art models of atmospheric radiation transport and modern codes are used to accurately compute atmospheric extinction over a wide range of observing conditions. We present results of an observing campaign that demonstrate that correction for extinction due to molecular constituents and aerosols can be done with precisions of a few millimagnitudes with this technique. C1 [Burke, David L.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Axelrod, T.] Univ Arizona, Steward Observ, Tucson, AZ 85718 USA. [Blondin, Stephane] ESO, D-85748 Garching, Germany. [Blondin, Stephane] CNRS, IN2P3, CPPM, F-13288 Marseille 09, France. [Claver, Chuck; Saha, Abhijit] Natl Opt Astron Observ, Tucson, AZ 85718 USA. [Ivezic, Zeljko; Jones, Lynne] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Smith, Allyn] Austin Peay State Univ, Dept Phys & Astron, Clarksville, TN 37044 USA. [Smith, R. Chris] Cerro Tololo Interamer Observ, La Serena, Chile. [Stubbs, Christopher W.] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Burke, DL (reprint author), SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. EM daveb@slac.stanford.edu RI Stubbs, Christopher/C-2829-2012 OI Stubbs, Christopher/0000-0003-0347-1724 FU National Science Foundation [9 (AST-0551161), AST-0132798]; Department of Energy [DE-AC02-76SF00515, DE-AC02-98Ch10886, DE-FG02-91ER40, DE-FG02-91ER40677, W-7405-Eng-48] FX This work has been done as part of the design and development activity of the Large Synoptic Survey Telescope (LSST). The LSST is supported by the National Science Foundation under Scientific Program Order No. 9 (AST-0551161) through Cooperative Agreement AST-0132798, and under Department of Energy contracts DE-AC02-76SF00515, DE-AC02-98Ch10886, DE-FG02-91ER40, DE-FG02-91ER40677, and W-7405-Eng-48. Additional funding conies from private donations, in-kind support at Department of Energy laboratories and other LSSTC Institutional Members. NR 29 TC 23 Z9 23 U1 2 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2010 VL 720 IS 1 BP 811 EP 823 DI 10.1088/0004-637X/720/1/811 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 647DJ UT WOS:000281596000069 ER PT J AU Cranmer, SR Van Ballegooijen, AA AF Cranmer, Steven R. Van Ballegooijen, Adriaan A. TI CAN THE SOLAR WIND BE DRIVEN BY MAGNETIC RECONNECTION IN THE SUN'S MAGNETIC CARPET? SO ASTROPHYSICAL JOURNAL LA English DT Article DE magnetic fields; magnetohydrodynamics (MHD); plasmas; solar wind; Sun: corona; Sun: photosphere ID CORONAL MASS EJECTIONS; ELEMENTARY HEATING EVENTS; 2 FLUX SOURCES; QUIET SUN; ACTIVE REGIONS; TRANSITION REGION; MAGNETOHYDRODYNAMIC TURBULENCE; CHROMOSPHERIC NETWORK; PHOTOSPHERIC MOTIONS; HINODE OBSERVATIONS AB The physical processes that heat the solar corona and accelerate the solar wind remain unknown after many years of study. Some have suggested that the wind is driven by waves and turbulence in open magnetic flux tubes, and others have suggested that plasma is injected into the open tubes by magnetic reconnection with closed loops. In order to test the latter idea, we developed Monte Carlo simulations of the photospheric "magnetic carpet" and extrapolated the time-varying coronal field. These models were constructed for a range of different magnetic flux imbalance ratios. Completely balanced models represent quiet regions on the Sun and source regions of slow solar wind streams. Highly imbalanced models represent corona] holes and source regions of fast wind streams. The models agree with observed emergence rates, surface flux densities, and number distributions of magnetic elements. Despite having no imposed supergranular motions in the models, a realistic network of magnetic "funnels" appeared spontaneously. We computed the rate at which closed field lines open up (i.e., recycling times for open flux), and we estimated the energy flux released in reconnection events involving the opening up of closed flux tubes. For quiet regions and mixed-polarity coronal holes, these energy fluxes were found to be much lower than that which is required to accelerate the solar wind. For the most imbalanced coronal holes, the energy fluxes may be large enough to power the solar wind, but the recycling times are far longer than the time it takes the solar wind to accelerate into the low corona. Thus, it is unlikely that either the slow or fast solar wind is driven by reconnection and loop-opening processes in the magnetic carpet. C1 [Cranmer, Steven R.; Van Ballegooijen, Adriaan A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Cranmer, SR (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM scranmer@cfa.harvard.edu; avanballegooijen@cfa.harvard.edu OI van Ballegooijen, Adriaan/0000-0002-5622-3540 FU National Aeronautics and Space Administration (NASA) [NNX09AB27G] FX The authors gratefully acknowledge Ben Chandran, Phil Isenberg, Terry Gaetz, and the anonymous referee for valuable discussions. This work was supported by the National Aeronautics and Space Administration (NASA) under grant NNX09AB27G to the Smithsonian Astrophysical Observatory. The SOLIS data used in this paper are produced cooperatively by NSF/NSO and NASA/LWS. NR 161 TC 29 Z9 30 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 SEP 1 PY 2010 VL 720 IS 1 BP 824 EP 847 DI 10.1088/0004-637X/720/1/824 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 647DJ UT WOS:000281596000070 ER PT J AU Tullmann, R Plucinsky, PP Gaetz, TJ Slane, P Hughes, JP Harrus, I Pannuti, TG AF Tuellmann, R. Plucinsky, P. P. Gaetz, T. J. Slane, P. Hughes, J. P. Harrus, I. Pannuti, T. G. TI SEARCHING FOR THE PULSAR IN G18.95-1.1: DISCOVERY OF AN X-RAY POINT SOURCE AND ASSOCIATED SYNCHROTRON NEBULA WITH CHANDRA SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: supernova remnants; pulsars: general; X-rays: individual (G18.95-1.1) ID SUPERNOVA REMNANT; RADIO-SOURCE; H I; GALAXY; STARS AB Using the Chandra X-ray Observatory, we have pinpointed the location of a faint X-ray point source (CXOU J182913.1-125113) and an associated diffuse nebula in the composite supernova remnant (SNR) G18.95-1.1. These objects appear to be the long-sought pulsar and its wind nebula. The X-ray spectrum of the point source is best described by an absorbed power-law model with Gamma = 1.6 and an N(H) of similar to 1 x 10(22) cm(-2). This model predicts a relatively low unabsorbed X-ray luminosity of about L(X)(0.5-8.0 keV) similar or equal to 4.1 x 10(31) D(2)(2) erg s(-1), where D(2) is the distance in units of 2 kpc. The best-fit model of the diffuse nebula is a combination of thermal (kT = 0.48 keV) and non-thermal (1.4 <= Gamma <= 1.9) emission. The unabsorbed X-ray luminosity of L(X) similar or equal to 5.4 x 10(33) D(2)(2) erg s(-1) in the 0.5-8 keV energy band seems to be largely dominated by the thermal component from the SNR, providing 87% of L(X) in this band. No radio or X-ray pulsations have been reported for CXOU J182913.1-125113. If we assume an age of similar to 5300 yr for G18.95-1.1 and use the X-ray luminosity for the pulsar and the wind nebula together with the relationship between spin-down luminosity (via magnetic dipole radiation) and period, we estimate the pulsar's period to be P similar or equal to 0.4 s. Compared to other rotation-powered pulsars, a magnetic field of 2.2 x 10(13) G is implied by its location in the P-(P) over dot diagram, a value which is close to that of the quantum critical field. C1 [Tuellmann, R.; Plucinsky, P. P.; Gaetz, T. J.; Slane, P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hughes, J. P.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Harrus, I.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Pannuti, T. G.] Morehead State Univ, Ctr Space Sci, Morehead, KY 40351 USA. RP Tullmann, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rtuellmann@cfa.harvard.edu FU NASA [GO9-0081X] FX Support for this work was provided by NASA through Chandra Award Number GO9-0081X. NR 21 TC 2 Z9 2 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2010 VL 720 IS 1 BP 848 EP 852 DI 10.1088/0004-637X/720/1/848 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 647DJ UT WOS:000281596000071 ER PT J AU Gezari, S Rest, A Huber, ME Narayan, G Forster, K Neill, JD Martin, DC Valenti, S Smartt, SJ Chornock, R Berger, E Soderberg, AM Mattila, S Kankare, E Burgett, WS Chambers, KC Dombeck, T Grav, T Heasley, JN Hodapp, KW Jedicke, R Kaiser, N Kudritzki, R Luppino, G Lupton, RH Magnier, EA Monet, DG Morgan, JS Onaka, PM Price, PA Rhoads, PH Siegmund, WA Stubbs, CW Tonry, JL Wainscoat, RJ Waterson, MF Wynn-Williams, CG AF Gezari, S. Rest, A. Huber, M. E. Narayan, G. Forster, K. Neill, J. D. Martin, D. C. Valenti, S. Smartt, S. J. Chornock, R. Berger, E. Soderberg, A. M. Mattila, S. Kankare, E. Burgett, W. S. Chambers, K. C. Dombeck, T. Grav, T. Heasley, J. N. Hodapp, K. W. Jedicke, R. Kaiser, N. Kudritzki, R. Luppino, G. Lupton, R. H. Magnier, E. A. Monet, D. G. Morgan, J. S. Onaka, P. M. Price, P. A. Rhoads, P. H. Siegmund, W. A. Stubbs, C. W. Tonry, J. L. Wainscoat, R. J. Waterson, M. F. Wynn-Williams, C. G. TI GALEX AND PAN-STARRS1 DISCOVERY OF SN IIP 2010aq: THE FIRST FEW DAYS AFTER SHOCK BREAKOUT IN A RED SUPERGIANT STAR SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE supernovae: individual (SN 2010aq); surveys; ultraviolet: general ID CORE-COLLAPSE SUPERNOVAE; FORMING GALAXIES; P SUPERNOVAE; LIGHT CURVES; GRB-060218; SPECTROSCOPY; PROGENITORS; ABUNDANCES; EMISSION; PLATEAU AB We present the early UV and optical light curve of Type IIP supernova (SN) 2010aq at z = 0.0862, and compare it to analytical models for thermal emission following SN shock breakout in a red supergiant star. SN 2010aq was discovered in joint monitoring between the Galaxy Evolution Explorer (GALEX) Time Domain Survey (TDS) in the NUV and the Pan-STARRS1 Medium Deep Survey (PS1 MDS) in the g, r, i, and z bands. The GALEX and Pan-STARRS1 observations detect the SN less than 1 day after the shock breakout, measure a diluted blackbody temperature of 31,000 +/- 6000 K 1 day later, and follow the rise in the UV/optical light curve over the next 2 days caused by the expansion and cooling of the SN ejecta. The high signal-to-noise ratio of the simultaneous UV and optical photometry allows us to fit for a progenitor star radius of 700 +/- 200R(circle dot), the size of a red supergiant star. An excess in UV emission two weeks after shock breakout compared with SNe well fitted by model atmosphere-code synthetic spectra with solar metallicity is best explained by suppressed line blanketing due to a lower metallicity progenitor star in SN 2010aq. Continued monitoring of PS1 MDS fields by the GALEX TDS will increase the sample of early UV detections of Type II SNe by an order of magnitude and probe the diversity of SN progenitor star properties. C1 [Gezari, S.; Huber, M. E.; Grav, T.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Rest, A.; Narayan, G.; Stubbs, C. W.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Forster, K.; Neill, J. D.; Martin, D. C.] CALTECH, Pasadena, CA 91125 USA. [Valenti, S.; Smartt, S. J.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. [Chornock, R.; Berger, E.; Soderberg, A. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Mattila, S.; Kankare, E.] Univ Turku, Dept Phys & Astron, Tuorla Observ, FI-21500 Piikkio, Finland. [Mattila, S.] AlbaNova Univ Ctr, Dept Astron, Stockholm Observ, SE-10691 Stockholm, Sweden. [Kankare, E.] Nord Opt Telescope, E-38700 Santa Cruz De La Palma, Spain. [Burgett, W. S.; Chambers, K. C.; Dombeck, T.; Heasley, J. N.; Hodapp, K. W.; Jedicke, R.; Kaiser, N.; Kudritzki, R.; Luppino, G.; Magnier, E. A.; Morgan, J. S.; Onaka, P. M.; Price, P. A.; Rhoads, P. H.; Siegmund, W. A.; Tonry, J. L.; Wainscoat, R. J.; Waterson, M. F.; Wynn-Williams, C. G.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Lupton, R. H.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Monet, D. G.] USN Observ, Flagstaff Stn, Flagstaff, AZ 86001 USA. RP Gezari, S (reprint author), Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA. EM suvi@pha.jhu.edu RI Stubbs, Christopher/C-2829-2012; Waterson, Mark/B-7352-2013; OI Stubbs, Christopher/0000-0003-0347-1724; Waterson, Mark/0000-0002-0192-2686; Narayan, Gautham/0000-0001-6022-0484; Chambers, Kenneth /0000-0001-6965-7789 FU NASA through Space Telescope Science Institute [HST-HF-01219.01-A]; NASA [NAS 5-26555] FX S.G. thanks I. Rabinak and E. Nakar for kindly providing their models in the GALEX and PS1 filters, L. Dessart for helpful discussions, and the anonymous referee for useful comments. S. G. was supported by NASA through Hubble Fellowship grant HST-HF-01219.01-A awarded by the Space Telescope Science Institute, which is operated by AURA, Inc., for NASA, under contract NAS 5-26555. The PS1 Surveys have been made possible through the combinations of the Institute for Astronomy at 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, the Queen's University of Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Network, and the National Central University of Taiwan. We gratefully acknowledge NASA's support for construction, operation, and science analysis for the GALEX mission, developed in cooperation with CNES of France and the Korean MOST. NR 36 TC 25 Z9 25 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD SEP 1 PY 2010 VL 720 IS 1 BP L77 EP L81 DI 10.1088/2041-8205/720/1/L77 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 647HW UT WOS:000281610100016 ER PT J AU Gnedin, OY Brown, WR Geller, MJ Kenyon, SJ AF Gnedin, Oleg Y. Brown, Warren R. Geller, Margaret J. Kenyon, Scott J. TI THE MASS PROFILE OF THE GALAXY TO 80 kpc SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE Galaxy: formation; Galaxy: halo; Galaxy: kinematics and dynamics ID VELOCITY DISPERSION PROFILE; DIGITAL SKY SURVEY; DARK-MATTER HALOS; MILKY-WAY HALO; STELLAR MASS; STRIPE 82; CURVE; SUBSTRUCTURE; CONSTRAINTS; STARS AB The Hypervelocity Star Survey presents the currently largest sample of radial velocity measurements of halo stars out to 80 kpc. We apply spherical Jeans modeling to these data in order to derive the mass profile of the Galaxy. We restrict the analysis to distances larger than 25 kpc from the Galactic center, where the density profile of halo stars is well approximated by a single power law with logarithmic slope between -3.5 and -4.5. With this restriction, we also avoid the complication of modeling a flattened Galactic disk. In the range 25 kpc < r < 80 kpc, the radial velocity dispersion declines remarkably little; a robust measure of its logarithmic slope is between -0.05 and -0.1. The circular velocity profile also declines remarkably little with radius. The allowed range of V(c) (80 kpc) lies between 175 and 231 km s(-1), with the most likely value of 193 km s(-1). Compared with the value at the solar location, the Galactic circular velocity declines by less than 20% over an order of magnitude in radius. Such a flat profile requires a massive and extended dark matter halo. The mass enclosed within 80 kpc is 6.9(-1.2)(+3.0)x10(11) M(circle dot). Our sample of radial velocities is large enough that the biggest uncertainty in the mass is not statistical but systematic, dominated by the density slope and anisotropy of the tracer population. Further progress requires modeling observed data sets within realistic simulations of galaxy formation. C1 [Gnedin, Oleg Y.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Brown, Warren R.; Geller, Margaret J.; Kenyon, Scott J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Gnedin, OY (reprint author), Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. EM ognedin@umich.edu; wbrown@cfa.harvard.edu; mgeller@cfa.harvard.edu; skenyon@cfa.harvard.edu OI Kenyon, Scott/0000-0003-0214-609X; Gnedin, Oleg/0000-0001-9852-9954 FU NSF [AST-0708087] FX We thank Hans-Walter Rix for clarifying discussions and the organizers of the Sixth Harvard-Smithsonian Sackler Conference, where this work was completed. O.G. is supported in part by the NSF Grant AST-0708087. NR 21 TC 78 Z9 80 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD SEP 1 PY 2010 VL 720 IS 1 BP L108 EP L112 DI 10.1088/2041-8205/720/1/L108 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 647HW UT WOS:000281610100022 ER PT J AU Munoz-Jaramillo, A Nandy, D Martens, PCH Yeates, AR AF Munoz-Jaramillo, Andres Nandy, Dibyendu Martens, Petrus C. H. Yeates, Anthony R. TI A DOUBLE-RING ALGORITHM FOR MODELING SOLAR ACTIVE REGIONS: UNIFYING KINEMATIC DYNAMO MODELS AND SURFACE FLUX-TRANSPORT SIMULATIONS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE Sun: activity; Sun: dynamo; Sun: interior ID OPEN MAGNETIC-FLUX; MERIDIONAL FLOW; TORSIONAL OSCILLATIONS; DIFFERENTIAL ROTATION; FIELD; CYCLE; TACHOCLINE; EVOLUTION; CIRCULATION; CORONA AB The emergence of tilted bipolar active regions (ARs) and the dispersal of their flux, mediated via processes such as diffusion, differential rotation, and meridional circulation, is believed to be responsible for the reversal of the Sun's polar field. This process (commonly known as the Babcock-Leighton mechanism) is usually modeled as a near-surface, spatially distributed alpha-effect in kinematic mean-field dynamo models. However, this formulation leads to a relationship between polar field strength and meridional flow speed which is opposite to that suggested by physical insight and predicted by surface flux-transport simulations. With this in mind, we present an improved double-ring algorithm for modeling the Babcock-Leighton mechanism based on AR eruption, within the framework of an axisymmetric dynamo model. Using surface flux-transport simulations, we first show that an axisymmetric formulation-which is usually invoked in kinematic dynamo models-can reasonably approximate the surface flux dynamics. Finally, we demonstrate that our treatment of the Babcock-Leighton mechanism through double-ring eruption leads to an inverse relationship between polar field strength and meridional flow speed as expected, reconciling the discrepancy between surface flux-transport simulations and kinematic dynamo models. C1 [Munoz-Jaramillo, Andres; Martens, Petrus C. H.] Montana State Univ, Dept Phys, Bozeman, MT 59717 USA. [Nandy, Dibyendu] Indian Inst Sci Educ & Res, Dept Phys Sci, Mohampur 741252, W Bengal, India. [Martens, Petrus C. H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Yeates, Anthony R.] Univ Dundee, Div Math, Dundee DD1 4HN, Scotland. RP Munoz-Jaramillo, A (reprint author), Montana State Univ, Dept Phys, Bozeman, MT 59717 USA. EM munoz@solar.physics.montana.edu; dnandi@iiserkol.ac.in; martens@solar.physics.montana.edu; anthony@maths.dundee.ac.uk RI Yeates, Anthony/D-1338-2014; OI Yeates, Anthony/0000-0002-2728-4053; Munoz-Jaramillo, Andres/0000-0002-4716-0840 FU NASA [NNG05GE47G]; Government of India; UK STFC FX We thank Aad van Ballegooijen for useful discussions that were crucial for the development of the algorithm mentioned in Section 4. The computations required for this work were performed using the resources of Montana State University and the Harvard-Smithsonian Center for Astrophysics. We thank Keiji Yoshimura at MSU and Alisdair Davey and Henry (Trae) Winter at the CfA for much appreciated technical support. This research was funded by NASA Living With a Star grant NNG05GE47G and has made extensive use of NASA's Astrophysics Data System. D.N. acknowledges support from the Government of India through the Ramanujan Fellowship. A.R.Y. thanks the UK STFC for financial support. NR 27 TC 25 Z9 25 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD SEP 1 PY 2010 VL 720 IS 1 BP L20 EP L25 DI 10.1088/2041-8205/720/1/L20 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 647HW UT WOS:000281610100005 ER PT J AU Raghavan, D McAlister, HA Henry, TJ Latham, DW Marcy, GW Mason, BD Gies, DR White, RJ ten Brummelaar, TA AF Raghavan, Deepak McAlister, Harold A. Henry, Todd J. Latham, David W. Marcy, Geoffrey W. Mason, Brian D. Gies, Douglas R. White, Russel J. ten Brummelaar, Theo A. TI A SURVEY OF STELLAR FAMILIES: MULTIPLICITY OF SOLAR-TYPE STARS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE binaries: general; planetary systems; stars: solar-type; stars: statistics; surveys ID ALL-SKY SURVEY; BROWN DWARF DESERT; EXOPLANET HOST STARS; PROPER-MOTION STARS; SPECTROSCOPIC BINARY ORBITS; ICCD SPECKLE OBSERVATIONS; PHOTOELECTRIC RADIAL-VELOCITIES; LONG-PERIOD COMPANIONS; ADAPTIVE OPTICS SURVEY; RHO-CORONAE-BOREALIS AB We present the results of a comprehensive assessment of companions to solar-type stars. A sample of 454 stars, including the Sun, was selected from the Hipparcos catalog with pi > 40 mas, sigma(pi)/pi < 0.05, 0.5 <= B - V <= 1.0 (similar to F6-K3), and constrained by absolute magnitude and color to exclude evolved stars. These criteria are equivalent to selecting all dwarf and subdwarf stars within 25 pc with V-band flux between 0.1 and 10 times that of the Sun, giving us a physical basis for the term "solar-type." New observational aspects of this work include surveys for (1) very close companions with long-baseline interferometry at the Center for High Angular Resolution Astronomy Array, (2) close companions with speckle interferometry, and (3) wide proper-motion companions identified by blinking multi-epoch archival images. In addition, we include the results from extensive radial-velocity monitoring programs and evaluate companion information from various catalogs covering many different techniques. The results presented here include four new common proper-motion companions discovered by blinking archival images. Additionally, the spectroscopic data searched reveal five new stellar companions. Our synthesis of results from many methods and sources results in a thorough evaluation of stellar and brown dwarf companions to nearby Sun-like stars. The overall observed fractions of single, double, triple, and higher-order systems are 56% +/- 2%, 33% +/- 2%, 8% +/- 1%, and 3% +/- 1%, respectively, counting all confirmed stellar and brown dwarf companions. If all candidate, i.e., unconfirmed, companions identified are found to be real, the percentages would change to 54% +/- 2%, 34% +/- 2%, 9% +/- 2%, and 3% +/- 1%, respectively. Our completeness analysis indicates that only a few undiscovered companions remain in this well-studied sample, implying that the majority (54% +/- 2%) of solar-type stars are single, in contrast to the results of prior multiplicity studies. Our sample is large enough to enable a check of the multiplicity dependence on various physical parameters by analyzing appropriate subsamples. Bluer, more massive stars are seen as more likely to have companions than redder, less massive ones, consistent with the trend seen over the entire spectral range. Systems with larger interaction cross sections, i.e., those with more than two components or long orbital periods, are preferentially younger, suggesting that companions may be stripped over time by dynamical interactions. We confirm the planet-metallicity correlation (i.e., higher metallicity stars are more likely to host planets), but are unable to check it for brown dwarfs due to the paucity of such companions, implying that the brown dwarf desert extends over all separation regimes. We find no correlation between stellar companions and metallicity for B - V < 0.625, but among the redder subset, metal-poor stars ([Fe/H] < -0.3) are more likely to have companions with a 2.4 sigma significance. The orbital-period distribution of companions is unimodal and roughly log normal with a peak and median of about 300 years. The period-eccentricity relation shows the expected circularization for periods below 12 days, caused by tidal forces over the age of the Galaxy, followed by a roughly flat distribution. The mass-ratio distribution shows a preference for like-mass pairs, which occur more frequently in relatively close pairs. The fraction of planet hosts among single, binary, and multiple systems are statistically inditinguishable, suggesting that planets are as likely to form around single stars as they are around components of binary or multiple systems with sufficiently wide separations. This, along with the preference of long orbital periods among stellar systems, increases the space around stars conducive for planet formation, and perhaps life. C1 [Raghavan, Deepak; McAlister, Harold A.; Henry, Todd J.; Gies, Douglas R.; White, Russel J.] Georgia State Univ, Ctr High Angular Resolut Astron, Atlanta, GA 30302 USA. [Latham, David W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Marcy, Geoffrey W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Mason, Brian D.] USN Observ, Washington, DC 20392 USA. [ten Brummelaar, Theo A.] Mt Wilson Observ, CHARA Array, Mt Wilson, CA 91023 USA. RP Raghavan, D (reprint author), Georgia State Univ, Ctr High Angular Resolut Astron, POB 3969, Atlanta, GA 30302 USA. EM raghavan@chara.gsu.edu FU College of Arts and Sciences at Georgia State University; National Science Foundation [AST-0606958, AST-0908253]; U.S. Government [NAGW-2166]; National Aeronautics and Space Administration FX We thank Andy Boden, Bill Cochran, Richard Gray, Roger Griffin, Bill Hartkopf, Artie Hatzes, Elliott Horch, Mike Ireland, Hugh Jones, Davy Kirkpatrick, Dagny Looper, Dimitri Pourbaix, Sam Quinn, Andrei Tokovinin, and Nils Turner for their helpful insights on the nature of some specific systems, and in some instances, for making specific observations at our request and sharing their unpublished results. We acknowledge the insightful comments from an anonymous referee, which resulted in a more robust completion analysis of this survey, improving the confidence in our results. Research at the CHARA Array is supported by the College of Arts and Sciences at Georgia State University and by the National Science Foundation through NSF grants AST-0606958 and AST-0908253. Some of the photometric and spectroscopic observations reported here were carried out under the auspices of the SMARTS (Small and Moderate Aperture Research Telescope System) Consortium, which operates several small telescopes at CTIO. We thank RECONS group members, particularly, Jennifer Winters for reducing photometry data, and Wei-Chun Jao for his insights with some of the analysis. This research has made use of the SIMBAD literature database, operated at CDS, Strasbourg, France, NASA's Astrophysics Data System, and the Washington Double Star Catalog maintained by the U.S. Naval Observatory. This effort used multi-epoch images from the Digitized Sky Survey, which was produced at the Space Telescope Science Institute under U.S. Government grant NAGW-2166, and from the SuperCOSMOS Sky Survey. This publication also made use of data products from the Two Micron All Sky Survey (2MASS), which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. NR 215 TC 519 Z9 521 U1 2 U2 14 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD SEP PY 2010 VL 190 IS 1 BP 1 EP 42 DI 10.1088/0067-0049/190/1/1 PG 42 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 654WN UT WOS:000282201900001 ER PT J AU Kilic, M Leggett, SK Tremblay, PE von Hippel, T Bergeron, P Harris, HC Munn, JA Williams, KA Gates, E Farihi, J AF Kilic, Mukremin Leggett, S. K. Tremblay, P. -E. von Hippel, Ted Bergeron, P. Harris, Hugh C. Munn, Jeffrey A. Williams, Kurtis A. Gates, Evalyn Farihi, J. TI A DETAILED MODEL ATMOSPHERE ANALYSIS OF COOL WHITE DWARFS IN THE SLOAN DIGITAL SKY SURVEY SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE stars: atmospheres; stars: evolution; white dwarfs ID LUMINOSITY FUNCTION; PHOTOMETRIC ANALYSIS; GALACTIC DISK; HELIUM-ATMOSPHERE; DATA RELEASE; USNO-B; STARS; HALO; CATALOG; DEEP AB We present optical spectroscopy and near-infrared photometry of 126 cool white dwarfs (WDs) in the Sloan Digital Sky Survey (SDSS). Our sample includes high proper motion targets selected using the SDSS and USNOB astrometry and a dozen previously known ultracool WD candidates. Our optical spectroscopic observations demonstrate that a clean selection of large samples of cool WDs in the SDSS (and the SkyMapper, Pan-STARRS, and the Large Synoptic Survey Telescope data sets) is possible using a reduced proper motion diagram and a tangential velocity cut-off (depending on the proper motion accuracy) of 30 km s(-1). Our near-infrared observations reveal eight new stars with significant absorption. We use the optical and near-infrared photometry to perform a detailed model atmosphere analysis. More than 80% of the stars in our sample are consistent with either pure hydrogen or pure helium atmospheres. However, the eight stars with significant infrared absorption and the majority of the previously known ultracool WD candidates are best explained with mixed hydrogen and helium atmosphere models. The age distribution of our sample is consistent with a Galactic disk age of 8 Gyr. A few ultracool WDs may be as old as 12-13 Gyr, but our models have problems matching the spectral energy distributions of these objects. There are only two halo WD candidates in our sample. However, trigonometric parallax observations are required for accurate mass and age determinations and to confirm their membership in the halo. C1 [Kilic, Mukremin] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Leggett, S. K.] Gemini Observ, Hilo, HI 96720 USA. [Tremblay, P. -E.; Bergeron, P.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. [von Hippel, Ted] Siena Coll, Dept Phys, Loudonville, NY 12211 USA. [Harris, Hugh C.; Munn, Jeffrey A.] US Naval Observ, Flagstaff Stn, Flagstaff, AZ 86001 USA. [Williams, Kurtis A.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Gates, Evalyn] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Gates, Evalyn] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Farihi, J.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. RP Kilic, M (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM mkilic@cfa.harvard.edu OI Leggett, Sandy/0000-0002-3681-2989; Williams, Kurtis/0000-0002-1413-7679; Farihi, Jay/0000-0003-1748-602X FU NASA; Caltech; National Science Foundation [AST-0607480, AST-0602288]; NSERC Canada; FQRNT (Quebec); Gemini Observatory; National Aeronautics and Space Administration, Office of Space Science [NCC 5-538] FX We thank J. Liebert for many useful discussions, Andy Stephens for the derivation of the NIRI nonlinearity correction, and an anonymous referee for useful suggestions. Support for this work was provided by NASA through the Spitzer Space Telescope Fellowship Program, under an award from Caltech. This material is also based on work supported by the National Science Foundation under grants AST-0607480 and AST-0602288 and by the NSERC Canada and by the Fund FQRNT (Quebec). S.K.L.'s research is supported by Gemini Observatory. P. Bergeron is a Cottrell Scholar of Research Corporation for Science Advancement.; The Hobby-Eberly Telescope (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 Gemini observatory is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the Science and Technology Facilities Council (United Kingdom), theNational Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministerio da Ciencia e Tecnologia (Brazil), and Ministerio de Ciencia, Tecnologia e Innovacion Productiva (Argentina). The IRTF is operated by the University of Hawaii under Cooperative Agreement no. NCC 5-538 with the National Aeronautics and Space Administration, Office of Space Science, Planetary Astronomy Program. NR 63 TC 39 Z9 39 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD SEP PY 2010 VL 190 IS 1 BP 77 EP 99 DI 10.1088/0067-0049/190/1/77 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 654WN UT WOS:000282201900004 ER PT J AU Prasifka, JR Bradshaw, JD Boe, AA Lee, D Adamski, D Gray, ME AF Prasifka, Jarrad R. Bradshaw, Jeffrey D. Boe, Arvid A. Lee, DoKyoung Adamski, David Gray, Michael E. TI Symptoms, Distribution and Abundance of the Stem-Boring Caterpillar, Blastobasis repartella (Dietz), in Switchgrass SO BIOENERGY RESEARCH LA English DT Article DE Biofuel; Coleophoridae; Microlepidoptera; Tallgrass prairie; Yield ID BORER LEPIDOPTERA AB A potential pest of switchgrass, Panicum virgatum L., was first detected in South Dakota in 2004, where death of partially emerged leaves was noted in a small proportion of tillers. Similar "dead heart" symptoms were observed in switchgrass in Illinois during 2008 and adults of a stem-boring caterpillar were collected and identified as Blastobasis repartella (Dietz). In 2009, a survey of the central United States was used to estimate the distribution and abundance of this insect. In eight northern states, B. repartella was consistently found in both cultivated plots and natural stands of switchgrass. In four southern states, B. repartella was not detected. However, because symptoms are conspicuous for a short period of time, failure to collect stem-borers on one survey date for each southern location does not necessarily define the limit of distribution for B. repartella. Sampling in four northern states showed the proportion of tillers damaged by B. repartella ranged from 1.0-7.2%. Unlike some caterpillars that feed on native grasses, it appears that the egg-laying behavior of adult moths may preclude the use of prescribed burns as an effective method to suppress this stem-boring caterpillar. As a potential pest of switchgrass planted for biomass production, near-term research needs include refining the geographic distribution of B. repartella, quantifying potential losses of switchgrass biomass, and determining whether switchgrass may be bred for resistance this and other stem-boring insects. C1 [Prasifka, Jarrad R.] Univ Illinois, Energy Biosci Inst, Inst Genom Biol, Urbana, IL 61801 USA. [Adamski, David] Smithsonian Inst, Dept Entomol, Washington, DC 20560 USA. [Lee, DoKyoung; Gray, Michael E.] Univ Illinois, Dept Crop Sci, Urbana, IL 61801 USA. [Boe, Arvid A.] S Dakota State Univ, Dept Plant Sci, Brookings, SD 57007 USA. RP Prasifka, JR (reprint author), Univ Illinois, Energy Biosci Inst, Inst Genom Biol, Room 1117, Urbana, IL 61801 USA. EM prasifka@illinois.edu FU Energy Biosciences Institute FX Research funding was provided by the Energy Biosciences Institute. The authors wish to thank a number of people who assisted in locating and surveying field plots of switchgrass; Jerry Roitsch (Bristol, South Dakota), Jim Muir (Texas AgriLife Research), Twain Butler (The Samuel Roberts Noble Foundation), Mike Blazier (Lousiana State University Agricultural Center), Randy King (USDA-NRCS), Ken Moore (Iowa State University), Rob Mitchell (USDA-ARS), Mike Casler (USDA-ARS), John Leif (USDA-NRCS), and Yvonne Lawley (North Dakota State University). NR 13 TC 16 Z9 18 U1 1 U2 10 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1939-1234 J9 BIOENERG RES JI BioEnergy Res. PD SEP PY 2010 VL 3 IS 3 BP 238 EP 242 DI 10.1007/s12155-009-9064-8 PG 5 WC Energy & Fuels; Environmental Sciences SC Energy & Fuels; Environmental Sciences & Ecology GA 637HJ UT WOS:000280807800002 ER PT J AU Kennedy, CM Marra, PP AF Kennedy, Christina M. Marra, Peter P. TI Matrix mediates avian movements in tropical forested landscapes: Inference from experimental translocations SO BIOLOGICAL CONSERVATION LA English DT Article DE Neotropics; Caribbean; Tropical conservation; Connectivity; Dispersal; Homing ID GAP-CROSSING DECISIONS; HABITAT FRAGMENTATION; POSTFLEDGING PERIOD; POPULATION-DYNAMICS; BREEDING DISPERSAL; NONBREEDING SEASON; CORRIDOR USE; BIRDS; PATTERNS; JAMAICA AB Maintaining animal movement in fragmented landscapes depends upon the levels of connectivity among habitat patches, which in turn may depend upon the landscape matrix. Little is known about how the matrix affects dispersal abilities, in part because few experimental tests have been conducted. We experimentally translocated 142 migratory American Redstarts (Setophaga ruticilla) and resident Jamaican Todies (Todus todus) 0.6-4 km from their territories across landscapes fragmented by pen-urban development and bauxite mining and continuous forest. Redstarts returned more rapidly and with greater success than todies across all landscapes, with 95% of redstarts returning in an average of 2.5 days versus 60% of todies in >20 days. Return success was best predicted by translocation distance for redstarts and by sex for todies, with a trend of fewer birds returning when released in bauxite landscapes. Return time was strongly affected by matrix type, with both species returning more rapidly in a forested relative to a bauxite matrix and intermediately in a pen-urban matrix. These findings provide strong experimental evidence that land cover surrounding forested habitat influences species mobility. (C) 2010 Elsevier Ltd. All rights reserved. C1 [Kennedy, Christina M.] Univ Maryland, Dept Biol, College Pk, MD 20742 USA. [Marra, Peter P.] Migratory Bird Center, Smithsonian Conservat Biol Inst, Washington, DC 20008 USA. RP Kennedy, CM (reprint author), Univ Maryland, Dept Biol, 3221 Biol Psychol Bldg, College Pk, MD 20742 USA. EM cmk6@umd.edu; marrap@si.edu FU NASA; Fulbright; Washington Explorer's Club; Cosmos Club Foundation; University of Maryland; Smithsonian Institution (James Bond Trust); National Science Foundation FX We thank A. Hayes-Sutton for sharing her knowledge of the study region and for providing logistical field support; S. Franks (NASA Goddard Space Flight Center) for assistance in the object-based land cover classification; S. Schill (The Nature Conservancy) and O. Evelyn (Jamaica Forestry Department) for providing remote sensing imagery and GIS data; and Y. Strong and A. Donaldson (Jamaica National Environment and Planning Agency, NEPA) for granting in-country permits. This manuscript was improved with comments from M. Neel, W. Fagan, and D. Inouye (University of Maryland), T. Ricketts (World Wildlife Fund), and two anonymous reviewers. Fieldwork was directed by C. Kennedy with essential field assistance by C. Samuels, M. Podolsky, H. Davis, M. Beale, and M. White. All work was conducted under applicable permits and approved animal care/use protocols (University of Maryland IACUC protocol #R-06-83 to W.F.F. and C.M.K., Smithsonian National Zoological Park CRC-IACUC proposal #06-25 and Jamaica NEPA Ref. No. 18/27 to P.P.M. and C.M.K.). Research was made possible by the permission of many land owners to access their lands, including the Jamaica Forestry Department, Windalco, Alpart Mining Venture, and Jamalco bauxite mining companies, S&G Road Surfacing Materials Ltd., private farmers and Mandeville citizens. Funding was provided to C.M.K. by NASA Earth System Science Program (Doctoral Fellowship), Fulbright US Scholarship Program, Washington Explorer's Club, Cosmos Club Foundation, and the University of Maryland (Behavior, Ecology, Evolution, and Systematics Graduate Program and an Ann G. Wylie Dissertation Fellowship), and provided to P.P.M. and C.M.K. by the Smithsonian Institution (James Bond Trust) and to P.P.M. by the National Science Foundation. NR 63 TC 26 Z9 26 U1 5 U2 36 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0006-3207 J9 BIOL CONSERV JI Biol. Conserv. PD SEP PY 2010 VL 143 IS 9 BP 2136 EP 2145 DI 10.1016/j.biocon.2010.05.025 PG 10 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 641KW UT WOS:000281125400024 ER PT J AU Nyman, T Vikberg, V Smith, DR Boeve, JL AF Nyman, Tommi Vikberg, Veli Smith, David R. Boeve, Jean-Luc TI How common is ecological speciation in plant-feeding insects? A 'Higher' Nematinae perspective SO BMC EVOLUTIONARY BIOLOGY LA English DT Article ID HOST-PLANT; SYMPATRIC SPECIATION; INTERSPECIFIC INTERACTIONS; PHYLOGENETIC ANALYSIS; GEOGRAPHICAL PATTERN; SAWFLIES HYMENOPTERA; CONVERGENT EVOLUTION; PHYTOPHAGOUS INSECTS; MOLECULAR PHYLOGENY; BEETLES COLEOPTERA AB Background: Ecological speciation is a process in which a transiently resource-polymorphic species divides into two specialized sister lineages as a result of divergent selection pressures caused by the use of multiple niches or environments. Ecology-based speciation has been studied intensively in plant-feeding insects, in which both sympatric and allopatric shifts onto novel host plants could speed up diversification. However, while numerous examples of species pairs likely to have originated by resource shifts have been found, the overall importance of ecological speciation in relation to other, non-ecological speciation modes remains unknown. Here, we apply phylogenetic information on sawflies belonging to the 'Higher' Nematinae (Hymenoptera: Tenthredinidae) to infer the frequency of niche shifts in relation to speciation events. Results: Phylogenetic trees reconstructed on the basis of DNA sequence data show that the diversification of higher nematines has involved frequent shifts in larval feeding habits and in the use of plant taxa. However, the inferred number of resource shifts is considerably lower than the number of past speciation events, indicating that the majority of divergences have occurred by non-ecological allopatric speciation; based on a time-corrected analysis of sister species, we estimate that a maximum of c. 20% of lineage splits have been triggered by a change in resource use. In addition, we find that postspeciational changes in geographic distributions have led to broad sympatry in many species having identical host-plant ranges. Conclusion: Our analysis indicates that the importance of niche shifts for the diversification of herbivorous insects is at present implicitly and explicitly overestimated. In the case of the Higher Nematinae, employing a time correction for sister-species comparisons lowered the proportion of apparent ecology-based speciation events from c. 50-60% to around 20%, but such corrections are still lacking in other herbivore groups. The observed convergent but asynchronous shifting among dominant northern plant taxa in many higher-nematine clades, in combination with the broad overlaps in the geographic distributions of numerous nematine species occupying near-identical niches, indicates that host-plant shifts and herbivore community assembly are largely unconstrained by direct or indirect competition among species. More phylogeny-based studies on connections between niche diversification and speciation are needed across many insect taxa, especially in groups that exhibit few host shifts in relation to speciation. C1 [Nyman, Tommi] Univ Eastern Finland, Dept Biol, FI-80101 Joensuu, Finland. [Smith, David R.] ARS, Systemat Entomol Lab, PSI, USDA,Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA. [Boeve, Jean-Luc] Royal Belgian Inst Nat Sci, Dept Entomol, B-1000 Brussels, Belgium. RP Nyman, T (reprint author), Univ Eastern Finland, Dept Biol, POB 111, FI-80101 Joensuu, Finland. EM Tommi.Nyman@uef.fi FU European Community [BE-TAF-1462]; Academy of Finland [124695] FX We especially wish to thank colleagues who provided samples of higher-nematine species, many of which would otherwise have been impossible to obtain: Lauri Kapari, Heikki Roininen, Alexey Zinovjev, Ewald Altenhofer, Mikk Heidemaa, Marko Prous, Akira Yamagami, Matti Viitasaari, Herbert R. Jacobson, Valerie Caron, Urs Schaffner, Jens Rydell, Jeffrey Joy, and B. DeJonge. We also thank two anonymous referees for their constructive criticisms, which helped to improve the manuscript. The Centre of Scientific Computing in Helsinki and the Cyberinfrastructure for Phylogenetic Research (CIPRES) project in San Diego allocated computing resources for phylogenetic analyses on their servers. This research was initiated with support from the SYNTHESYS Project http://www.synthesys.info which is financed by the European Community Research Infrastructure Action under the FP6 "Structuring the European Research Area Programme" (project BE-TAF-1462), and the main part of the funding was provided by the Academy of Finland (project 124695 for TN). NR 95 TC 46 Z9 47 U1 2 U2 42 PU BIOMED CENTRAL LTD PI LONDON PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND SN 1471-2148 J9 BMC EVOL BIOL JI BMC Evol. Biol. PD SEP 1 PY 2010 VL 10 AR 266 DI 10.1186/1471-2148-10-266 PG 13 WC Evolutionary Biology; Genetics & Heredity SC Evolutionary Biology; Genetics & Heredity GA 661YI UT WOS:000282768900001 PM 20807452 ER PT J AU Saarela, JM Peterson, PM Elizondo, MSG Rosen, DJ AF Saarela, Jeffery M. Peterson, Paul M. Gonzalez Elizondo, M. Socorro Rosen, David J. TI Eleocharis cryptica (Cyperaceae), a dwarf new species from Durango, Mexico SO BRITTONIA LA English DT Article DE conservation; Eleocharis nigrescens; Sierra Madre Occidental; Tenuissimae ID INFRAGENERIC CLASSIFICATION; LIMNOCHLOA CYPERACEAE; NOMENCLATURE; TAXONOMY; FLORA AB Eleocharis cryptica (Cyperaceae), known from pine-oak forest in Durango, Mexico, is described and illustrated. It belongs to Eleocharis subg. Eleocharis ser. Tenuissimae and can be distinguished by its diminutive size, with culms 2-13 mm long (including spikelets 1.3-1.7 mm long), and the folliform prolongations of its upper sheaths. It is the smallest species of Eleocharis thus far known. C1 [Saarela, Jeffery M.] Canadian Museum Nat, Ottawa, ON K1P 6P4, Canada. [Peterson, Paul M.] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. [Gonzalez Elizondo, M. Socorro] IPN, CIIDIR, Unidad Durango, Durango 34220, Mexico. [Rosen, David J.] Texas A&M Univ, Dept Ecosyst Sci & Management, SM Tracy Herbarium, College Stn, TX 77843 USA. RP Saarela, JM (reprint author), Canadian Museum Nat, POB 3443,Stn D, Ottawa, ON K1P 6P4, Canada. EM jsaarela@mus-nature.ca FU Smithsonian Institutions Restricted Endowment fund; National Geographic Society Committee for Research and Exploration [8087-06]; Canadian Museum of Nature FX We thank Christopher S. Reid for field assistance, Julian Starr for helpful discussion, Alice Tangerini for preparing the illustration, and the constructive comments of two reviewers. Our field research was supported financially by the Smithsonian Institutions Restricted Endowment fund, the National Geographic Society Committee for Research and Exploration (grant number 8087-06) and the Canadian Museum of Nature. NR 47 TC 4 Z9 5 U1 0 U2 1 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0007-196X J9 BRITTONIA JI Brittonia PD SEP PY 2010 VL 62 IS 3 BP 233 EP 238 DI 10.1007/s12228-009-9111-y PG 6 WC Plant Sciences SC Plant Sciences GA 651BY UT WOS:000281900800007 ER PT J AU Stellaccio, AE AF Stellaccio, Anthony E. TI Asuurkeraamika SO CERAMICS-ART AND PERCEPTION LA English DT Article C1 [Stellaccio, Anthony E.] Smithsonian Inst, Natl Museum African Art, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU CERAMICS-ART & PERCEPTION PTY LTD PI SHERIDAN PA 23 N SCOTT ST, STE 16, SHERIDAN, WYOMING 82801 USA SN 1035-1841 J9 CERAMICS-ART PERCEPT JI Ceramics-Art Percept. PD SEP-NOV PY 2010 IS 81 BP 48 EP 51 PG 4 WC Art SC Art GA 643XQ UT WOS:000281334400012 ER PT J AU Liebherr, JK Casale, A Erwin, TL Ball, GE AF Liebherr, James K. Casale, Achille Erwin, Terry L. Ball, George E. TI ON THE PROVENANCE OF BOHEMAN'S "EUGENIES RESA" CARABIDAE (COLEOPTERA) ALLEGEDLY DESCRIBED FROM HAWAII SO COLEOPTERISTS BULLETIN LA English DT Article DE ground beetles; taxonomy; biogeography; distribution; new synonymies AB Five carabid beetle species described from the Hawaiian Islands, Polynesia-Calleida gracilis Gemminger and de Harold, 1868 (= Calleida amoenula Boheman, 1858), Calleida sanguinicollis Dejean, 1831 (= Calleida insularis Boheman, 1858), Lebia insularis Boheman, 1858, Selenophorus insularis Boheman, 1858, and Selenophorus picinus Boheman, 1858 are shown to be properly attributed to the American biogeographic region, with their type localities corrected to either Central America or Pacific South America. Two of the five names are newly synonymized: L. insularis Boheman = L. analis Dejean, 1825 (new synonymy), and S. insularis Boheman = S. chalcosomus Reiche, 1843 (new synonymy), Calleida gracilis is shown to be a member taxon of the janthina species-group of South America, most similar to Calleida tibialis Brulle, 1837. However, taxonomic uncertainty surrounding C. gracilis, C. tibialis, and an undescribed taxon precludes definitive species circumscription in this group, and C. gracilis is retained as a valid member of the janthina species-group pending future revision. Selenophorus picinus is placed as species incertae sedis within Selenophorus subgenus Gynandropus Dejean, alternately treated as the hylacis species-group. The biogeographical and ecological consequences obtained from removing these taxa from the Polynesian fauna include: 1) recognition of more natural biogeographical distributions for the genera Calleida Latreille and Dejean, Lebia Latreille, and Selenophorus Dejean; 2) elimination of all examples that could demonstrate extinction of a non-native carabid beetle species subsequent to its accidental introduction into the Hawaiian Islands. C1 [Liebherr, James K.] Cornell Univ, Dept Entomol, Ithaca, NY 14853 USA. [Casale, Achille] Univ Sassari, Dipartimento Zool & Genet Evoluzionist, I-07100 Sassari, Italy. [Erwin, Terry L.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. [Ball, George E.] Univ Alberta, Dept Biol Sci, Edmonton, AB T6G 2E3, Canada. RP Liebherr, JK (reprint author), Cornell Univ, Dept Entomol, Ithaca, NY 14853 USA. EM jkl5@cornell.edu; casale@uniss.it; erwint@si.edu; gball@ualberta.ca NR 38 TC 0 Z9 0 U1 1 U2 2 PU COLEOPTERISTS SOC PI ATHENS PA UNIV GEORGIA, 413 BIOLOGICAL SCIENCES BUILDING, ATHENS, GA 30602-2603 USA SN 0010-065X J9 COLEOPTS BULL JI Coleopt. Bull. PD SEP PY 2010 VL 64 IS 3 BP 221 EP 229 PG 9 WC Entomology SC Entomology GA 658XZ UT WOS:000282530000007 ER PT J AU Aiello, A Nunez, ED Stockwell, HP AF Aiello, Annette Dominguez Nunez, Edwin Stockwell, Henry P. TI NOTHING IS PERFECT: BIODEGRADABLE PACKING MATERIAL AS FOOD AND TRANSPORTATION FOR A MUSEUM PEST, LASIODERMA SERRICORNE (F.) (COLEOPTERA: ANOBIIDAE) SO COLEOPTERISTS BULLETIN LA English DT Editorial Material C1 [Aiello, Annette; Dominguez Nunez, Edwin; Stockwell, Henry P.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Aiello, A (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama. NR 5 TC 0 Z9 1 U1 3 U2 11 PU COLEOPTERISTS SOC PI ATHENS PA UNIV GEORGIA, 413 BIOLOGICAL SCIENCES BUILDING, ATHENS, GA 30602-2603 USA SN 0010-065X J9 COLEOPTS BULL JI Coleopt. Bull. PD SEP PY 2010 VL 64 IS 3 BP 256 EP 257 PG 2 WC Entomology SC Entomology GA 658XZ UT WOS:000282530000012 ER PT J AU Cusatti, UV Garay, AL Johnson, PJ AF Vargas Cusatti, Ursula Lanuza Garay, Alfredo Johnson, Paul J. TI NEW RECORDS OF PLATYCREPIDIUS COSTARICENSIS JOHNSON AND PLATYCREPIDIUS EBURATUS (CHAMPION) (COLEOPTERA: ELATERIDAE) IN PANAMA SO COLEOPTERISTS BULLETIN LA English DT Editorial Material C1 [Vargas Cusatti, Ursula] Univ Panama, Colon, Panama. [Lanuza Garay, Alfredo] Smithsonian Trop Res Inst, Punta Galeta Marine Lab, Colon, Panama. [Johnson, Paul J.] S Dakota State Univ, Brookings, SD 57007 USA. RP Cusatti, UV (reprint author), Univ Panama, Colon, Panama. EM ucusatti@hotmail.com; lanuzaa@si.edu; paul.johnson@sdstate.edu NR 6 TC 1 Z9 1 U1 0 U2 0 PU COLEOPTERISTS SOC PI ATHENS PA UNIV GEORGIA, 413 BIOLOGICAL SCIENCES BUILDING, ATHENS, GA 30602-2603 USA SN 0010-065X J9 COLEOPTS BULL JI Coleopt. Bull. PD SEP PY 2010 VL 64 IS 3 BP 285 EP 286 PG 2 WC Entomology SC Entomology GA 658XZ UT WOS:000282530000018 ER PT J AU Clark, MA Babich, R Barros, K Brower, RC Rebbi, C AF Clark, M. A. Babich, R. Barros, K. Brower, R. C. Rebbi, C. TI Solving lattice QCD systems of equations using mixed precision solvers on GPUs SO COMPUTER PHYSICS COMMUNICATIONS LA English DT Article DE CUDA; GPGPU; CPU; Lattice QCD; Mixed precision AB Modern graphics hardware is designed for highly parallel numerical tasks and promises significant cost and performance benefits for many scientific applications. One such application is lattice quantum chromodynamics (lattice QCD), where the main computational challenge is to efficiently solve the discretizecl Dirac equation in the presence of an SU(3) gauge field. Using NVIDIA's CUDA platform we have implemented a Wilson-Dirac sparse matrix-vector product that performs at up to 40, 135 and 212 Gflops for double, single and half precision respectively on NVIDIA's GeForce GTX 280 CPU. We have developed a new mixed precision approach for Krylov solvers using reliable updates which allows for full double precision accuracy while using only single or half precision arithmetic for the bulk of the computation. The resulting BiCGstab and CG solvers run in excess of 100 Gflops and, in terms of iterations until convergence, perform better than the usual defect-correction approach for mixed precision. (C) 2010 Elsevier B.V. All rights reserved. C1 [Clark, M. A.] Harvard Univ, Sch Engn & Appl Sci, Initiat Innovat Comp, Cambridge, MA 02138 USA. [Clark, M. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Babich, R.; Brower, R. C.; Rebbi, C.] Boston Univ, Ctr Computat Sci, Boston, MA 02215 USA. [Babich, R.; Brower, R. C.; Rebbi, C.] Boston Univ, Dept Phys, Boston, MA 02215 USA. [Barros, K.] Northwestern Univ, Dept Engn Sci & Appl Math, Evanston, IL 60208 USA. [Barros, K.] Northwestern Univ, Dept Mat Sci & Engn, Evanston, IL 60208 USA. RP Clark, MA (reprint author), Harvard Univ, Sch Engn & Appl Sci, Initiat Innovat Comp, 29 Oxford St, Cambridge, MA 02138 USA. EM mikec@seas.harvard.edu FU US DOE [DE-FG02-91ER40676, DE-FC02-06ER41440]; NSF [DGE-0221680, PHY-0427646, PHY-0835713, OCI-0749300] FX This work was supported in part by US DOE grants DE-FG02-91ER40676 and DE-FC02-06ER41440 and NSF grants DGE-0221680, PHY-0427646, PHY-0835713 and OCI-0749300. We would like to thank D. Luebke of NVIDIA for generous hardware donations and G. Shi for improving the numerical stability of the half precision 8 parameter reconstruction. NR 20 TC 85 Z9 85 U1 0 U2 12 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0010-4655 J9 COMPUT PHYS COMMUN JI Comput. Phys. Commun. PD SEP PY 2010 VL 181 IS 9 BP 1517 EP 1528 DI 10.1016/j.cpc.2010.05.002 PG 12 WC Computer Science, Interdisciplinary Applications; Physics, Mathematical SC Computer Science; Physics GA 638DX UT WOS:000280873500005 ER PT J AU Newsome, SD Bentall, GB Tinker, MT Oftedal, OT Ralls, K Estes, JA Fogel, ML AF Newsome, Seth D. Bentall, Gena B. Tinker, M. Tim Oftedal, Olav T. Ralls, Katherine Estes, James A. Fogel, Marilyn L. TI Variation in delta C-13 and delta N-15 diet-vibrissae trophic discrimination factors in a wild population of California sea otters SO ECOLOGICAL APPLICATIONS LA English DT Article DE Enhydra lutris nereis; San Nicolas Island, California, USA; sea otter; stable isotopes; trophic discrimination factors (TDFs); vibrissae ID ISOTOPE MIXING MODELS; FOOD WEB STRUCTURE; STABLE-ISOTOPES; NUTRITIONAL STRESS; NITROGEN-BALANCE; FORAGING ECOLOGY; CARBON ISOTOPES; AMINO-ACIDS; ENRICHMENT; FRACTIONATION AB The ability to quantify dietary inputs using stable isotope data depends on accurate estimates of isotopic differences between a consumer (c) and its diet (d), commonly referred to as trophic discrimination factors (TDFs) and denoted by Delta(c-d). At present, TDFs are available for only a few mammals and are usually derived in captive settings. The magnitude of TDFs and the degree to which they vary in wild populations is unknown. We determined delta C-13 and delta N-15 TDFs for vibrissae (i.e., whiskers), a tissue that is rapidly becoming an informative isotopic substrate for ecologists, of a wild population of sea otters for which individual diet has been quantified through extensive observational study. This is one of the very few studies that report TDFs for free-living wild animals feeding on natural diets. Trophic discrimination factors of 2.2 parts per thousand +/- 0.7 parts per thousand for delta C-13 and 3.5 parts per thousand +/- 0.6 parts per thousand for delta N-15 (mean +/- SD) were similar to those reported for captive carnivores, and variation in individual delta C-13 TDFs was negatively but significantly related to sea urchin consumption. This pattern may relate to the lipid-rich diet consumed by most sea otters in this population and suggests that it may not be appropriate to lipid-extract prey samples when using the isotopic composition of keratinaceous tissues to examine diet in consumers that frequently consume lipid-rich foods, such as many marine mammals and seabirds. We suggest that inherent variation in TDFs should be included in isotopically based estimates of trophic level, food chain length, and mixing models used to quantify dietary inputs in wild populations; this practice will further define the capabilities and limitations of isotopic approaches in ecological studies. C1 [Newsome, Seth D.; Fogel, Marilyn L.] Carnegie Inst Washington, Geophys Lab, Washington, DC 20015 USA. [Bentall, Gena B.] Monterey Bay Aquarium, Sea Otter Res & Conservat, Monterey, CA 93940 USA. [Tinker, M. Tim; Estes, James A.] Univ Calif Santa Cruz, Ctr Ocean Hlth, Long Marine Lab, Santa Cruz, CA 95060 USA. [Oftedal, Olav T.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Ralls, Katherine] Smithsonian Inst, Natl Zool Pk, Washington, DC 20008 USA. RP Newsome, SD (reprint author), Univ Wyoming, Dept Zool & Physiol, 1000 E Univ Ave,Dept 3166, Laramie, WY 82071 USA. EM snewsome@uwyo.edu RI Tinker, Martin/F-1277-2011 FU Monterey Bay National Marine Sanctuary Foundation; U.S. Marine Mammal Commission; National Science Foundation [ATM-0502491]; Carnegie Institution of Washington; W. M. Keck Foundation [072000] FX Thanks to the Monterey Bay National Marine Sanctuary Foundation and the U.S. Marine Mammal Commission for funding the collection and processing of prey samples. We thank E. Snyder, C. Mancuso, W. Wurzel, E. Heil, and R. Harley for laboratory assistance; A. Green, M. Kenner, K. Miles, and J. Bodkin for assistance in prey collection; and K. Fox-Dobbs, D. H. Monson, A. C. Jakle, B. Fry, and C. Martinez del Rio for constructive reviews. We thank A. Green for obtaining the necessary California Fish and Game permit for marine invertebrate collection and the U. S. Navy for permission to conduct research on San Nicolas Island. S. D. Newsome was partially funded by the National Science Foundation (ATM-0502491), Carnegie Institution of Washington, and the W. M. Keck Foundation (072000). NR 42 TC 50 Z9 50 U1 8 U2 43 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 1051-0761 J9 ECOL APPL JI Ecol. Appl. PD SEP PY 2010 VL 20 IS 6 BP 1744 EP 1752 DI 10.1890/09-1502.1 PG 9 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA 643EN UT WOS:000281278500020 PM 20945772 ER PT J AU Mangan, SA Herre, EA Bever, JD AF Mangan, Scott A. Herre, Edward A. Bever, James D. TI Specificity between Neotropical tree seedlings and their fungal mutualists leads to plant-soil feedback SO ECOLOGY LA English DT Article DE arbuscular mycorrhizal fungi (AMF); Barro Colorado Island, Panama; belowground interactions; Glomus spp.; light level; plant-fungal interactions; plant-soil feedback; specificity; tropical forest ID ARBUSCULAR MYCORRHIZAL FUNGI; TROPICAL FOREST; NEGATIVE FEEDBACK; SPATIAL-PATTERNS; COMMUNITY STRUCTURE; MAINTAIN DIVERSITY; LIGHT-INTENSITY; GROWTH; PATHOGENS; COLONIZATION AB A growing body of evidence obtained largely from temperate grassland studies suggests that feedbacks occurring between plants and their associated soil biota are important to plant community assemblage. However, few studies have examined the importance of soil organisms in driving plant-soil feedbacks in forested systems. In a tropical forest in central Panama, we examined whether interactions between tree seedlings and their associated arbuscular mycorrhizal fungi (AMF) lead to plant-soil feedback. Specifically, do tropical seedlings modify their own AMF communities in a manner that either favors or inhibits the next cohort of conspecific seedlings (i.e., positive or negative feedback, respectively)? Seedlings of two shade-tolerant tree species (Eugenia nesiotica, Virola surinamensis) and two pioneer tree species (Luehea seemannii, Apeiba aspera) were grown in pots containing identical AMF communities composed of equal amounts of inoculum of six co-occurring AMF species. The different AMF-host combinations were all exposed to two light levels. Under low light (2% PAR), only two of the six AMF species sporulated, and we found that host identity did not influence composition of AMF spore communities. However, relative abundances of three of the four AMF species that produced spores were influenced by host identity when grown under high light (20% PAR). Furthermore, spores of one of the AMF species, Glomus geosporum, were common in soils of Luehea and Eugenia but absent in soils of Apeiba and Virola. We then conducted a reciprocal experiment to test whether AMF communities previously modified by Luehea and Apeiba differentially affected the growth of conspecific and heterospecific seedlings. Luehea seedling growth did not differ between soils containing AMF communities modified by Luehea and Apeiba. However, Apeiba seedlings were significantly larger when grown with Apeiba-modified AMF communities, as compared to Apeiba seedlings grown with Luehea-modifed AMF communities. Our experiments suggest that interactions between tropical trees and their associated AMF are species-specific and that these interactions may shape both tree and AMF communities through plant-soil feedback. C1 [Mangan, Scott A.; Bever, James D.] Indiana Univ, Dept Biol, Bloomington, IN 47405 USA. [Mangan, Scott A.; Herre, Edward A.] Smithsonian Trop Res Inst, Dpo, AA 34002 USA. RP Mangan, SA (reprint author), Indiana Univ, Dept Biol, Bloomington, IN 47405 USA. EM smangan37@gmail.com FU Smithsonian Tropical Research Institute (STRI); National Science Foundation [DIGG-0308779, DEB-0049080, DEB-0616891]; Indiana University; American Mammalogy Society; Sigma Xi FX We are indebted to Dora Alvarez, Camila Pizano, Charlotte Jander, Andrea Vincent, and Robert Horan for their assistance. We thank two anonymous reviewers for improving this manuscript. This work would not have been possible without the logistical support and funding provided by the Smithsonian Tropical Research Institute (STRI predoctoral fellowship to S. A. Mangan and a soil initiative grant to E. A. Herre). The National Science Foundation provided grant DIGG-0308779 to S. A. Mangan and James D. Bever, and grants DEB-0049080 and DEB-0616891 to James D. Bever. Funding was also provided by Indiana University, Sigma Xi, and the American Mammalogy Society to S. A. Mangan. NR 45 TC 27 Z9 32 U1 5 U2 100 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 0012-9658 J9 ECOLOGY JI Ecology PD SEP PY 2010 VL 91 IS 9 BP 2594 EP 2603 DI 10.1890/09-0396.1 PG 10 WC Ecology SC Environmental Sciences & Ecology GA 648MO UT WOS:000281698400016 PM 20957954 ER PT J AU Poorter, L Kitajima, K Mercado, P Chubina, J Melgar, I Prins, HHT AF Poorter, Lourens Kitajima, Kaoru Mercado, Pablo Chubina, Jose Melgar, Israel Prins, Herbert H. T. TI Resprouting as a persistence strategy of tropical forest trees: relations with carbohydrate storage and shade tolerance SO ECOLOGY LA English DT Article DE Bolivia; disturbance; dry forest; growth-survival trade-off; leaf size; resprouting; shade tolerance; total nonstructural carbohydrates (NSC); tropical rain forest; wood density ID LIFE-HISTORY VARIATION; RAIN-FOREST; DRY FOREST; INTERSPECIFIC VARIATION; LIGHT REQUIREMENTS; FUNCTIONAL TRAITS; SEEDLING SURVIVAL; LEAF TRAITS; GROWTH; ALLOCATION AB Resprouting is an important persistence strategy for woody species and represents a dominant pathway of regeneration in many plant communities, with potentially large consequences for vegetation dynamics, community composition, and species coexistence. Most of our knowledge of resprouting strategies comes from fire-prone systems, but this cannot be readily applied to other systems where disturbances are less intense. In this study we evaluated sapling responses to stem snapping for 49 moist-forest species and 36 dry-forest species from two Bolivian tropical forests. To this end we compared in a field experiment the survival and height growth of clipped and control saplings for a two-year period, and related this to the shade tolerance, carbohydrate reserves, and the morphological traits (wood density, leaf size) of the species. Nearly all saplings resprouted readily after stem damage, although dry-forest species realized, on average, a better survival and growth after stem damage compared to moist-forest species. Shade-tolerant species were better at resprouting than light-demanding species in moist forest. This resprouting ability is an important prerequisite for successful regeneration in the shaded understory, where saplings frequently suffer damage from falling debris. Survival after stem damage was, surprisingly, only modestly related to stem reserves, and much more strongly related to wood density, possibly because a high wood density enables plants to resist fungi and pathogens and to reduce stem decay. Correlations between sapling performance and functional traits were similar for the two forest types, and for phylogenetically independent contrasts and for cross-species analyses. The consistency of these results suggests that tropical forest species face similar trade-offs in different sites and converge on similar sets of solutions. A high resprouting ability, as well as investments in stem defense and storage reserves, form part of a suite of co-evolved traits that underlies the growth-survival trade-off, and contributes to light gradient partitioning and species coexistence. These links with shade tolerance are important in the moist evergreen forest, which casts a deep, more persistent shade, but tend to diminish in dry deciduous forest where light is a less limiting resource. C1 [Poorter, Lourens] Wageningen Univ, Ctr Ecosyst Studies, Forest Ecol & Forest Management Grp, NL-6700 AA Wageningen, Netherlands. [Poorter, Lourens; Mercado, Pablo; Chubina, Jose; Melgar, Israel] IBIF, Santa Cruz, Bolivia. [Poorter, Lourens; Prins, Herbert H. T.] Wageningen Univ, Ctr Ecosyst Studies, Resource Ecol Grp, NL-6700 AA Wageningen, Netherlands. [Kitajima, Kaoru] Univ Florida, Dept Bot, Gainesville, FL 32611 USA. [Kitajima, Kaoru] Smithsonian Trop Res Inst, Balboa, Panama. RP Poorter, L (reprint author), Wageningen Univ, Ctr Ecosyst Studies, Forest Ecol & Forest Management Grp, POB 47, NL-6700 AA Wageningen, Netherlands. EM lourens.poorter@wur.nl RI Kitajima, Kaoru/E-8877-2012 FU BOLFOR1 forest management; Netherlands Organisation of Scientific Research [863.02.007]; Wageningen Graduate School Production Ecology and Resource Conservation FX We thank staff and personnel of the Instituto Boliviano de Investigacion Forestal (IBIF) for logistical support. This research would not have been possible without the excellent help of many tree-spotters: Victor Hugo Hurtado, Carmelo Flores, Angel Subirana, Juan Alvarez, and Juan Carlos Alvarez. We thank Zhi-Quan Cai and two anonymous reviewers for their very helpful comments on the manuscript, Naomi Renelus for carbohydrate analysis, and last but not least, serebo, momoqui, negrillo tropero, and all the others who suffered along in this experiment. This research was funded by grants from the BOLFOR1 forest management project, The Netherlands Organisation of Scientific Research (Veni grant 863.02.007), and the Wageningen Graduate School Production Ecology and Resource Conservation. NR 66 TC 41 Z9 44 U1 9 U2 70 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 0012-9658 J9 ECOLOGY JI Ecology PD SEP PY 2010 VL 91 IS 9 BP 2613 EP 2627 DI 10.1890/09-0862.1 PG 15 WC Ecology SC Environmental Sciences & Ecology GA 648MO UT WOS:000281698400018 PM 20957956 ER PT J AU Launius, RD AF Launius, Roger D. TI Can we colonize the solar system? Human biology and survival in the extreme space environment SO ENDEAVOUR LA English DT Article AB Throughout the history of the space age the dominant vision for the future has been great spaceships plying the solar system, and perhaps beyond, moving living beings from one planet to another. Spacesuited astronauts would carry out exploration, colonization, and settlement as part of a relentlessly forward looking movement of humanity beyond Earth. As time has progressed this image has not changed appreciably even as the full magnitude of the challenges it represents have become more and more apparent. This essay explores the issues associated with the human movement beyond Earth and raises questions about whether humanity will ever be able to survive in the extreme environment of space and the other bodies of the solar system. This paper deals with important historical episodes as well as wider conceptual issues about life in space. Two models of expansion beyond Earth are discussed: (1) the movement of microbes and other types of life on Earth that can survive the space environment and (2) the modification of humans into cyborgs for greater capability to survive in the extreme environments encountered beyond this planet. C1 Natl Air & Space Museum, Smithsonian Inst, Washington, DC 20013 USA. RP Launius, RD (reprint author), Natl Air & Space Museum, Smithsonian Inst, POB 37012,NASM Room 3556,MRC 311, Washington, DC 20013 USA. EM launiusr@si.edu OI Launius, Roger/0000-0003-1633-1253 FU NASA FX One strategy for resolving this problem was offered by life scientists Manfred E. Clynes and Nathan S. Kline in their seminal 1960 article, 'Cyborgs and Space.' Reporting on research funded by NASA, this article set forth an agenda that challenged the dominant paradigm of human space exploration recreating Earth's environment beyond this planet. Clynes and Kline suggested at the very beginning of the space age that it made more sense to change humans through biological and technological alteration so as to make them better able to survive the existing conditions of space. NR 51 TC 5 Z9 6 U1 2 U2 21 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0160-9327 J9 ENDEAVOUR JI Endeavour PD SEP PY 2010 VL 34 IS 3 BP 122 EP 129 DI 10.1016/j.endeavour.2010.07.001 PG 8 WC History & Philosophy Of Science; Multidisciplinary Sciences SC History & Philosophy of Science; Science & Technology - Other Topics GA 659JV UT WOS:000282563700006 PM 20692704 ER PT J AU Krivosheina, M Mathis, WN AF Krivosheina, Marina Mathis, Wayne N. TI A REVIEW OF THE SHORE-FLY GENUS AXYSTA HALIDAY (DIPTERA: EPHYDRIDAE) WITH DESCRIPTION OF NEW SPECIES FROM AUSTRALIA, INDIA, AND THAILAND SO ENTOMOLOGICAL NEWS LA English DT Review DE Diptera; Ephydridae; Axysta; new species; Australia; India; Thailand AB Axysta austra sp. n. from Australia, A. indica sp. n. from India, and A. nikita sp. n. from Thailand are described. The synonymy of A. americana Clausen with A. nigrifacies (Miyagi) is proposed. The genus Axysta is recorded from the Australasian and Oriental Regions for the first time. Keys to genera in Hyadinini and species of Axysta are provided, as are illustrations of all species. C1 [Krivosheina, Marina] Inst Ecol & Evolut, Moscow 119071, Russia. [Mathis, Wayne N.] Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA. RP Krivosheina, M (reprint author), Inst Ecol & Evolut, 33 Leninsky Prospect, Moscow 119071, Russia. EM dipteramarina@rambler.ru; mathisw@si.edu NR 41 TC 0 Z9 0 U1 0 U2 0 PU AMER ENTOMOL SOC PI PHILADELPHIA PA 1900 BENJ FRANKLIN PARKWAY, PHILADELPHIA, PA 19103-1195 USA SN 0013-872X J9 ENTOMOL NEWS JI Entomol. News PD SEP-OCT PY 2010 VL 121 IS 4 BP 369 EP 390 PG 22 WC Entomology SC Entomology GA 850JU UT WOS:000297191700012 ER PT J AU Chen, DY Yang, HT Zu, XT AF Chen, Deyou Yang, Haitang Zu, Xiaotao TI Area spectra of near extremal black holes SO EUROPEAN PHYSICAL JOURNAL C LA English DT Article ID QUASI-NORMAL MODES; KERR AB Motivated by Maggiore's new interpretation of quasinormal modes, we investigate area spectra of a near extremal Schwarzschild-de Sitter black hole and a higher-dimensional near extremal Reissner-Nordstrom-de Sitter black hole. The result shows that the area spectra are equally spaced and irrelevant to the parameters of the black holes. C1 [Chen, Deyou; Yang, Haitang; Zu, Xiaotao] Univ Elect Sci & Technol China, Sch Phys Elect, Chengdu 610054, Sichuan, Peoples R China. [Chen, Deyou] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Chen, DY (reprint author), Univ Elect Sci & Technol China, Sch Phys Elect, Chengdu 610054, Sichuan, Peoples R China. EM deyouchen@uestc.edu.cn; hyanga@uestc.edu.cn FU NSFC [10705008]; NCET FX This work is supported in part by NSFC (Grant No. 10705008) and NCET. NR 39 TC 28 Z9 28 U1 0 U2 2 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1434-6044 J9 EUR PHYS J C JI Eur. Phys. J. C PD SEP PY 2010 VL 69 IS 1-2 BP 289 EP 292 DI 10.1140/epjc/s10052-010-1380-9 PG 4 WC Physics, Particles & Fields SC Physics GA 652FK UT WOS:000281987700025 ER PT J AU Bourke, MC Lancaster, N Fenton, LK Parteli, EJR Zimbelman, JR Radebaugh, J AF Bourke, Mary C. Lancaster, Nick Fenton, Lori K. Parteli, Eric J. R. Zimbelman, James R. Radebaugh, Jani TI Extraterrestrial dunes: An introduction to the special issue on planetary dune systems SO GEOMORPHOLOGY LA English DT Article DE Aeolian; Dune; Mars; Venus; Titan; Earth ID NORTH POLAR-REGION; OPTICALLY STIMULATED LUMINESCENCE; DIRECTIONALLY VARYING FLOWS; GENERAL-CIRCULATION MODEL; TRANSVERSE AEOLIAN RIDGES; MARTIAN ANALOG MATERIALS; INNER SOLAR-SYSTEM; SAND DUNES; LONGITUDINAL DUNES; LAYERED DEPOSITS AB Aeolian dune fields have been described on Earth, Mars, Venus and Titan. The plethora of data returned from recent planetary missions has enabled a new era in planetary geomorphic studies. Much of our understanding of planetary dune systems comes from the application of Earth analogs, wind tunnel experiments and modeling studies. Despite the range of atmospheric pressures, composition and gravity, many of the dune forms on extraterrestrial surfaces are similar to those on Earth, although some have notable differences in bedform scale and composition. As an introduction to the special issue on planetary dune systems this paper summarizes the current state of knowledge of planetary dune studies and highlights outstanding questions that require further investigation. (C) 2010 Elsevier B.V. All rights reserved. C1 [Bourke, Mary C.] PSI, Tucson, AZ 85719 USA. [Bourke, Mary C.] Univ Oxford, Sch Geog & Environm, Oxford OX1 3QY, England. [Lancaster, Nick] Desert Res Inst, Reno, NV 89512 USA. [Fenton, Lori K.] NASA, Ames Res Ctr, Carl Sagan Ctr, Moffett Field, CA 94035 USA. [Parteli, Eric J. R.] Univ Fed Ceara, Dept Fis, BR-60455900 Fortaleza, Ceara, Brazil. [Zimbelman, James R.] Smithsonian Inst, Natl Air & Space Museum, MRC 315, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. [Radebaugh, Jani] Brigham Young Univ, Dept Geol Sci, Provo, UT 84602 USA. RP Bourke, MC (reprint author), PSI, 1700 E Ft Lowell 106, Tucson, AZ 85719 USA. EM mbourke@psi.edu RI Parteli, Eric/K-7085-2014; Bourke, Mary/I-4387-2012; UFC, DF/E-1564-2017; Universidade Federal do Ceara, Physics Department/J-4630-2016 OI Bourke, Mary/0000-0002-0424-0322; Universidade Federal do Ceara, Physics Department/0000-0002-9247-6780 NR 202 TC 47 Z9 48 U1 8 U2 28 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0169-555X J9 GEOMORPHOLOGY JI Geomorphology PD SEP 1 PY 2010 VL 121 IS 1-2 SI SI BP 1 EP 14 DI 10.1016/j.geomorph.2010.04.007 PG 14 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA 636AH UT WOS:000280699300001 ER PT J AU Zimbelman, JR AF Zimbelman, James R. TI Transverse Aeolian Ridges on Mars: First results from HiRISE images SO GEOMORPHOLOGY LA English DT Article DE Sand; Dune; Ripple; Granule ripple; Topography; Transverse dune ID SAND DUNES; GUSEV CRATER; AIR-FLOW; WIND; MORPHOLOGY; RIPPLES; SIMULATION; RESOLUTION; SALTATION; TRANSPORT AB Three images obtained by the High Resolution Imaging Science Experiment (HiRISE) were analyzed for the information they could provide regarding Transverse Aeolian Ridges (TARS) on Mars. TARs from five locations in a HiRISE image of the floor of Ius Chasma show remarkably symmetric (cross-sectional) profiles, with average slopes for the entire feature of similar to 15 degrees; these results apply to TARs that span an order of magnitude in wavelength and a factor of 6 in height. A HiRISE image of Gamboa impact crater in the northern lowlands shows low albedo sand patches <2 m high that are covered with sand ripples, surrounded by larger TAR-like ripples that are very similar in profile to surveyed granule ripples on Earth. TARS in a HiRISE image from Terra Sirenum, in the cratered southern highlands, are comparable in height to those in Ius Chasma, but many have tapered extensions that are more consistent with them being erosional remnants rather than the result of extension of the TAR by deposition from the tapered end. The new observations generally support a reversing transverse dune origin for TARS with heights >= 1 m, and a granule ripple origin for TAR-like ripples with heights <= 0.5 m. Published by Elsevier B.V. C1 Smithsonian Inst, Natl Air & Space Museum, MRC 315, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. RP Zimbelman, JR (reprint author), Smithsonian Inst, Natl Air & Space Museum, MRC 315, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. EM zimbelmanj@si.edu FU NASA [NNG04GN88G, NNX08AK90G] FX Comments by two anonymous reviewers were very helpful during the revision of the manuscript. This work was supported by grants NNG04GN88G and NNX08AK90G to JRZ from the Mars Data Analysis Program of NASA. NR 58 TC 31 Z9 32 U1 0 U2 7 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0169-555X EI 1872-695X J9 GEOMORPHOLOGY JI Geomorphology PD SEP 1 PY 2010 VL 121 IS 1-2 SI SI BP 22 EP 29 DI 10.1016/j.geomorph.2009.05.012 PG 8 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA 636AH UT WOS:000280699300003 ER PT J AU Rodriguez, JAP Tanaka, KL Yamamoto, A Berman, DC Zimbelman, JR Kargel, JS Sasaki, S Yan, JG Miyamoto, H AF Rodriguez, J. Alexis P. Tanaka, Kenneth L. Yamamoto, Aya Berman, Daniel C. Zimbelman, James R. Kargel, Jeffrey S. Sasaki, Sho Yan Jinguo Miyamoto, Hideaki TI The sedimentology and dynamics of crater-affiliated wind streaks in western Arabia Terra, Mars and Patagonia, Argentina SO GEOMORPHOLOGY LA English DT Article DE Mars; Windstreaks; Aeolian; Resurfacing; Sediment transport ID MARTIAN SURFACE; AEOLIAN PROCESSES; MERIDIANI-PLANUM; EXPLORATION; MINERALOGY; MARINER-9; CHEMISTRY; CONTRAST; DEPOSITS; FEATURES AB Wind streaks comprise recent aeolian deposits that have been extensively documented on Venus, Earth and Mars. Martian wind streaks are among the most abundant surface features on the planet and commonly extend from the downwind margins of impact craters. Previous studies of wind streaks emerging from crater interior deposits suggested that the mode of emplacement was primarily related to the deposition of silt-sized particles as these settled from plumes. We have performed geologic investigations of two wind streaks clusters: one situated in western Arabia Terra, a region in the northern hemisphere of Mars, and another in an analogous terrestrial site located in southern Patagonia. Argentina, where occurrences of wind streaks emanate from playas within maar craters. In both these regions we have identified bedforms in sedimentary deposits on crater floors, along wind-facing interior crater margins, and along wind streaks. These observations indicate that these deposits contain sand-sized particles and that sediment migration has occurred via saltation from crater interior deposits to wind streaks. In Arabia Terra and in Patagonia wind streaks initiate from crater floors that contain lithic and evaporitic sedimentary deposits, suggesting that the composition of wind streak source materials has played an important role in development. Spatial and topographic analyses suggest that regional clustering of wind streaks in the studied regions directly correlates to the areal density of craters with interior deposits, the degree of proximity of these deposits, and the craters' rim-to-floor depths. In addition, some (but not all) wind streaks within the studied clusters have propagated at comparable yearly (Earth years) rates. Extensive saltation is inferred to have been involved in its propagation based on the studied terrestrial wind streak that shows ripples and dunes on its surface and the Martian counterpart changes orientation toward the downslope direction where it extends into an impact crater. (C) 2009 Elsevier B.V. All rights reserved. C1 [Rodriguez, J. Alexis P.; Berman, Daniel C.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Tanaka, Kenneth L.] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA. [Yamamoto, Aya] RESTEC, Minato Ku, Tokyo 106, Japan. [Zimbelman, James R.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. [Kargel, Jeffrey S.] Univ Arizona, Tucson, AZ 85721 USA. [Sasaki, Sho] Natl Inst Nat Sci, Natl Astron Observ Japan, Mizusawa, Iwate 0230861, Japan. [Yan Jinguo] Wuhan Univ, State Key Lab Informat Engn Surveying Mapping & R, Wuhan 430070, Peoples R China. [Miyamoto, Hideaki] Univ Tokyo, Univ Museum, Tokyo 1130033, Japan. RP Rodriguez, JAP (reprint author), Planetary Sci Inst, 1700 E Ft Lowell Rd,Suite 106, Tucson, AZ 85719 USA. EM alexis@psi.edu RI Miyamoto, Hideaki/B-9666-2008; Miyamoto, Hideaki/E-3381-2012 NR 88 TC 6 Z9 6 U1 0 U2 10 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0169-555X EI 1872-695X J9 GEOMORPHOLOGY JI Geomorphology PD SEP 1 PY 2010 VL 121 IS 1-2 SI SI BP 30 EP 54 DI 10.1016/j.geomorph.2009.07.020 PG 25 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA 636AH UT WOS:000280699300004 ER PT J AU Foerster, S Monfort, SL AF Foerster, Steffen Monfort, Steven L. TI Fecal glucocorticoids as indicators of metabolic stress in female Sykes' monkeys (Cercopithecus mitis albogularis) SO HORMONES AND BEHAVIOR LA English DT Article DE Cercopithecus mitis; Glucocorticoids; Metabolic stress; Proximate causes; Social behavior; Feeding ecology; Temporal variation; Individual differences; Rank effects ID BABOONS PAPIO-CYNOCEPHALUS; MACAQUES MACACA-FASCICULARIS; MOTHER-INFANT INTERACTIONS; PITUITARY-ADRENAL-FUNCTION; POST-CONFLICT BEHAVIOR; BROWN CAPUCHIN MONKEYS; WILD OLIVE BABOONS; LEMURS LEMUR-CATTA; CORTISOL-LEVELS; CHACMA BABOONS AB Because of their mediating role in the stress response and potential effects on fitness, glucocorticoid (GC) hormones are increasingly used to assess the physiological costs of environmental and behavioral variation among wild vertebrates. Identifying the proximate causes of GC variation, however, is complicated by simultaneous exposure to multiple potentially stressful stimuli. Here, we use data from a partially provisioned social group of Sykes' monkeys to evaluate the effects of potential psychological and metabolic stressors on temporal and individual variation in fecal GC (fGC) excretion among 11 adult females. Despite high rates of agonism over provisioned foods fGCs declined during periods of high provisioning frequency when fruit availability was dominated by neem (Azadirachta indica), an item requiring great feeding effort. Provisioned foods did not prevent fGC increases when availability of the most preferred main fruit item, tamarind (Tamarindus indica), declined drastically. Although rank-related differences in access to provisioned foods and rates of agonism did not lead to an overall effect of rank on fGCs, low-ranking females excreted more fGCs than high-ranking females during a period of high provisioning intensity and low fruit availability. The emergence of this rank effect was associated with elevated feeding effort in all females, a greater access to provisioned items by high-ranking females, and a higher proportion of time spent moving in low-ranking females. Our findings suggest that metabolic stressors were the primary determinants of both temporal and individual variation in fGCs, indicating potential fitness benefits for high-ranking females when food availability is limited. (C) 2010 Elsevier Inc. All rights reserved. C1 [Foerster, Steffen] Columbia Univ, Dept Ecol Evolut & Environm Biol, New York, NY 10027 USA. [Foerster, Steffen] Natl Museums Kenya, Inst Primate Res, Nairobi, Kenya. [Monfort, Steven L.] Smithsonian Conservat Biol Inst, Front Royal, VA USA. RP Foerster, S (reprint author), Columbia Univ, Dept Ecol Evolut & Environm Biol, 1200 Amsterdam Ave,10th Floor Schermerhorn Extens, New York, NY 10027 USA. EM sf2041@columbia.edu FU National Science Foundation [BCS 0550509]; Columbia University; Earthwatch Institute; Animal Behavior Society; American Society of Primatologists; Friends of the National Zoo; Smithsonian Institution FX We are grateful to the Ministry of Education, Science and Technology, Government of Kenya, for permission to conduct research in the country, to the National Museums of Kenya for permission to work at the Cede Ruins National Monument, and to the Institute of Primate Research, Nairobi, for collaboration and local sponsorship. For their assistance with data collection we thank P. Sirya, M. Ogutu, M. Ngonyo, N. Msindai, L Kadane, L Loyola, C. Johnson, M. and S. McDonald Johnson, V. Friedrich, K. Schultz, K. Talbot, and E. Kneip. Thanks to N. Heywood and S. Hodgkiss for their help with sample processing and analysis, and to N. Presley for training SF in hormone extraction and assay procedures. We are grateful to G. Wahungu and L Mureu, Eldoret University, Kenya, for their collaboration on the Earthwatch project "Kenya's Forest Monkeys". We thank all Earthwatch volunteers for donating their vacation time and financial resources to help making this project possible. SF is grateful to M. Cords for guidance throughout all stages of the project and for valuable comments on earlier versions of the manuscript. M. Brown and two anonymous reviewers provided valuable comments and suggestions for improvement. Funding was provided by the National Science Foundation (BCS 0550509), Columbia University, the Earthwatch Institute, the Animal Behavior Society, the American Society of Primatologists, the Friends of the National Zoo and the Smithsonian Institution. NR 110 TC 18 Z9 18 U1 1 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 J9 HORM BEHAV JI Horm. Behav. PD SEP PY 2010 VL 58 IS 4 BP 685 EP 697 DI 10.1016/j.yhbeh.2010.06.002 PG 13 WC Behavioral Sciences; Endocrinology & Metabolism SC Behavioral Sciences; Endocrinology & Metabolism GA 658DG UT WOS:000282469700017 PM 20540944 ER PT J AU Lawrence, DJ Feldman, WC Goldsten, JO McCoy, TJ Blewett, DT Boynton, WV Evans, LG Nittler, LR Rhodes, EA Solomon, SC AF Lawrence, David J. Feldman, William C. Goldsten, John O. McCoy, Timothy J. Blewett, David T. Boynton, William V. Evans, Larry G. Nittler, Larry R. Rhodes, Edgar A. Solomon, Sean C. TI Identification and measurement of neutron-absorbing elements on Mercury's surface SO ICARUS LA English DT Article DE Mercury, surface ID IRON-SILICATE FRACTIONATION; LUNAR PROSPECTOR; GLOBAL PERSPECTIVE; GAMMA-RAY; MESSENGER; MOON; SPECTROMETER; REFLECTANCE; SPECTRA; FLYBY AB MESSENGER Neutron Spectrometer (NS) observations of cosmic-ray-generated thermal neutrons provide the first direct measurements of Mercury's sui face elemental composition Specifically, we show that Mercury's surface is enriched in neutron-absorbing elements and has a measured macroscopic neutron-absorption cross section of 45-81 x 10(-4) cm(2)/g. a range similar to the neutron absorption of lunar basalts from Mare Crisium. The expected neutron-absorbing elements are Fe and Ti, with possible trace amounts of Gd and Sm Fe and Ti, in particular, are important for understanding Mercury's formation and how its surface may have changed over time through magmatic processes. With neutron Doppler filtering - a neutron energy separation technique based on spacecraft velocity - we demonstrate that Mercury's surface composition cannot be matched by prim models, which have characteristically low abundances of Fe, Ti, Gd, and Sm While neutron spectroscopy alone cannot separate the relative contributions of individual neutron-absorbing elements, these results provide strong new constraints on the nature of Mercury's surface materials. For example, if all the measured neutron absorption were due to the presence of an Fe-Ti oxide and that oxide were ilmenite, then Mercury's surface would have an ilmenite content of 7-18 wt% This result is in general agreement with the inference from color imaging and visible-near-infrared spectroscopy that Mercury's overall low reflectance is consistent with a surface composition that is enriched in Fe-Ti oxides The incorporation of substantial Fe and Ti in oxides would imply that the oxygen fugacity of basalts on Mercury is at the upper range of oxygen fugacities inferred for basalts on the Moon (C) 2010 Elsevier Inc All rights reserved C1 [Lawrence, David J.; Goldsten, John O.; Blewett, David T.; Rhodes, Edgar A.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Feldman, William C.] Planetarh Sci Inst, Tucson, AZ 85719 USA. [McCoy, Timothy J.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. [Boynton, William V.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Nittler, Larry R.; Solomon, Sean C.] Carnegie Inst Sci, Washington, DC 20015 USA. [Evans, Larry G.] Comp Sci Corp, Lanham, MD 20706 USA. RP Lawrence, DJ (reprint author), Johns Hopkins Univ, Appl Phys Lab, MP3-E169,11100 Johns Hopkins Dr, Laurel, MD 20723 USA. RI Lawrence, David/E-7463-2015; Blewett, David/I-4904-2012 OI Lawrence, David/0000-0002-7696-6667; Blewett, David/0000-0002-9241-6358 FU MESSENGER Participating Scientist Program; NASA [NASW-00002, NAS5-97271] FX The first author thanks Dorthea Delapp of Los Alamos National Laboratory for early help in the data reduction of MESSENGER NS data and acknowledges support from the MESSENGER Participating Scientist Program. Thorough suggestions by Richard Elphic and an anonymous reviewer greatly improved this paper We thank Miriam Ruler for pointing out a need to clarify the discussion in the text on the application of Eq. (3) The MESSENGER project is supported by the NASA Discovery Program under contracts NASW-00002 to the Carnegie Institution of Washington and NAS5-97271 to the Johns Hopkins University Applied Physics Laboratory. NR 45 TC 36 Z9 36 U1 0 U2 10 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD SEP PY 2010 VL 209 IS 1 SI SI BP 195 EP 209 DI 10.1016/j.icarus.2010.04.005 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 648IZ UT WOS:000281687800016 ER PT J AU Oberst, J Preusker, F Phillips, RJ Watters, TR Head, JW Zuber, MT Solomon, SC AF Oberst, Juergen Preusker, Frank Phillips, Roger J. Watters, Thomas R. Head, James W. Zuber, Maria T. Solomon, Sean C. TI The morphology of Mercury's Caloris basin as seen in MESSENGER stereo topographic models SO ICARUS LA English DT Article DE Mercury; Cratering; Geological processes ID DIGITAL TERRAIN MODELS; EXPRESS HRSC DATA; MARS EXPRESS; GLOBAL PERSPECTIVE; SMOOTH PLAINS; FLYBY AB A digital terrain model (1000-m effective spatial resolution) of the Caloris basin, the largest well-characterized impact basin on Mercury, was produced from 208 stereo images obtained by the MESSENGER narrow-angle camera The basin rim is far from uniform and is characterized by rugged terrain or knobby plains, often disrupted by craters and radial troughs In some sectors, the rim is represented by a single marked elevation step, where height levels drop from the surroundings toward the basin interior by approximately 2 km Two concentric rings, with radii of 690 km and 850 kin, can be discerned in the topography Several pre-Caloris basins and craters can be identified from the terrain model, suggesting that rugged pre-impact topography may have contributed to the varying characteristics of the Caloris rim The basin interior is relatively smooth and shallow, comparable to typical lunar mascon mare basins, supporting the idea that Caloris was partially filled with lava after formation The model displays long-wavelength undulations in topography across the basin interior, but these undulations cannot readily be related to pre-impact topography, volcanic construction, or post-volcanic uplift Because errors in the long-wavelength topography of the model cannot be excluded, confirmation of these undulations must await data from MESSENGER's orbital mission phase (C) 2010 Elsevier Inc All rights reserved C1 [Oberst, Juergen; Preusker, Frank] German Aerosp Ctr, Inst Planetary Sci, D-12489 Berlin, Germany. [Phillips, Roger J.] SW Res Inst, Planetary Sci Directorate, Boulder, CO 80302 USA. [Watters, Thomas R.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. [Head, James W.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. [Zuber, Maria T.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. [Solomon, Sean C.] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA. RP Oberst, J (reprint author), German Aerosp Ctr DLR, Rutherfordstr 2, D-12489 Berlin, Germany. FU NASA [NASW-00002, NAS5-97271] FX We wish to thank two anonymous reviewers whose thoughtful comments improved this manuscript The MESSENGER project is supported by the NASA Discovery Program under contracts NASW-00002 to the Carnegie Institution of Washington and NAS5-97271 to the Johns Hopkins University Applied Physics Laboratory. NR 23 TC 24 Z9 25 U1 0 U2 5 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD SEP PY 2010 VL 209 IS 1 SI SI BP 230 EP 238 DI 10.1016/j.icarus.2010.03.009 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 648IZ UT WOS:000281687800019 ER PT J AU Zuber, MT Montesi, LGJ Farmer, GT Hauck, SA Ritzer, JA Phillips, RJ Solomon, SC Smith, DE Talpe, MJ Head, JW Neumann, GA Watters, TR Johnson, CL AF Zuber, Maria T. Montesi, Laurent G. J. Farmer, Grant T. Hauck, Steven A., II Ritzer, J. Andreas Phillips, Roger J. Solomon, Sean C. Smith, David E. Talpe, Matthieu J. Head, James W., III Neumann, Gregory A. Watters, Thomas R. Johnson, Catherine L. TI Accommodation of lithospheric shortening on Mercury from altimetric profiles of ridges and lobate scarps measured during MESSENGER flybys 1 and 2 SO ICARUS LA English DT Article DE Mercury; Terrestrial planets; Tectonics; Thermal histories ID WRINKLE RIDGES; LOCALIZATION INSTABILITY; TERRESTRIAL PLANETS; OCEANIC LITHOSPHERE; GLOBAL PERSPECTIVE; THRUST FAULTS; FRICTION LAWS; MARS; MISSION; VOLCANISM AB The Mercury Laser Altimeter on the NASA MESSENGER mission has ranged to several ridges and lobate scarps during two equatorial flybys of the planet Mercury The tectonic features sampled, like others documented by spacecraft imaging and Earth-based radar, are spatially isolated and have vertical relief in excess of 1 km The profiles also indicate that the faulting associated with their formation penetrated to tens of kilometers depth into the lithosphere and accommodated substantial shortening To gain insight into the mechanism(s) of strain accommodation across these structures. we per form analytical and numerical modeling of representative dynamic localization mechanisms We find that ductile localization due to shear heating is not favored, given our current understanding of thermal gradients and shallow thermal structure of Mercury at the time of ridge and scarp formation, and is likely to be of secondary importance at best Brittle localization, associated with loss of resistance during fault development or with velocity weakening during sliding on mature faults, is weakly localizing but permits slip to accumulate over geological time scales The range of shallow thermal gradients that produce isolated faults rather than distributed fault sets under the assumption of modest fault weakening is consistent with previous models for Mercury's early global thermal history To be consistent with strain rates predicted nom thermal history models and the amount of shortening required to account for the underlying large-offset faults. ridges and scarps on Mercury likely developed over geologically substantial time S pans (C) 2010 Elsevier Inc All rights reserved C1 [Zuber, Maria T.; Farmer, Grant T.; Smith, David E.; Talpe, Matthieu J.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. [Montesi, Laurent G. J.] Univ Maryland, Dept Geol, College Pk, MD 20742 USA. [Hauck, Steven A., II; Ritzer, J. Andreas] Case Western Reserve Univ, Dept Geol Sci, Cleveland, OH 44106 USA. [Phillips, Roger J.] SW Res Inst, Planetary Sci Directorate, Boulder, CO 80302 USA. [Solomon, Sean C.] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA. [Head, James W., III] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. [Neumann, Gregory A.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. [Watters, Thomas R.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. [Johnson, Catherine L.] Univ British Columbia, Dept Earth & Ocean Sci, Vancouver, BC V6T 1Z4, Canada. RP Zuber, MT (reprint author), MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. RI Hauck, Steven/A-7865-2008; Montesi, Laurent/C-5216-2009; Neumann, Gregory/I-5591-2013 OI Hauck, Steven/0000-0001-8245-146X; Montesi, Laurent/0000-0002-3519-1412; Neumann, Gregory/0000-0003-0644-9944 FU NASA [NAS5-97271, NASW-00002] FX The MESSENGER project and the Mercury Laser Altimeter investigation are supported by the NASA Discovery Program under Contracts NAS5-97271 to the Johns Hopkins University Applied Physics Laboratory and NASW-00002 to the Carnegie Institution of Washington. We are grateful to Karl Mueller and Stephen Martel for thorough reviews NR 68 TC 14 Z9 14 U1 0 U2 5 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD SEP PY 2010 VL 209 IS 1 SI SI BP 247 EP 255 DI 10.1016/j.icarus.2010.02.026 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 648IZ UT WOS:000281687800021 ER PT J AU Bowlin, MS Bisson, IA Shamoun-Baranes, J Reichard, JD Sapir, N Marra, PP Kunz, TH Wilcove, DS Hedenstrom, A Guglielmo, CG Akesson, S Ramenofsky, M Wikelski, M AF Bowlin, Melissa S. Bisson, Isabelle-Anne Shamoun-Baranes, Judy Reichard, Jonathan D. Sapir, Nir Marra, Peter P. Kunz, Thomas H. Wilcove, David S. Hedenstrom, Anders Guglielmo, Christopher G. Akesson, Susanne Ramenofsky, Marilyn Wikelski, Martin TI Grand Challenges in Migration Biology SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Article; Proceedings Paper CT Symposium on Integrative Migration Biology CY JAN 03-07, 2010 CL Seattle, WA SP Soc Integrat & Comparat Biol ID BODY-MASS CHANGES; NOCTURNAL PASSERINE MIGRANTS; LONG-DISTANCE MIGRATION; WIND DRIFT COMPENSATION; KNOTS CALIDRIS-CANUTUS; FATTY-ACID-COMPOSITION; EASTERN NORTH-AMERICA; POLARIZED-LIGHT CUES; OPTIMAL FLIGHT SPEED; GREATER SNOW GEESE AB Billions of animals migrate each year. To successfully reach their destination, migrants must have evolved an appropriate genetic program and suitable developmental, morphological, physiological, biomechanical, behavioral, and life-history traits. Moreover, they must interact successfully with biotic and abiotic factors in their environment. Migration therefore provides an excellent model system in which to address several of the "grand challenges" in organismal biology. Previous research on migration, however, has often focused on a single aspect of the phenomenon, largely due to methodological, geographical, or financial constraints. Integrative migration biology asks 'big questions' such as how, when, where, and why animals migrate, which can be answered by examining the process from multiple ecological and evolutionary perspectives, incorporating multifaceted knowledge from various other scientific disciplines, and using new technologies and modeling approaches, all within the context of an annual cycle. Adopting an integrative research strategy will provide a better understanding of the interactions between biological levels of organization, of what role migrants play in disease transmission, and of how to conserve migrants and the habitats upon which they depend. C1 [Bowlin, Melissa S.; Hedenstrom, Anders] Lund Univ, Dept Biol, S-22362 Lund, Sweden. [Bisson, Isabelle-Anne; Marra, Peter P.] Smithsonian Migratory Bird Ctr, Washington, DC 20013 USA. [Shamoun-Baranes, Judy] Univ Amsterdam, Inst Biodivers & Ecosyst Dynam, NL-1090 GE Amsterdam, Netherlands. [Reichard, Jonathan D.; Kunz, Thomas H.] Boston Univ, Dept Biol, Ctr Ecol & Conservat Biol, Boston, MA 02215 USA. [Sapir, Nir] Hebrew Univ Jerusalem, Dept Evolut Systemat & Ecol, Movement Ecol Lab, Alexander Silberman Inst Life Sci, IL-91904 Jerusalem, Israel. [Wilcove, David S.] Princeton Univ, Woodrow Wilson Sch, Princeton, NJ 08544 USA. [Wilcove, David S.] Princeton Univ, Dept Ecol & Evolutionary Biol, Princeton, NJ 08544 USA. [Guglielmo, Christopher G.] Univ Western Ontario, Dept Biol, Adv Facil Avian Res, London, ON N6A 5B7, Canada. [Akesson, Susanne] Lund Univ, Dept Biol, SE-22362 Lund, Sweden. [Ramenofsky, Marilyn] Univ Calif Davis, Davis, CA 95616 USA. [Wikelski, Martin] Max Planck Inst Ornithol, Dept Migrat & Immunoecol, D-78315 Radolfzell am Bodensee, Germany. RP Bowlin, MS (reprint author), Lund Univ, Dept Biol, Ecol Bldg, S-22362 Lund, Sweden. EM melissabowlin@gmail.com RI Hedenstrom, Anders/F-5377-2010; Shamoun-Baranes, Judy/C-6921-2013; Akesson, Susanne/F-3175-2015; OI Hedenstrom, Anders/0000-0002-1757-0945; Shamoun-Baranes, Judy/0000-0002-1652-7646; Akesson, Susanne/0000-0001-9039-2180; Sapir, Nir/0000-0002-2477-0515 NR 220 TC 69 Z9 70 U1 10 U2 87 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 EI 1557-7023 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD SEP PY 2010 VL 50 IS 3 BP 261 EP 279 DI 10.1093/icb/icq013 PG 19 WC Zoology SC Zoology GA 644AX UT WOS:000281343900001 PM 21558203 ER PT J AU Bayha, KM Dawson, MN Collins, AG Barbeitos, MS Haddock, SHD AF Bayha, Keith M. Dawson, Michael N. Collins, Allen G. Barbeitos, Marcos S. Haddock, Steven H. D. TI Evolutionary Relationships Among Scyphozoan Jellyfish Families Based on Complete Taxon Sampling and Phylogenetic Analyses of 18S and 28S Ribosomal DNA SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Article; Proceedings Paper CT Symposium on Integrative Migration Biology CY JAN 03-07, 2010 CL Seattle, WA SP Soc Integrat & Comparat Biol ID MULTIPLE SEQUENCE ALIGNMENT; CHAIN MONTE-CARLO; MOLECULAR EVIDENCE; SUBSTITUTION MODELS; MAXIMUM-LIKELIHOOD; N SPEC; CNIDARIA; SELECTION; BLOOMS; RATES AB A stable phylogenetic hypothesis for families within jellyfish class Scyphozoa has been elusive. Reasons for the lack of resolution of scyphozoan familial relationships include a dearth of morphological characters that reliably distinguish taxa and incomplete taxonomic sampling in molecular studies. Here, we address the latter issue by using maximum likelihood and Bayesian methods to reconstruct the phylogenetic relationships among all 19 currently valid scyphozoan families, using sequence data from two nuclear genes: 18S and 28S rDNA. Consistent with prior morphological hypotheses, we find strong evidence for monophyly of subclass Discomedusae, order Coronatae, rhizostome suborder Kolpophorae and superfamilies Actinomyariae, Kampylomyariae, Krikomyariae, and Scapulatae. Eleven of the 19 currently recognized scyphozoan families are robustly monophyletic, and we suggest recognition of two new families pending further analyses. In contrast to long-standing morphological hypotheses, the phylogeny shows coronate family Nausithoidae, semaeostome family Cyaneidae, and rhizostome suborder Daktyliophorae to be nonmonophyletic. Our analyses neither strongly support nor strongly refute monophyly of order Rhizostomeae, superfamily Inscapulatae, and families Ulmaridae, Catostylidae, Lychnorhizidae, and Rhizostomatidae. These taxa, as well as familial relationships within Coronatae and within rhizostome superfamily Inscapulatae, remain unclear and may be resolved by additional genomic and taxonomic sampling. In addition to clarifying some historically difficult taxonomic questions and highlighting nodes in particular need of further attention, the molecular phylogeny presented here will facilitate more robust study of phenotypic evolution in the Scyphozoa, including the evolution characters associated with mass occurrences of jellyfish. C1 [Bayha, Keith M.; Dawson, Michael N.] Univ Calif Merced, Sch Nat Sci, Merced, CA 95343 USA. [Collins, Allen G.] Smithsonian Inst, Natl Systemat Lab, NOAAs Fisheries Serv, Natl Museum Nat Hist, Washington, DC 20013 USA. [Barbeitos, Marcos S.] Univ Kansas, Dept Ecol & Evolutionary Biol, Lawrence, KS 66045 USA. [Haddock, Steven H. D.] Monterey Bay Aquarium Res Inst, Moss Landing, CA 95039 USA. RP Bayha, KM (reprint author), Dauphin Isl Sea Lab, 101 Bienville Blvd, Dauphin Isl, AL 36528 USA. EM mdawson@ucmerced.edu RI Barbeitos, Marcos/L-3516-2016; Collins, Allen/A-7944-2008 OI Dawson, Michael/0000-0001-7927-8395; Collins, Allen/0000-0002-3664-9691 NR 119 TC 25 Z9 32 U1 2 U2 24 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 EI 1557-7023 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD SEP PY 2010 VL 50 IS 3 BP 436 EP 455 DI 10.1093/icb/icq074 PG 20 WC Zoology SC Zoology GA 644AX UT WOS:000281343900014 PM 21558214 ER PT J AU Ubelaker, DH AF Ubelaker, Douglas H. TI Paleopathology SO JOURNAL OF ANTHROPOLOGICAL RESEARCH LA English DT Book Review C1 [Ubelaker, Douglas H.] Smithsonian Inst, Washington, DC 20560 USA. RP Ubelaker, DH (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 3 PU UNIV NEW MEXICO, DEPT ANTHROPOL PI ALBUQUERQUE PA MSC01 1040, ANTHROPOLOGY 1, UNIV NEW MEXICO, ALBUQUERQUE, NM 87131 USA SN 0091-7710 J9 J ANTHROPOL RES JI J. Anthropol. Res. PD FAL PY 2010 VL 66 IS 3 BP 426 EP 427 PG 2 WC Anthropology SC Anthropology GA 656SU UT WOS:000282357700022 ER PT J AU Moskal-del Hoyo, M Wachowiak, M Blanchette, RA AF Moskal-del Hoyo, M. Wachowiak, M. Blanchette, R. A. TI Preservation of fungi in archaeological charcoal SO JOURNAL OF ARCHAEOLOGICAL SCIENCE LA English DT Article DE Wood charcoal; Fungal attack; Biodeterioration; Deadwood collection; Anthracology; Archaeobotany ID WOOD; ENVIRONMENTS; VEGETATION; FRANCE; SITES AB During the analysis of wood charcoal remains from archaeological sites, it is common to find different microorganisms and different forms of degradation present in the plant tissue. However, one may encounter difficulties when attempting to identify these microorganisms and determine when their attack occurred. This paper focuses on preservation aspects related to the microorganisms in wood and demonstrates the structural changes that take place in different types of decayed wood after it was converted into charcoal. The study seeks to determine whether the microbial attack found in archaeological woods took place before the burning of the wood or after. Burning experiments were conducted using wood that had been decayed by various types of fungi including white-rot, brown-rot, and soft-rot. The laboratory burnt wood samples showed decay patterns that were comparable to those observed in archaeological charcoal samples, indicating that signs of fungal infestation and features of decay can be preserved after burning with micromorphological details of mycelium and cell wall attack evident. This indication may provide important information related to the gathering of deadwood as fuelwood. In addition, examples of decayed wood preserved in archaeological charcoal assemblages are described. Their relationship to the archaeological context and environmental conditions may suggest different interpretative models concerning wood management strategies applied by past Societies. (C) 2010 Elsevier Ltd. All rights reserved. C1 [Moskal-del Hoyo, M.] Univ Valencia, Dept Prehist & Arqueol, Valencia 46010, Spain. [Wachowiak, M.] Smithsonian Inst, Smithsonian Museum Conservat Inst, Museum Support Ctr, Suitland, MD 20746 USA. [Blanchette, R. A.] Univ Minnesota, Dept Plant Pathol, St Paul, MN 55108 USA. RP Moskal-del Hoyo, M (reprint author), Univ Valencia, Dept Prehist & Arqueol, Avgda Blasco Ibanez 28, Valencia 46010, Spain. EM magdalena.moskal@uv.es; wachowiakm@si.edu; robertb@umn.edu RI Moskal-del Hoyo, Magdalena/B-2696-2012 OI Moskal-del Hoyo, Magdalena/0000-0003-3632-7227 FU University of Valencia FX The authors would like to express their gratitude to Dr. R.J. Koestler and Dr. P. DePriest from the Smithsonian Museum Conservation Institute and Prof. Dr. E. Badal from the University of Valencia for their valuable comments. We would like to thank Prof. Dr. P. Raczky, Dr. A. Anders (Eotvos Lorand University, Budapest), A. Matoga (Archaeological Museum, Krakow), and the Krakow Archaeological Team for Excavation of the Motorways for providing archaeological charcoals. Special thanks to J. Watson (MCI) and the personnel of SEM Laboratory (University of Valencia) for their help. M. Moskal-del Hoyo would also like to thank the University of Valencia (program "V Segles") for the financial support provided while conducting research at the Smithsonian's Museum Conservation Institute. NR 51 TC 16 Z9 17 U1 0 U2 13 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0305-4403 EI 1095-9238 J9 J ARCHAEOL SCI JI J. Archaeol. Sci. PD SEP PY 2010 VL 37 IS 9 BP 2106 EP 2116 DI 10.1016/j.jas.2010.02.007 PG 11 WC Anthropology; Archaeology; Geosciences, Multidisciplinary SC Anthropology; Archaeology; Geology GA 631VB UT WOS:000280377100004 ER PT J AU Driskell, AC Prum, RO Pruett-Jones, S AF Driskell, Amy C. Prum, Richard O. Pruett-Jones, Stephen TI The evolution of black plumage from blue in Australian fairy-wrens (Maluridae): genetic and structural evidence SO JOURNAL OF AVIAN BIOLOGY LA English DT Article ID FEATHER BARBS; MELANOCORTIN-1 RECEPTOR; COLOR; PIGMENTATION; CHICKEN; MC1R; POPULATIONS; VERTEBRATES; 1-RECEPTOR; SCATTERING AB Genetic variation in the melanocortin-1 receptor (MC1R) locus is responsible for color variation, particularly melanism, in many groups of vertebrates. Fairy-wrens, Maluridae, are a family of Australian and New Guinean passerines with several instances of dramatic shifts in plumage coloration, both intra- and inter-specifically. A number of these color changes are from bright blue to black plumage. In this study, we examined sequence variation at the MC1R locus in most genera and species of fairy-wrens. Our primary focus was subspecies of the white-winged fairy-wren Malurus leucopterus in which two subspecies, each endemic to islands off the western Australian coast, are black while the mainland subspecies is blue. We found fourteen variable amino acid residues within M. leucopterus, but at only one position were alleles perfectly correlated with plumage color. Comparison with other fairy-wren species showed that the blue mainland subspecies, not the black island subspecies, had a unique genotype. Examination of MC1R protein sequence variation across our sample of fairy-wrens revealed no correlation between plumage color and sequence in this group. We thus conclude that amino acid changes in the MC1R locus are not directly responsible for the black plumage of the island subspecies of M. leucopterus. Our examination of the nanostructure of feathers from both black and blue subspecies of M. leucopterus and other black and blue fairy-wren species clarifies the evolution of black plumage in this family. Our data indicate that the black white-winged fairy-wrens evolved from blue ancestors because vestiges of the nanostructure required for the production of blue coloration exist within their black feathers. Based on our phylogeographic analysis of M. leucopterus, in which the two black subspecies do not appear to be each other's closest relatives, we infer that there have been two independent evolutionary transitions from blue to black plumage. A third potential transition from blue to black appears to have occurred in a sister clade. C1 [Driskell, Amy C.] Smithsonian Inst, Natl Museum Nat Hist, Lab Analyt Biol, Suitland, MD 20746 USA. [Prum, Richard O.] Yale Univ, Dept Ecol & Evolutionary Biol, New Haven, CT 06520 USA. [Prum, Richard O.] Yale Univ, Peabody Museum Nat Hist, New Haven, CT 06520 USA. [Pruett-Jones, Stephen] Univ Chicago, Dept Ecol & Evolut, Chicago, IL 60546 USA. RP Driskell, AC (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Lab Analyt Biol, 4210 Silver Hill Rd, Suitland, MD 20746 USA. EM pruett-jones@uchicago.edu FU National Science Foundation; Division of Biological Sciences, University of Chicago; Wettenhall Foundation; Chicago Zoological Society; Section of Evolution and Ecology, Univ. of California Davis; Chevron Corporation; Western Australian Petroleum FX This research was supported by the National Science Foundation (all authors), the Division of Biological Sciences, University of Chicago (SP-J), the Wettenhall Foundation (SP-J), Western Australian Petroleum (SP-J), Chevron Corporation (SP-J), the Chicago Zoological Society (SP-J) and the Section of Evolution and Ecology, Univ. of California Davis (ACD). We wish to thank the curators at Australian National Museum, National Museum of Victoria, Western Australian Museum, Burke Museum, the Univ. of Kansas Natural History Museum, Academy of Natural Sciences, and Leo Joseph and Melanie Rathburn for access to specimen samples, the many field and laboratory assistants that helped us during this work, Trevor Price, Emily Kay and Leo Joseph for comments on the manuscript, and lastly T. Quinn for electron microscopy. NR 32 TC 11 Z9 11 U1 1 U2 17 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0908-8857 J9 J AVIAN BIOL JI J. Avian Biol. PD SEP PY 2010 VL 41 IS 5 BP 505 EP 514 DI 10.1111/j.1600-048X.2009.04823.x PG 10 WC Ornithology SC Zoology GA 650KX UT WOS:000281849500002 ER PT J AU Hobson, KA Jehl, JR AF Hobson, Keith A. Jehl, Joseph R., Jr. TI Arctic waders and the capital-income continuum: Further tests using isotopic contrasts of egg components SO JOURNAL OF AVIAN BIOLOGY LA English DT Article ID NUTRIENT ALLOCATIONS; BREEDING GROUNDS; STABLE-ISOTOPES; DELTA-D; BIRDS; SHOREBIRDS; BREEDERS AB Birds migrating annually to high-latitude breeding grounds may benefit from the transport of endogenous nutrient reserves that ultimately contribute to reproduction. Shorebirds represent a diverse group of Arctic breeders that typically arrive on the breeding grounds with body reserves enriched in 13C and 15N due to wintering and staging in marine or estuarine habitats. Such isotopic differences between endogenous macronutrient reserves and local foodwebs allow the use of stable isotopes to test for the source of nutrient allocations to eggs. We examined delta 13C and delta 15N values in lipid-free yolk and albumen and delta 13C values in yolk lipid of first clutches of ten species of sandpiper and plover breeding near Churchill, Manitoba, Canada in 2003. Most birds had egg isotope values indicating a C3 terrestrial biome, which fits primarily an income (exogenous) breeding strategy. Two exceptions were single sandpiper and plover with strong marine isotope values. Among species, strong positive relationships for each isotope between egg tissue components suggest that egg proteins and lipids tended to be derived from the same isotopic source. Correlations of egg delta 13C values for lipids and proteins approached theoretical relationships expected for exogenous breeding strategies, based on captive studies. Significant positive correlations between clutch initiation date and delta 13C values of egg lipids and albumen suggest some endogenous nutrient contributions to later laid eggs but the circumstances under which this may occur are unstudied. Where possible, we recommend that researchers use blood and fat biopsies from laying females as a means of anchoring endogenous and exogenous endpoints for modeling of each reproductive event. We encourage the isotopic analysis of egg albumen, yolk and yolk lipids among individuals and species and tests of correlations among these components as a means of inferring origins of nutrients to eggs. C1 [Hobson, Keith A.] Environm Canada, Saskatoon, SK S7N 3H5, Canada. [Jehl, Joseph R., Jr.] Smithsonian Inst, US Natl Museum Nat Hist 8, Dept Vertebrate Zool, Div Birds, Washington, DC 20013 USA. RP Hobson, KA (reprint author), Environm Canada, 11 Innovat Blvd, Saskatoon, SK S7N 3H5, Canada. EM Keith.Hobson@EC.GC.CA FU Environment Canada FX We thank the staff of the Churchill Northern Studies center for logistical support. This study was supported by an operating grant to KAH from Environment Canada. B. X. Mora Alvarez assisted with sample preparation and stable isotope measurements were conducted at the Dept of Soil Science, University of Saskatchewan by M. Stocki. Paul Smith and an anonymous reviewer provided useful comments on an earlier manuscript draft. NR 21 TC 6 Z9 6 U1 4 U2 17 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0908-8857 EI 1600-048X J9 J AVIAN BIOL JI J. Avian Biol. PD SEP PY 2010 VL 41 IS 5 BP 565 EP 572 DI 10.1111/j.1600-048X.2010.04980.x PG 8 WC Ornithology SC Zoology GA 650KX UT WOS:000281849500009 ER PT J AU Sayer, EJ Tanner, EVJ AF Sayer, Emma J. Tanner, Edmund V. J. TI Experimental investigation of the importance of litterfall in lowland semi-evergreen tropical forest nutrient cycling SO JOURNAL OF ECOLOGY LA English DT Article DE foliar nutrients; litter addition; litter manipulation; litter removal; litterfall seasonality; nitrogen; nutrient limitation; phosphorus; potassium; soil nutrients ID RAIN-FOREST; MOIST FOREST; LEAF-LITTER; SEASONAL DROUGHT; SOIL PROPERTIES; DRY FOREST; PHOSPHORUS; ECOSYSTEMS; PANAMA; FALL AB P>1. The cycling of nutrients in litterfall is considered a key mechanism in the maintenance of tropical forest fertility but its importance has rarely been quantified experimentally. 2. We carried out a long-term (5 years), large-scale litter manipulation experiment in lowland semi-evergreen tropical forest to determine how changes in litterfall affect forest nutrient cycling. We hypothesized that: (i) long-term litter removal would decrease the forest's nutrient supply; (ii) litter addition would increase the forest's nutrient supply; (iii) soil and foliar nutrient concentrations would change in response to litter manipulation and would eventually affect above-ground productivity. 3. To test our hypotheses, we measured trunk growth, litterfall, and nutrient concentrations in live leaves, litter and soil in plots where litter was removed once a month (L-), litter was added once a month (L+) and controls (CT). 4. After 5 years, the concentration of nitrate in the soil and soil stocks of inorganic nitrogen were higher in the L+ plots and lower in the L- plots compared to the controls. Ammonium concentrations in the soil were also lower in the L- plots. Nitrogen in leaves and litter and the annual nitrogen return by litter were higher in the L+ plots, while potassium return was lower in the L- plots. Surprisingly, our treatments had little effect on phosphorus in soil, leaves or litter, even though lowland tropical forests are generally thought to be largely phosphorus limited. 5. Trunk growth of large trees was not affected by litter manipulation but rainy season litterfall from 2003 to 2008 was 13% higher in the L+ plots compared to the controls. 6. Synthesis. Litter removal affected forest nutrient cycling and productivity less than expected, probably because the soil at our site is moderately fertile. However, litter addition increased litterfall indicating that some limitation of forest production was removed by litter addition. We expected strong effects of litter manipulation on phosphorus cycling; instead, we found a stronger effect on nitrogen cycling. Our results suggest that litter is an important source of nutrients, in particular nitrogen, to trees in this lowland semi-evergreen tropical forest. C1 [Sayer, Emma J.; Tanner, Edmund V. J.] Univ Cambridge, Dept Plant Sci, Cambridge CB2 3EA, England. [Sayer, Emma J.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Sayer, EJ (reprint author), Ctr Ecol & Hydrol, Maclean Bldg,Benson Lane, Wallingford OX10 8BB, Oxon, England. EM emsa@ceh.ac.uk RI Sayer, Emma/B-2514-2010 OI Sayer, Emma/0000-0002-3322-4487 FU Gates Cambridge; European Union [MOIF-CT-2005-21728] FX We thank Francisco Valdez, Jesus Valdez, Geraldino Perez, Fabienne Zeugin, Didimo Urena, Andrea Vincent and many Cambridge students for their help in the field; we particularly wish to thank Jennie Bee, Lucy Hayes, Simon Queenborough, Rebecca Upson and Maria Vorontsova for their hard work setting up the plots. We are also grateful to the BCI gamewardens for collecting the live leaf samples, Milton Garcia for his advice on methodology and Robbie Holdaway and Dave Wright for statistical help. E.J.S. was funded by a Gates Cambridge Scholarship, a European Union Marie-Curie Outgoing Fellowship MOIF-CT-2005-21728, and a Cambridge Philosophical Society Travel Grant, E.V.T. was funded by a Mellon Fund Grant, Gonville and Caius College Cambridge and the Department of Plant Sciences, Cambridge. This study was carried out with the permission and support of the Smithsonian Tropical Research Institute and S.J. Wright, to whom we are very grateful. NR 40 TC 37 Z9 44 U1 7 U2 59 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0022-0477 J9 J ECOL JI J. Ecol. PD SEP PY 2010 VL 98 IS 5 BP 1052 EP 1062 DI 10.1111/j.1365-2745.2010.01680.x PG 11 WC Plant Sciences; Ecology SC Plant Sciences; Environmental Sciences & Ecology GA 635PD UT WOS:000280667200008 ER PT J AU Orwin, KH Buckland, SM Johnson, D Turner, BL Smart, S Oakley, S Bardgett, RD AF Orwin, Kate H. Buckland, Sarah M. Johnson, David Turner, Benjamin L. Smart, Simon Oakley, Simon Bardgett, Richard D. TI Linkages of plant traits to soil properties and the functioning of temperate grassland SO JOURNAL OF ECOLOGY LA English DT Article DE bacteria:fungi ratio; carbon cycling; leaf traits; nutrient cycling; plant growth strategy; relative growth rate; root traits; soil microbial community structure ID LITTER DECOMPOSITION; EXTRACTION METHOD; LAND-USE; TERRESTRIAL ECOSYSTEMS; COMMUNITY STRUCTURE; ROOT DECOMPOSITION; GLOBAL CHANGE; CARBON-CYCLE; LEAF TRAITS; NITROGEN AB P>1. Global change is likely to alter plant community structure, with consequences for the structure and functioning of the below-ground community and potential feedbacks to climate change. Understanding the mechanisms behind these plant-soil interactions and feedbacks to the Earth-system is therefore crucial. One approach to understanding such mechanisms is to use plant traits as predictors of functioning. 2. We used a field-based monoculture experiment involving nine grassland species that had been growing on the same base soil for 7 years to test whether leaf, litter and root traits associated with different plant growth strategies can be linked to an extensive range of soil properties relevant to carbon, nitrogen and phosphorus cycling. Soil properties included the biomass and structure of the soil microbial community, soil nutrients, soil microclimate and soil process rates. 3. Plant species with a high relative growth rate (RGR) were associated with high leaf and litter quality (e.g. low toughness, high nitrogen concentrations), an elevated biomass of bacteria relative to fungi in soil, high rates of soil nitrogen mineralization and concentrations of extractable inorganic nitrogen, and to some extent higher available phosphorus pools. 4. In contrast to current theory, species with a high RGR and litter quality were associated with soils with a lower rate of soil respiration and slow decomposition rates. This indicates that predicting processes that influence carbon cycling from plant traits may be more complex than predicting processes that influence nitrogen and phosphorus cycling. 5. Root traits did not show strong relationships to RGR, leaf or litter traits, but were strongly correlated with several soil properties, particularly the biomass of bacteria relative to fungi in soil and measures relating to soil carbon cycling. 6. Synthesis. Our results indicate that plant species from a single habitat can result in significant divergence in soil properties and functioning when grown in monoculture, and that many of these changes are strongly and predictably linked to variation in plant traits associated with different growth strategies. Traits therefore have the potential to be a powerful tool for understanding the mechanisms behind plant-soil interactions and ecosystem functioning, and for predicting how changes in plant species composition associated with global change will feedback to the Earth-system. C1 [Orwin, Kate H.; Bardgett, Richard D.] Univ Lancaster, Lancaster Environm Ctr, Soil & Ecosyst Ecol Lab, Lancaster LA1 4YQ, England. [Johnson, David] Univ Aberdeen, Inst Biol & Environm Sci, Aberdeen AB24 3UU, Scotland. [Turner, Benjamin L.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Smart, Simon; Oakley, Simon] CEH Lancaster, Lancaster Environm Ctr, Lancaster LA1 4UX, England. RP Orwin, KH (reprint author), Univ Lancaster, Lancaster Environm Ctr, Soil & Ecosyst Ecol Lab, Lancaster LA1 4YQ, England. EM k.orwin@lancaster.ac.uk RI Turner, Benjamin/E-5940-2011; Oakley, Simon/K-1857-2013; Johnson, David/N-3193-2013 OI Turner, Benjamin/0000-0002-6585-0722; Oakley, Simon/0000-0002-5757-7420; Johnson, David/0000-0002-6724-1648 NR 67 TC 104 Z9 111 U1 22 U2 231 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0022-0477 J9 J ECOL JI J. Ecol. PD SEP PY 2010 VL 98 IS 5 BP 1074 EP 1083 DI 10.1111/j.1365-2745.2010.01679.x PG 10 WC Plant Sciences; Ecology SC Plant Sciences; Environmental Sciences & Ecology GA 635PD UT WOS:000280667200010 ER PT J AU McCarthy, MC Thaddeus, P AF McCarthy, M. C. Thaddeus, P. TI High-resolution rotational spectroscopy of NNOH+, DCS+, Ar center dot center dot center dot D-3(+), Ar center dot center dot center dot DCO+, and Ar center dot center dot center dot HN2+ SO JOURNAL OF MOLECULAR SPECTROSCOPY LA English DT Article DE Ions; Ion complexes; Rotational spectroscopy; High-resolution; Hyperfine structure ID INFRARED-LASER SPECTROSCOPY; MILLIMETER-WAVE SPECTRUM; HYPERFINE-STRUCTURE; PROTONATED N2O; MOLECULAR-STRUCTURE; COUPLING-CONSTANTS; MICROWAVE-SPECTRA; NITROUS-OXIDE; CARBON CHAINS; HCS+ AB The rotational spectra of the protonated molecules NNOH+ and DCS+, and the ion complexes Ar center dot center dot center dot D-3(+), Ar center dot center dot center dot DCO+,, and Ar center dot center dot center dot HNN+ have been detected by Fourier transform microwave spectroscopy at high spectral resolution, in which the supersonic molecular beam expands along the axis of the Farby-Perot cavity. These new measurements either better resolve or reveal additional line structure not observed in the previous lower resolution studies. Precise nitrogen or deuterium quadrupole coupling constants have been determined for the first time for both ions and Ar center dot center dot center dot DCO+; a tunneling splitting of 72 +/- 5 kHz has been measured for the 1(0.1) -> 0(0.0) transition of Ar center dot center dot center dot D-3(+). Published by Elsevier Inc. C1 [McCarthy, M. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Harvard Univ, Sch Engn & Appl Sci, 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 McCarthy, Michael/0000-0001-9142-0008 FU NSF [CHE-0701204]; NASA [NNX08AE05G] FX We thank CA Gottlieb, D. Kokkin, and H. Gupta for helpful discussions. The work is supported by NSF grant CHE-0701204 and NASA grant NNX08AE05G. NR 41 TC 7 Z9 7 U1 0 U2 2 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0022-2852 J9 J MOL SPECTROSC JI J. Mol. Spectrosc. PD SEP PY 2010 VL 263 IS 1 BP 71 EP 77 DI 10.1016/j.jms.2010.06.006 PG 7 WC Physics, Atomic, Molecular & Chemical; Spectroscopy SC Physics; Spectroscopy GA 647KI UT WOS:000281617000009 ER PT J AU Zanol, J AF Zanol, Joana TI Homology of Prostomial and Pharyngeal Structures in Eunicida (Annelida) Based on Innervation and Morphological Similarities SO JOURNAL OF MORPHOLOGY LA English DT Article DE Annelida; cLSM; Eunicida; homology; nervous system; pharynx; polychaete; prostomium ID CEPHALIC NERVOUS-SYSTEM; DORVILLEIDAE ANNELIDA; PHYLOGENETIC ANALYSIS; POLYCHAETA ANNELIDA; NEREIS-DIVERSICOLOR; ANTERIOR END; BRAIN; REGENERATION; MICROANATOMY; APPENDAGES AB Eunicidan bristle worm families are commonly identified by the shape of their prostomia and pharyngeal structures. However, current hypotheses of homology among these structures are conflicting, making it difficult to assess morphological evolution, reconstruct phylogeny, and produce a stable classification. To generate more consistent hypotheses of homology among eunicidan anterior structures, the author examined the anterior morphology and the nervous system stained with anti-alpha-tubulin and serotonin antibodies in representative species of Eunicidae, Onuphidae, Oenonidae, Dorvilleidae and Lumbrineridae. The shape of the brain varied conspicuously among families; however, it has mostly the same commissures (usually two of the dorsal and five of the ventral roots of the circumoesophageal connective). The stomatogastric system is also conservative in composition, having two main pairs of stomatogastric nerves which vary in their relative position among the different families. Innervation similarities combined with correspondence and topological morphological similarities made it possible to present explicit hypotheses of primary homology of features, such as buccal lips, pharyngeal fold, and dorsolateral fold anterior extension. Buccal lips are present in all families; however, ventral pads on the prostomium of the Dorvillea line of Dorvilleidae are anterior prolongations of the pharyngeal fold and not buccal lips. All examined taxa, except dorvilleid species, have conspicuous dorsolateral fold anterior extension. In Eunicidae, this anterior extension is a transverse band, while in other families it is a pair of folds. Observed similarities also gave insights on the homology of maxillary elements of Dorvilleidae, providing background knowledge for future studies. J. Morphol. 271:1023-1043, 2010. (C) 2010 Wiley-Liss, Inc. C1 [Zanol, Joana] George Washington Univ, Dept Biol Sci, Washington, DC 20052 USA. [Zanol, Joana] Smithsonian Inst, NMNH, Dept Invertebrate Zool, Washington, DC 20013 USA. RP Zanol, J (reprint author), Univ Fed Rio de Janeiro, Dept Genet, Lab Biodiversidade Mol, Inst Biol,Ilha Fundao, Av Prof Rodolpho Paulo Rocco S-N CCS,Bloco A,A2-0, BR-21941617 Rio De Janeiro, Brazil. EM jzanol@gwmail.gwu.edu RI Zanol, Joana/J-6263-2016 OI Zanol, Joana/0000-0002-2178-791X FU NSF; Link Foundation/Smithsonian Institution; Department of Biological Sciences, George Washington University FX Contract grant sponsor: NSF Dissertation Improvement Grant, Link Foundation/Smithsonian Institution Graduate Fellowship and King Research Fellowship, Department of Biological Sciences, George Washington University. NR 59 TC 2 Z9 3 U1 3 U2 5 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0362-2525 J9 J MORPHOL JI J. Morphol. PD SEP PY 2010 VL 271 IS 9 BP 1023 EP 1043 DI 10.1002/jmor.10843 PG 21 WC Anatomy & Morphology SC Anatomy & Morphology GA 643WU UT WOS:000281331700001 PM 20597101 ER PT J AU Matthew, S Salvador, LA Schupp, PJ Paul, VJ Luesch, H AF Matthew, Susan Salvador, Lilibeth A. Schupp, Peter J. Paul, Valerie J. Luesch, Hendrik TI Cytotoxic Halogenated Macrolides and Modified Peptides from the Apratoxin-Producing Marine Cyanobacterium Lyngbya bouillonii from Guam SO JOURNAL OF NATURAL PRODUCTS LA English DT Article ID PAPUA-NEW-GUINEA; MAJUSCULA; COLLECTION; CYANOPHYCEAE; POTENT; STEREOCHEMISTRY; LIPOPEPTIDES; MALYNGAMIDE; LAINGOLIDE; METABOLITE AB Collections of the marine cyanobacterium Lyngbya bouillonii from shallow patch reefs in Apra Harbor, Guam, afforded three hitherto undescribed analogues of the glycosidic macrolide lyngbyaloside, namely, 2-epi-lyngbyaloside (1) and the regioisomeric 18E- and 18Z-lyngbyalosides C (2 and 3). Concurrently we discovered two new analogues of the cytoskeletal actin-disrupting lyngbyabellins, 27-deoxylyngbyabellin A (4) and lyngbyabellin J (5), a novel macrolide of the laingolide family, laingolide B (6), and a linear modified peptide, lyngbyapeptin D (7), along with known lyngbyabellins A and B, lyngbyapeptin A, and lyngbyaloside. The structures of 1-7 were elucidated by a combination of NMR spectroscopic and mass spectrometric analysis. Compounds 1-6 were either brominated (1-3) or chlorinated (4-6), consistent with halogenation being a hallmark of many marine natural products. All extracts derived from these L. bouillonii collections were highly cytotoxic due to the presence of apratoxin A or apratoxin C. Compounds 1-5 showed weak to moderate cytotoxicity to HT29 colorectal adenocarcinoma and HeLa cervical carcinoma cells. C1 [Matthew, Susan; Salvador, Lilibeth A.; Luesch, Hendrik] Univ Florida, Dept Med Chem, Gainesville, FL 32610 USA. [Schupp, Peter J.] Univ Guam, Marine Lab, UOG Stn, Mangilao, GU 96923 USA. [Paul, Valerie J.] Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. RP Luesch, H (reprint author), Univ Florida, Dept Med Chem, 1600 SW Archer Rd, Gainesville, FL 32610 USA. EM luesch@cop.ufl.edu RI Matthew, Susan/E-3817-2012 FU National Institutes of Health (NIGMS) [P41GM086210]; James & Esther King Biomedical Research Program [06-NIR07]; NIH [S06-GM-44796]; NSF FX This research was supported by the National Institutes of Health (NIGMS grant P41GM086210 to H.L. and V.J.P.) and the James & Esther King Biomedical Research Program (Grant No. 06-NIR07 to H.L.). P.J.S. acknowledges NIH MBRS SCORE grant S06-GM-44796 for support. The authors gratefully acknowledge NSF for funding through the External User Program of the National High Magnetic Field Laboratory (NHMFL), which supported some of the NMR studies at the Advanced Magnetic Resonance Imaging and Spectroscopy (AMRIS) facility in the McKnight Brain Institute of the University of Florida (UF). The 600 MHz, 1 mm triple-resonance HTS cryogenic probe was developed through collaboration between UF, NHMFL, and Bruker Biospin. We thank P. Williams for providing standards of 2,3-dihydroxy-3-methylpentanoic acid. This is contribution #660 of the University of Guam Marine Laboratory and contribution #829 from the Smithsonian Marine Station at Fort Pierce. NR 35 TC 41 Z9 41 U1 1 U2 22 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0163-3864 J9 J NAT PROD JI J. Nat. Prod. PD SEP PY 2010 VL 73 IS 9 BP 1544 EP 1552 DI 10.1021/np1004032 PG 9 WC Plant Sciences; Chemistry, Medicinal; Pharmacology & Pharmacy SC Plant Sciences; Pharmacology & Pharmacy GA 652VL UT WOS:000282038800015 PM 20704304 ER PT J AU Salvador, LA Paul, VJ Luesch, H AF Salvador, Lilibeth A. Paul, Valerie J. Luesch, Hendrik TI Caylobolide B, a Macrolactone from Symplostatin 1-Producing Marine Cyanobacteria Phormidium spp. from Florida SO JOURNAL OF NATURAL PRODUCTS LA English DT Article ID UNIVERSAL NMR DATABASE; STEREOCHEMICAL ASSIGNMENT; NATURAL-PRODUCTS; DESERTOMYCIN/OASOMYCIN CLASS; ABSOLUTE-CONFIGURATION; DOLASTATIN 10; ANALOG; AMPHIDINIUM; CREATION AB A Phormidium spp. collection from Key West, Florida, afforded caylobolide B (1), an analogue of the known macrolactone caylobolide A, previously isolated from a Lyngbya tnajuscula collection from the Bahamas. The planar structure of 1 was determined using NMR and MS experiments. The relative configuration for subunits C7 C9 and C25 C29 was assigned using Kishi's Universal NMR Database. Caylobolide B (1) displayed cytotoxic activity against HT29 colorectal adenocarcinoma and HeLa cervical carcinoma cells with IC(50) values of 4.5 and 12.2 mu M, respectively. C1 [Salvador, Lilibeth A.; Luesch, Hendrik] Univ Florida, Dept Med Chem, Gainesville, FL 32610 USA. [Paul, Valerie J.] Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. RP Luesch, H (reprint author), Univ Florida, Dept Med Chem, 1600 SW Archer Rd, Gainesville, FL 32610 USA. EM luesch@cop.ufl.edu OI zaraat, javad/0000-0001-5341-7481 FU National Institutes of Health NIGMS [P4 IGM086210] FX This research was supported by the National Institutes of Health. NIGMS grant P4 IGM086210. We thank Fort Zachary Taylor State Park for granting permission for sample collection. We are grateful to D. Littler for identifying the cyanobacteria, to J. Kwan and R. Ritson-Williams for collecting and extracting the cyanobacteria, and to J. Rocca for assistance in obtaining the NMR spectra. This is contribution #832 from the Smithsonian Marine Station. NR 20 TC 18 Z9 18 U1 0 U2 16 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0163-3864 J9 J NAT PROD JI J. Nat. Prod. PD SEP PY 2010 VL 73 IS 9 BP 1606 EP 1609 DI 10.1021/np100467d PG 4 WC Plant Sciences; Chemistry, Medicinal; Pharmacology & Pharmacy SC Plant Sciences; Pharmacology & Pharmacy GA 652VL UT WOS:000282038800028 PM 20806908 ER PT J AU Giblin-Davis, RM Kanzaki, N Esquivel, A Davies, KA Herre, EA Center, BJ Scheffrahn, RH AF Giblin-Davis, Robin M. Kanzaki, N. Esquivel, A. Davies, K. A. Herre, E. A. Center, B. J. Scheffrahn, R. H. TI FIRST REPORT OF PINWORMS FROM TERMITE HINDGUTS FROM CENTRAL AMERICA SO JOURNAL OF NEMATOLOGY LA English DT Meeting Abstract C1 [Giblin-Davis, Robin M.; Kanzaki, N.; Center, B. J.; Scheffrahn, R. H.] Univ Florida, IFAS, Ft Lauderdale Res & Educ Ctr, Davie, FL 33314 USA. [Kanzaki, N.] Forestry & Forest Prod Res Inst, Forest Pathol Lab, Tsukuba, Ibaraki 3058687, Japan. [Esquivel, A.] Univ Nacl, Escuela Ciencias Agr, Heredia, Costa Rica. [Davies, K. A.] Univ Adelaide, Ctr Evolutionary Biol & Biodivers, Sch Agr Food & Wine, Glen Osmond, SA 5064, Australia. [Herre, E. A.] Smithsonian Trop Res Inst, Balboa, Panama. RI Kanzaki, Natsumi/A-3864-2012 OI Kanzaki, Natsumi/0000-0001-8752-1674 NR 0 TC 0 Z9 0 U1 0 U2 0 PU SOC NEMATOLOGISTS PI MARCELINE PA PO BOX 311, MARCELINE, MO 64658 USA SN 0022-300X J9 J NEMATOL JI J. Nematol. PD SEP PY 2010 VL 42 IS 3 MA 39 BP 243 EP 243 PG 1 WC Zoology SC Zoology GA 792BL UT WOS:000292715400046 ER PT J AU Winkler, IS Labandeira, CC Wappler, T Wilf, P AF Winkler, Isaac S. Labandeira, Conrad C. Wappler, Torsten Wilf, Peter TI DISTINGUISHING AGROMYZIDAE (DIPTERA) LEAF MINES IN THE FOSSIL RECORD: NEW TAXA FROM THE PALEOGENE OF NORTH AMERICA AND GERMANY AND THEIR EVOLUTIONARY IMPLICATIONS SO JOURNAL OF PALEONTOLOGY LA English DT Article ID PLANT-INSECT ASSOCIATIONS; MINING FLIES DIPTERA; PALEOCENE; MORPHOLOGY; SYSTEMATICS; VEGETATION; ARTHROPOD; TERTIARY; MONTANA; EOCENE AB Fossilized leaf mines and other traces of phytophagous insects provide a unique window into ecological and evolutionary associations of the past. Leaf-mining flies (Diptera: Agromyzidae) are an important component of the recent leaf-mining fauna, but their fossil record is sparse compared to other mining insect lineages; many putative agromyzid body fossils and traces are dubiously assigned. Agromyzid leaf mines often can be distinguished from those of other insects by the presence of an intermittent, fluidized frass trail that may alternate between the sides of the mine. Here, we describe two new Paleogene leaf mine fossils, Phytomyzites biliapchaensis Winkler. Labandeira and Will n. sp. from the early Paleocene of southeastern Montana, USA, occurring in leaves of Platanus raynoldsii (Platanaceae); and Phytomyzites schaarschmidti Wappler n. sp., from the middle Eocene of Messel. Germany, occurring in leaves of Toddalia yam (Rutaceae). These fossils both exhibit frass trails indicative of an agromyzid origin, and P. biliapchaensis also exhibits associated stereotypical marks identical to damage caused by feeding punctures of extant adult female Agromyzidae prior to oviposition. Phytomyzites biliapchaensis represents the earliest confirmed record of Agromyzidae, and one of the earliest records for the large dipteran clade Schizophora. Plant hosts of both species belong to genera that are no longer hosts of leaf-mining Agromyzidae. suggesting a complex and dynamic history of early host-plant associations and, for the early Paleocene example, an evolutionary, possibly opportunistic colonization in the midst of the ecological chaos following the end-Cretaceous event in North America. C1 [Winkler, Isaac S.] N Carolina State Univ, Dept Entomol, Raleigh, NC 27695 USA. [Winkler, Isaac S.; Labandeira, Conrad C.] Univ Maryland, Dept Entomol, College Pk, MD 20742 USA. [Labandeira, Conrad C.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20213 USA. [Wappler, Torsten] Univ Bonn, Steinmann Inst Geol Mineral Palaontol, D-53115 Bonn, Germany. [Wilf, Peter] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. RP Winkler, IS (reprint author), N Carolina State Univ, Dept Entomol, Raleigh, NC 27695 USA. EM iswinkle@ncsu.edu RI Wappler, Torsten/D-4287-2011; OI Wappler, Torsten/0000-0003-1592-0988; Winkler, Isaac/0000-0003-2453-021X FU American Philosophical Society; Petroleum Research Fund [35229-G2]; Ryan Family Foundation; NSF [EAR-0236489]; David and Lucile Packard Foundation; Deutsche Forschungsgemeinschaft (DFG) [Ru 665/4-1, Ru 665/4-2] FX We thank Harding Land and Cattle Company for access to the Mexican Hat site; and F. Marsh, E. Currano, D. Danehy, R. Horwitt, K. Johnson, T. Menotti, and A. Mendoza for field and technical assistance with the MH material. PW was funded by the American Philosophical Society, the Petroleum Research Fund (grant 35229-G2), the Ryan Family Foundation, NSF EAR-0236489, and the David and Lucile Packard Foundation. Work of T.W. was supported by a grant from the Deutsche Forschungsgemeinschaft (DFG) no. Ru 665/4-1, 4-2. We thank also M. von Tschirnhaus for early examination of the Messel specimen, for providing important references, and for critical reading of an early draft; E. Currano and one anonymous reviewer for detailed and helpful suggestions; and W.N. Ellis for providing images and helpful comments. F. Marsh assisted with figure assembly. NR 122 TC 16 Z9 17 U1 0 U2 10 PU PALEONTOLOGICAL SOC INC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044 USA SN 0022-3360 J9 J PALEONTOL JI J. Paleontol. PD SEP PY 2010 VL 84 IS 5 BP 935 EP 954 DI 10.1666/09-163.1 PG 20 WC Paleontology SC Paleontology GA 653SE UT WOS:000282116200011 ER PT J AU Yu, F Kress, WJ Gao, JY AF Yu, Fei Kress, W. John Gao, Jiang-Yun TI Morphology, distribution, and chromosome counts of two varieties of Hedychium villosum (Zingiberaceae) SO JOURNAL OF SYSTEMATICS AND EVOLUTION LA English DT Article DE distribution; Hedychium villosum; morphology; polyploidy; Zingiberaceae ID FLOWERING PLANTS; POLYPLOIDY; EVOLUTION; COMPLEX AB Polyploidy is a major mechanism of adaptation and speciation in plants. Two varieties of Hedychium villosum, var. villosum and var. tenuiflorum, primarily differ in plant and flower size. Chromosome number suggests that var. tenuiflorum is diploid (2n = 34) and var. villosum is tetraploid (2n = 68). Although the flowers of the two varieties do not have any difference in floral shape, each can be easily distinguished morphologically because the shoots, leaves, and flowers of the tetraploid var. villosum are consistently larger than the diploid var. tenuiflorum. The two varieties each possess distinct geographic ranges and habitats, and no sympatric distribution has been found. The tetraploid var. villosum has a broader geographic distribution range and more diverse ecological habitats than the diploid var. tenuiflorum. The two varieties are also completely reproductively isolated due to the non-overlap of their flowering times. The two varieties should be recognized as two distinct species as they fulfill the requirements of various species concepts. Thus, we suggested that the tetraploid var. villosum should be kept as Hedychium villosum and the diploid var. tenuiflorum should be renewed to Hedychium tenuiflorum. C1 [Yu, Fei] Chinese Acad Sci, Grad Sch, Beijing 100049, Peoples R China. [Kress, W. John] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. EM gjy@xtbg.org.cn FU National Natural Science Foundation of China [30970440]; West Light Foundation of the Chinese Academy of Sciences; Natural Science Foundation of Yunnan Province of China [2007C108M] FX The authors thank Mr. Zi-Hui YANG for assistance in the field. This work was supported by the National Natural Science Foundation of China (Grant No. 30970440), the West Light Foundation of the Chinese Academy of Sciences to Jiang-Yun GAO, and the Natural Science Foundation of Yunnan Province of China (Grant No. 2007C108M). NR 27 TC 2 Z9 2 U1 0 U2 2 PU WILEY PERIODICALS, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN STREET, MALDEN, MA 02148-529 USA SN 1674-4918 J9 J SYST EVOL JI J. Syst. Evol. PD SEP PY 2010 VL 48 IS 5 BP 344 EP 349 DI 10.1111/j.1759-6831.2010.00094.x PG 6 WC Plant Sciences SC Plant Sciences GA 656RU UT WOS:000282355100005 ER PT J AU Rogala, D Lake, S Maines, C Mecklenburg, M AF Rogala, Dawn Lake, Susan Maines, Christopher Mecklenburg, Marion TI CONDITION PROBLEMS RELATED TO ZINC OXIDE UNDERLAYERS: EXAMINATION OF SELECTED ABSTRACT EXPRESSIONIST PAINTINGS FROM THE COLLECTION OF THE HIRSHHORN MUSEUM AND SCULPTURE GARDEN, SMITHSONIAN INSTITUTION SO JOURNAL OF THE AMERICAN INSTITUTE FOR CONSERVATION LA English DT Article ID PIGMENT; FILMS AB The presence of zinc oxide oil paint and the condition problems observed in a group of paintings from the collection of the Hirshhorn Museum and Sculpture Garden prompted analytical examination of the museum's mid-20th century holdings. Results reveal a link between upper layer deterioration and underlying zinc oxide paint layers, and suggest that certain visible signs of deterioration may signal the presence of more serious and widespread condition problems. The popularity of zinc oxide house paint among mid-century artists creates a higher probability of this type of deterioration in works from this period. C1 [Rogala, Dawn] Smithsonian Inst, Washington, DC 20013 USA. [Lake, Susan] Smithsonian Inst, Hirshhorn Museum & Sculpture Garden, Washington, DC 20013 USA. [Maines, Christopher] Natl Gallery Art, Landover, MD 20785 USA. [Mecklenburg, Marion] Smithsonian Inst, Museum Conservat Inst, Museum Support Ctr, Suitland, MD 20746 USA. RP Rogala, D (reprint author), 501 Holland Lane 809, Alexandria, VA 22314 USA. EM dvrogala@aol.com; lakes@si.edu; c-maines@nga.gov; mecklenburgm@si.edu NR 36 TC 3 Z9 3 U1 0 U2 1 PU MANEY PUBLISHING PI LEEDS PA STE 1C, JOSEPHS WELL, HANOVER WALK, LEEDS LS3 1AB, W YORKS, ENGLAND SN 0197-1360 EI 1945-2330 J9 J AM INST CONSERV JI J. Am. Inst. Conserv. PD FAL-WIN PY 2010 VL 49 IS 2 BP 96 EP 113 PG 18 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA V29YK UT WOS:000208783500003 ER PT J AU Geraci, CJ Zhou, X Morse, JC Kjer, KM AF Geraci, Christy Jo Zhou, Xin Morse, John C. Kjer, Karl M. TI Defining the genus Hydropsyche (Trichoptera:Hydropsychidae) based on DNA and morphological evidence SO JOURNAL OF THE NORTH AMERICAN BENTHOLOGICAL SOCIETY LA English DT Article DE Hydropsychinae; systematics; Hydropsyche; nomenclatural instability; genitalic plasticity; sexual selection ID SLOSSONAE LARVAE TRICHOPTERA; SEXUAL SELECTION; CAPTURE NETS; CADDISFLIES INSECTA; DISSOLVED CADMIUM; CHRONIC TOXICITY; MALE GENITALIA; EVOLUTION; COEVOLUTION; PHYLOGENY AB In this paper, we review the history of Hydropsychinae genus-level classification and nomenclature and present new molecular evidence from mitochondrial cytochrome c oxidase subunit I (COI) and nuclear large subunit ribosomal ribonucleic acid (28S) markers supporting the monophyly of the genus Hydro psyche. Both molecular and morphological characters support a broad conservative definition of Hydro psyche. Caledopsyche, Hydatomanicus, and Occutanspsyche are synonymized with Hydropsyche. The following species groups are established: Hydropsyche bronta Group (generally corresponding with Ceratopsyche and Hydropsyche morosa and newae Groups), Hydropsyche colonica Group (generally corresponding with Orthopsyche), Hydro psyche instabilis Group (generally corresponding with Hydropsyche s.s.), and Hydropsyche naumanni Group (generally corresponding with Occutanspsyche). Molecular data recovered Hydromanicus as paraphyletic, and Cheumatopsyche and Potamyia as sister taxa. The genus names Plectropsyche and Streptopsyche are reinstated. C1 [Zhou, Xin] Univ Guelph, Biodivers Inst Ontario, Guelph, ON N1G 2W1, Canada. [Geraci, Christy Jo] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. [Morse, John C.] Clemson Univ, Dept Entomol Soils & Plant Sci, Clemson, SC 29634 USA. [Kjer, Karl M.] Rutgers State Univ, Sch Environm & Biol Sci, Dept Ecol Evolut & Nat Resources, New Brunswick, NJ 08901 USA. RP Zhou, X (reprint author), Univ Guelph, Biodivers Inst Ontario, Guelph, ON N1G 2W1, Canada. EM geracic@si.edu; xinzhou@uoguelph.ca; jmorse@clemson.edu; kjer@aesop.rutgers.edu RI Zhou, Xin/D-4025-2009 OI Zhou, Xin/0000-0002-1407-7952 FU National Science Foundation (NSF) [DEB0316504, DEB081686]; Natural Sciences and Engineering Research Council of Canada (NSERC); Genome Canada through the Ontario Genomics Institute FX The following people and institutions provided specimens for this analysis: R. Blahnik, D. Cartwright, F. deMoor, T. L. Erwin, O. S. Flint, L. Harvey, H. Hoang, R. Holzenthal, K. A. Johanson, N. Sangpradub, D. Sembel and colleagues, I. Stocks, T. Tsuruishi, J. Ward, A. Wells, B. Welter, L. Yang, the Bishop Museum, Nanjing Agricultural University (China), the National Museum of Natural History (Smithsonian Institution), the University of Minnesota Insect Collection, and the University of Sam Ratulangi (Sulawesi). We thank P. H. Adler and M. W. Turnbull for manuscript reviews, T. L. Erwin for valuable advice on both content and style, and J. Korecki for suggestions on genitalic terminology. M. W. Turnbull also provided laboratory facilities and technical guidance. This research was funded by National Science Foundation (NSF) grant DEB0316504 and DEB081686. The acquisition of DNA barcodes was supported by a Natural Sciences and Engineering Research Council of Canada (NSERC) grant and by grants from Genome Canada through the Ontario Genomics Institute to P. D. N. Hebert. This is Technical Contribution Number 5575 of the Clemson University Experiment Station. NR 80 TC 10 Z9 10 U1 2 U2 12 PU NORTH AMER BENTHOLOGICAL SOC PI LAWRENCE PA 1041 NEW HAMSPHIRE STREET, LAWRENCE, KS 66044 USA SN 0887-3593 J9 J N AM BENTHOL SOC JI J. N. Am. Benthol. Soc. PD SEP PY 2010 VL 29 IS 3 BP 918 EP 933 DI 10.1899/09-031.1 PG 16 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 635XY UT WOS:000280692400011 ER PT J AU Jansen, PA Elschot, K Verkerk, PJ Wright, SJ AF Jansen, Patrick A. Elschot, Kelly Verkerk, P. Johannes Wright, S. Joseph TI Seed predation and defleshing in the agouti-dispersed palm Astrocaryum standleyanum SO JOURNAL OF TROPICAL ECOLOGY LA English DT Article DE Astrocaryum standleyanum; Barro Colorado Island; Bruchidae; cache pilferage; Dasyprocta punctata; scatter-hoarding; Panama; Scolytidae; seed handling; seed predation ID BRUCHID BEETLE; FOREST; PATTERNS; RODENTS; FRUITS; RECRUITMENT; GERMINATION; SURVIVAL; POACHERS; PERU AB The agouti (Dasyprocta punctata) meticulously defleshes Astrocaryum standleyanum palm seeds before scatter hoarding. On Barro Colorado Island, Panama, we experimentally tested three hypotheses on how this behaviour could reduce seed predation to the mutual benefit of the tree and the rodent. The first and established hypothesis that defleshing reduces seed predation by bruchid beetles by intercepting larvae - was rejected. Experiments in which manually defleshed seeds or entire fruits were incubated at different times showed that defleshing reduced bruchid infestation before fruit fall but not after fruit fall. The second hypothesis - that defleshing reduces cache pilferage by making seeds less conspicuous - was supported. An experiment in which intact fruits and manually defleshed seeds were placed in mimicked agouti caches and followed showed that seeds with flesh were pilfered at higher rates than defleshed seeds. The third hypothesis - that defleshing reduces post-dispersal infestation of cached seeds - was rejected. An experiment in which intact fruits and manually defleshed seeds were placed in mammal exclosures and later collected to assess infestation showed that burial reduced seed infestation but defleshing did not. Thus, seed defleshing reduced palm seed predation, but in a different way than previously believed. We also found that (1) bruchid beetles can be pre-dispersal rather than post-dispersal seed predators, (2) seed infestation by scolytid beetles may control bruchid larvae, and (3) scolytids rather than bruchids are the main invertebrate seed predators of this palm. C1 [Jansen, Patrick A.; Elschot, Kelly] Univ Groningen, NL-9750 AA Haren, Netherlands. [Jansen, Patrick A.; Wright, S. Joseph] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Jansen, Patrick A.; Verkerk, P. Johannes] Wageningen Univ, Ctr Ecosyst Studies, NL-6700 AA Wageningen, Netherlands. [Verkerk, P. Johannes] Wageningen Univ, Nematol Lab, NL-6700 ES Wageningen, Netherlands. RP Jansen, PA (reprint author), Univ Groningen, POB 14, NL-9750 AA Haren, Netherlands. EM patrick.jansen@wur.nl RI Wright, Stuart/M-3311-2013; Jansen, Patrick/G-2545-2015 OI Wright, Stuart/0000-0003-4260-5676; Jansen, Patrick/0000-0002-4660-0314 FU Netherlands Foundation for the Advancement of Tropical Research [W84- 584]; Eliasen-Uytenboogaart Foundation FX We thank Pieter van Eijk, Dumas Galvez, Carol Garzon-Lopez, Maaike Renard and Nina Verkerk for help in the field, the Smithsonian Tropical Research Institute for facilities, Jan den Ouden and Pierre-Michel Forget, Tad Theimer and two anonymous reviewers for comments, and the Netherlands Foundation for the Advancement of Tropical Research (Grant W84- 584) and the Eliasen-Uytenboogaart Foundation for funding. NR 45 TC 14 Z9 16 U1 0 U2 18 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0266-4674 EI 1469-7831 J9 J TROP ECOL JI J. Trop. Ecol. PD SEP PY 2010 VL 26 BP 473 EP 480 DI 10.1017/S0266467410000337 PN 5 PG 8 WC Ecology SC Environmental Sciences & Ecology GA 644JM UT WOS:000281371800001 ER PT J AU Ralls, K Sharma, S Smith, DA Bremner-Harrison, S Cypher, BL Maldonado, JE AF Ralls, Katherine Sharma, Sandeep Smith, Deborah A. Bremner-Harrison, Samantha Cypher, Brian L. Maldonado, Jesus E. TI Changes in Kit Fox Defecation Patterns During the Reproductive Season: Implications for Noninvasive Surveys SO JOURNAL OF WILDLIFE MANAGEMENT LA English DT Article DE capture heterogeneity; feces; kit fox; noninvasive surveys; scat; sex ratio; Vulpes macrotis; zinc finger protein gene ID VULPES-MACROTIS-MUTICA; ESTIMATING POPULATION-SIZE; GENOTYPING FECES; DNA; ABUNDANCE; SAMPLES; RELIABILITY; COYOTES; SCAT AB Noninvasive survey methods based on analyzing DNA extracted from feces can be useful for carnivores that are difficult to study by other methods. Changes in fecal deposition patterns associated with reproduction in kit foxes (Vulpes macrotis) might affect results of such surveys. We used a trained dog to collect fresh scats on 2-km transects in the home ranges of 11 radiocollared female kit foxes in January, February, and March 2008 and determined sex of the individual that deposited the scats by amplifying the zinc finger protein gene. Female foxes give birth in mid-February to mid-March. We found a similar number of scats each month. In January, the sex ratio of the scats was not different from the expected 1:1. However, in February there were almost 2 male scats for every female scat and in March there were >8 male scats for every female scat. Comparing March to January, there were more male scats on all 11 transects and fewer female scats on 10 of 11 transects. Around the time pups are born, both sexes appear to show changes in fecal deposition patterns that make it easier to find male scats and harder to find female scats. Effects of these changes on survey results will vary depending on the purpose and design of the survey. Surveys to determine distribution and relative abundance would probably not be negatively affected by these changes. However, if surveys to estimate abundance are conducted during the reproductive season, they could result in an underestimate of population size unless the increased heterogeneity in scat detectability is taken into account. C1 [Ralls, Katherine; Sharma, Sandeep; Maldonado, Jesus E.] Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, Washington, DC 20008 USA. [Smith, Deborah A.] Working Dogs Conservat, Three Forks, MT 59752 USA. [Bremner-Harrison, Samantha; Cypher, Brian L.] Calif State Univ Stanislaus, Endangered Species Recovery Program, Bakersfield, CA 93389 USA. RP Ralls, K (reprint author), Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, Natl Zool Pk, Washington, DC 20008 USA. EM rallsk@thegrid.net OI Bremner-Harrison, Samantha/0000-0003-4770-1376 FU Smithsonian Institution FX We thank S. Phillips for preparing the figure, C. Asa, O. Oftedal, and J. Seidensticker for helpful advice and references, Rio for locating scats, and the Smithsonian Institution's Walcott Fund for financial support. NR 33 TC 7 Z9 7 U1 1 U2 22 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0022-541X EI 1937-2817 J9 J WILDLIFE MANAGE JI J. Wildl. Manage. PD SEP PY 2010 VL 74 IS 7 BP 1457 EP 1462 DI 10.2193/2009-401 PG 6 WC Ecology; Zoology SC Environmental Sciences & Ecology; Zoology GA 644GF UT WOS:000281361200006 ER PT J AU Hong, T AF Hong, Terry TI Gush 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 SEP 1 PY 2010 VL 135 IS 14 BP 100 EP 100 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 645YR UT WOS:000281502600037 ER PT J AU Riley, S AF Riley, Sheila TI Eighteen Acres SO LIBRARY JOURNAL LA English DT Book Review C1 [Riley, Sheila] Smithsonian Inst Libs, Washington, DC USA. RP Riley, S (reprint author), Smithsonian Inst Libs, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU REED BUSINESS INFORMATION PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD SEP 1 PY 2010 VL 135 IS 14 BP 105 EP 105 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 645YR UT WOS:000281502600062 ER PT J AU Guz, SS AF Guz, Savannah Schroll TI Truman Capote Encyclopedia SO LIBRARY JOURNAL LA English DT Book Review C1 [Guz, Savannah Schroll] Smithsonian Lib, 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 SEP 1 PY 2010 VL 135 IS 14 BP 140 EP 140 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 645YR UT WOS:000281502600204 ER PT J AU Guz, SS AF Guz, Savannah Schroll TI Historical Dictionary of Spanish Cinema SO LIBRARY JOURNAL LA English DT Book Review C1 [Guz, Savannah Schroll] Smithsonian Lib, 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 SEP 1 PY 2010 VL 135 IS 14 BP 140 EP 140 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 645YR UT WOS:000281502600206 ER PT J AU Guz, SS AF Guz, Savannah Schroll TI The Diplomat's Dictionary, 2nd edition SO LIBRARY JOURNAL LA English DT Book Review C1 [Guz, Savannah Schroll] Smithsonian Lib, 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 SEP 1 PY 2010 VL 135 IS 14 BP 140 EP 140 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 645YR UT WOS:000281502600203 ER PT J AU Guz, SS AF Guz, Savannah Schroll TI Encyclopedia of Contemporary Writers and Their Work SO LIBRARY JOURNAL LA English DT Book Review C1 [Guz, Savannah Schroll] Smithsonian Lib, 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 SEP 1 PY 2010 VL 135 IS 14 BP 140 EP 140 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 645YR UT WOS:000281502600205 ER PT J AU Guz, SS AF Guz, Savannah Schroll TI A Dictionary of 20th-Century Communism SO LIBRARY JOURNAL LA English DT Book Review C1 [Guz, Savannah Schroll] Smithsonian Lib, 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 SEP 1 PY 2010 VL 135 IS 14 BP 140 EP 140 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 645YR UT WOS:000281502600201 ER PT J AU Guz, SS AF Guz, Savannah Schroll TI Historical Dictionary of French Theater SO LIBRARY JOURNAL LA English DT Book Review C1 [Guz, Savannah Schroll] Smithsonian Lib, 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 SEP 1 PY 2010 VL 135 IS 14 BP 140 EP 140 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 645YR UT WOS:000281502600202 ER PT J AU Maldonado, M Riesgo, A Bucci, A Rutzler, K AF Maldonado, Manuel Riesgo, Ana Bucci, Arianna Ruetzler, Klaus TI Revisiting silicon budgets at a tropical continental shelf: Silica standing stocks in sponges surpass those in diatoms SO LIMNOLOGY AND OCEANOGRAPHY LA English DT Article ID BIOGENIC SILICA; UPTAKE KINETICS; OCEAN; SEA; DISSOLUTION; ANTARCTICA; SPICULES; BALANCE; CYCLE AB Most of the silicon (Si) in marine coastal systems is thought to recirculate under the biological control of planktonic diatoms. We challenge this view after comparing the biogenic silica (bSi) standing stocks contributed by communities of planktonic diatoms and benthic sponges in five habitats of an extensive continental shelf area of the Mesoamerican Caribbean. In most habitats (outer reefs, patch reefs, sea grass beds, and mangroves), the sponge bSi stocks surpassed those of diatoms. Collectively, bSi in sponge communities was about 88.6% of the total Si pool. Diatoms represented 4.2% and ambient silicate about 7.2%. Consequently, when constructing future regional Si budgets in coastal areas, the Si standing stocks in sponge populations should be empirically examined before deciding that their contribution to the total is negligible. In order to understand Si fluxes in coastal areas where sponges are relevant, we need additional empirical approaches to set the timescale of sponge bSi turnover, which appears to be substantially slower than that of diatom bSi. C1 [Maldonado, Manuel; Riesgo, Ana; Bucci, Arianna] CSIC, Ctr Estudios Avanzados Blanes, Girona, Spain. [Ruetzler, Klaus] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Maldonado, M (reprint author), CSIC, Ctr Estudios Avanzados Blanes, Girona, Spain. EM maldonado@ceab.csic.es RI Maldonado, Manuel/J-9331-2012; Riesgo, Ana/E-3341-2014 OI Riesgo, Ana/0000-0002-7993-1523 FU "Formacion de Profesorado Universitario'' Program [AP2005-5369]; Smithsonian's Caribbean Coral Reef Ecosystems Program (CCRE) [880]; Spanish Government [MEC-CTM2005-05366/MAR, MCI-BFU2008-00227/BMC] FX We thank Dan Miller, Claudette De Courley, and Michelle Nestlerode for assisting with fieldwork; Zoila Velasquez for help with taxonomy of phytoplankton; Tanya Ruetzler, Jim Taylor, and Martha Richotas for logistic support at the Smithsonian's Marine Field Station at Carrie Bow Cay; Chip Clark for picture 4E; and Venka Macintyre for editorial review. We also thank P. Treguer for critical review of the manuscript and two anonymous reviewers for their constructive comments. This research benefited from funds provided by a fellowship from the "Formacion de Profesorado Universitario'' Program (AP2005-5369), a 2005-2006 grant from the Smithsonian's Caribbean Coral Reef Ecosystems Program (CCRE Contribution Number 880), and two grants (MEC-CTM2005-05366/MAR; MCI-BFU2008-00227/BMC) from the Spanish Government. NR 29 TC 22 Z9 22 U1 2 U2 20 PU AMER SOC LIMNOLOGY OCEANOGRAPHY PI WACO PA 5400 BOSQUE BLVD, STE 680, WACO, TX 76710-4446 USA SN 0024-3590 J9 LIMNOL OCEANOGR JI Limnol. Oceanogr. PD SEP PY 2010 VL 55 IS 5 BP 2001 EP 2010 DI 10.4319/lo.2010.55.5.2001 PG 10 WC Limnology; Oceanography SC Marine & Freshwater Biology; Oceanography GA 673MI UT WOS:000283667100018 ER PT J AU Barco, SG D'Eri, LR Woodward, BL Winn, JP Rotstein, DS AF Barco, Susan G. D'Eri, Linda R. Woodward, Becky L. Winn, Jeremy P. Rotstein, David S. TI Spectra (R) fishing twine entanglement of a bottlenose dolphin: A case study and experimental modeling SO MARINE POLLUTION BULLETIN LA English DT Article DE Bottlenose dolphin; Tursiops truncatus; Entanglement; Stranding AB We report here the first documented case of a cetacean fatality from entanglement in recreational Spectra (R) fishing twine. Spectra (R) twine is a relatively new microfilament braided twine that is marketed to replace nylon monofilament twine in rod and reel fisheries. Following the case of this entangled bottlenose dolphin (Tursiops truncatus), we conducted tests with Spectra (R) and comparable monofilament twines on Tursiops tissue from stranded animals to compare the abrasion properties of the twines. We found that Spectra (R) twine was significantly more abrasive on bottlenose dolphin fluke tissue than a similar strength and diameter monofilament. With the same forces applied, the Spectra (R) twine cut deeper than the monofilament, exhibiting a linear relationship with force applied where the monofilament appeared to reach a maximum depth of penetration of approximately 2 mm. These tests may explain why this bottlenose dolphin was so severely debilitated from carrying a relatively light load of twine over a short period of time (20 days). Future public and corporate outreach will be essential to minimize the effect that this increasingly popular fishing twine will have on non-target species. (C) 2010 Elsevier Ltd. All rights reserved. C1 [Barco, Susan G.; D'Eri, Linda R.] Virginia Aquarium Res & Conservat Div, Stranding Response Program, Virginia Beach, VA 23451 USA. [Woodward, Becky L.; Winn, Jeremy P.] Woods Hole Oceanog Inst, Woods Hole, MA 02543 USA. [Rotstein, David S.] Univ Corp Atmospher Res, Suitland, MD USA. [Rotstein, David S.] Smithsonian Inst, Suitland, MD USA. RP Barco, SG (reprint author), Virginia Aquarium Res & Conservat Div, Stranding Response Program, 717 Gen Booth Blvd, Virginia Beach, VA 23451 USA. EM sgbarco@virginiaaquarium.com FU Virginia Aquarium Foundation; John H. Prescott Marine Mammal Grant; Virginia Coastal Zone Management Program FX We would like to acknowledge Virginia Aquarium Stranding Response staff Wendy Walton, Christina Trapani, Gwynn Lockhart, Shannon Davis, Maureen Fender and Mark Swingle for work on this difficult case. We thank Michael Moore of Woods Hole Oceanographic Institution for valuable assistance and advice. Many thanks also go to Sentiel (Butch) Rommel at UNC Wilmington for fluke illustrations. Funding for stranding response was provided by the Virginia Aquarium Foundation, the John H. Prescott Marine Mammal Grant Program and the Virginia Coastal Zone Management Program. NR 3 TC 8 Z9 8 U1 5 U2 10 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 SEP PY 2010 VL 60 IS 9 BP 1477 EP 1481 DI 10.1016/j.marpolbul.2010.05.005 PG 5 WC Environmental Sciences; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 653FY UT WOS:000282075500021 PM 20553857 ER PT J AU Weisberg, MK Smith, C Herd, C Haack, H Yamaguchi, A Aoudjehane, HC Welzenbach, L Grossman, JN AF Weisberg, Michael K. Smith, Caroline Herd, Christopher Haack, Henning Yamaguchi, Akira Aoudjehane, Hasnaa Chennaoui Welzenbach, Linda Grossman, Jeffrey N. TI The Meteoritical Bulletin, No. 98, September 2010 SO METEORITICS & PLANETARY SCIENCE LA English DT Article AB This issue of The Meteoritical Bulletin reports information on 1103 meteorites including 281 non-Antarctic meteorites (Table 1) and 822 Antarctic meteorites (Table 2). Reported in full written descriptions are three falls. Full descriptions are also given for three shergottites, two ungrouped irons, a primitive achondrite, an olivine diogenite, and a lunar meteorite. One iron, Gebel Kamil, was found in and around the Kamil impact crater. Also reported is a new dense collection area in Tunisia. Tables list a wide variety of meteorites including chondrites, ureilites, irons, acapulcoites, and HEDs. Antarctic meteorites reported in this edition include meteorites recovered by ANSMET (US), CHINARE (China), KOREAMET (Korea), and the NIPR (Japan) meteorite recovery programs. C1 [Weisberg, Michael K.] Kingsborough Community Coll, Dept Phys Sci, Brooklyn, NY 11235 USA. [Weisberg, Michael K.] CUNY, Grad Sch, Brooklyn, NY 11235 USA. [Weisberg, Michael K.] Amer Museum Nat Hist, Dept Earth & Planetary Sci, New York, NY 10024 USA. [Smith, Caroline] Nat Hist Museum, Dept Mineral, London SW7 5BD, England. [Smith, Caroline] Univ Glasgow, Sch Geog & Earth Sci, Glasgow G12 8QQ, Lanark, Scotland. [Herd, Christopher] Univ Alberta, Dept Earth & Atmospher Sci, Edmonton, AB T6G 2E3, Canada. [Haack, Henning] Univ Copenhagen, Nat Hist Museum Denmark, DK-1350 Copenhagen K, Denmark. [Yamaguchi, Akira] Natl Inst Polar Res, Antarctic Meteorite Res Ctr, Tokyo 1908518, Japan. [Aoudjehane, Hasnaa Chennaoui] Univ Hassan 2, Fac Sci, Dept Geol, Casablanca, Morocco. [Welzenbach, Linda] Smithsonian Inst, Washington, DC 20013 USA. [Grossman, Jeffrey N.] NASA, Washington, DC 20546 USA. RP Weisberg, MK (reprint author), Kingsborough Community Coll, Dept Phys Sci, 2001 Oriental Blvd, Brooklyn, NY 11235 USA. EM meteorite@kingsborough.edu RI Haack, Henning/A-4807-2013 OI Haack, Henning/0000-0002-4618-3178 FU EC FX LF was supported by the EC through the ORIGINS project. NR 3 TC 7 Z9 7 U1 0 U2 0 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD SEP PY 2010 VL 45 IS 9 BP 1530 EP 1551 DI 10.1111/j.1945-5100.2010.01119.x PG 22 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 694NA UT WOS:000285303700011 ER PT J AU Frost, CL Fernandez-Marin, H Smith, JE Hughes, WOH AF Frost, C. L. Fernandez-Marin, H. Smith, J. E. Hughes, W. O. H. TI Multiple gains and losses of Wolbachia symbionts across a tribe of fungus-growing ants SO MOLECULAR ECOLOGY LA English DT Article DE Attini; multilocus sequence typing; phylogenetics; social insect; symbiosis; Wolbachia ID HORIZONTAL TRANSFER; SURFACE PROTEIN; TRANSMISSION; PIPIENTIS; INFECTION; POPULATIONS; TRANSITION; EVOLUTION; BACTERIA; DEFENSE AB Although the intracellular bacterium Wolbachia is ubiquitous in insects, it has a unique relationship with New World ants on which particular bacterial strains have specialized. However, data are from distantly related hosts and detailed phylogenetic information which could reveal transmission dynamics are lacking. Here, we investigate host-Wolbachia relationships in the monophyletic fungus-growing ant tribe Attini, screening 23 species and using multilocus sequence typing to reliably identify Wolbachia strains. This technique reduces the significant problem of recombination seen using traditional single gene techniques. The relationship between Wolbachia and the fungus-growing ants appears complex and dynamic. There is evidence of co-cladogenesis, supporting vertical transmission; however, this is incomplete, demonstrating that horizontal transmission has also occurred. Importantly, the infection prevalence is frequently different between closely related taxa, with the Acromyrmex leaf-cutting ants appearing particularly prone to infection and there being no consistent relationship with any of the major life history transitions. We suggest that infection loss and horizontal transmission have driven epidemics or selective sweeps of Wolbachia, resulting in multiple gains and losses of infection across the fungus-growing ants. C1 [Frost, C. L.; Smith, J. E.; Hughes, W. O. H.] Univ Leeds, Inst Integrat & Comparat Biol, Leeds LS2 9JT, W Yorkshire, England. [Fernandez-Marin, H.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Smith, J. E.] Univ Salford, Sch Environm & Life Sci, Salford M5 4WT, Lancs, England. RP Frost, CL (reprint author), Univ Leeds, Inst Integrat & Comparat Biol, Leeds LS2 9JT, W Yorkshire, England. EM bsclf@leeds.ac.uk RI Hughes, William/A-6957-2014; OI Hughes, William/0000-0003-0951-9768; Smith, Judith/0000-0002-2206-3534 FU Biotechnology and Biological Sciences Research Council; Royal Society; Natural Environment Research Council FX We are grateful to the Smithsonian Tropical Research Institute and Allen Herre for providing facilities in Gamboa, to Juliane Lopes for assistance with collecting the Brazilian samples, to Sophie Evison, Katherine Roberts, Xavier Didelot and Lorenzo Santorelli for technical assistance, to three anonymous reviewers for their constructive comments, and to Henrik De Fine Licht and Morten Schiott for kindly providing ant samples. We also thank the Autoridad Nacional del Ambiente (ANAM) and IBAMA for permission to collect and export the ants, and the Biotechnology and Biological Sciences Research Council, the Royal Society and Natural Environment Research Council for funding. NR 42 TC 26 Z9 26 U1 1 U2 19 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0962-1083 J9 MOL ECOL JI Mol. Ecol. PD SEP PY 2010 VL 19 IS 18 BP 4077 EP 4085 DI 10.1111/j.1365-294X.2010.04764.x PG 9 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 649TS UT WOS:000281797400021 PM 20738784 ER PT J AU Ebeling, H Edge, AC Mantz, A Barrett, E Henry, JP Ma, CJ van Speybroeck, L AF Ebeling, H. Edge, A. C. Mantz, A. Barrett, E. Henry, J. Patrick Ma, C. J. van Speybroeck, L. TI The X-ray brightest clusters of galaxies from the Massive Cluster Survey SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE catalogues; surveys; galaxies: clusters: general; X-rays: galaxies: clusters ID ALL-SKY SURVEY; TELESCOPE LENSING SURVEY; DARK-MATTER; OPTICAL SPECTROSCOPY; SPATIAL-DISTRIBUTION; MACS J0717.5+3745; MILKY-WAY; SAMPLE; CATALOG; CONSTRAINTS AB We present a statistically complete sample of very X-ray luminous galaxy clusters detected in the MAssive Cluster Survey (MACS). This second MACS release comprises all 34 MACS clusters with nominal X-ray fluxes in excess of 2 x 10-12 erg s-1 cm-2 (0.1-2.4 keV) in the ROSAT Bright Source Catalogue; two-thirds of them are new discoveries. Extending over the redshift range from 0.3 to 0.5, this subset complements the complete sample of the 12 most distant MACS clusters (z > 0.5) published in 2007 and further exemplifies the efficacy of X-ray selection for the compilation of samples of intrinsically massive galaxy clusters. Extensive follow-up observations with Chandra/ACIS led to three additional MACS cluster candidates being eliminated as (predominantly) X-ray point sources. For another four clusters - which, however, remain in our sample of 34 - the point-source contamination was found to be about 50 per cent. The median X-ray luminosity of 1.3 x 1045 erg s-1 (0.1-2.4 keV, Chandra, within r(500)) of the clusters in this subsample demonstrates the power of the MACS strategy to find the most extreme and rarest clusters out to significant redshift. A comparison of the optical and X-ray data for all clusters in this release finds a wide range of morphologies with no obvious bias in favour of either relaxed or merging systems. C1 [Ebeling, H.; Barrett, E.; Henry, J. Patrick; Ma, C. J.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Edge, A. C.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Mantz, A.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Mantz, A.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Mantz, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [van Speybroeck, L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Ebeling, H (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. EM ebeling@ifa.hawaii.edu OI Edge, Alastair/0000-0002-3398-6916 FU NASA LTSA [NAG 5-8253]; SAO [GO2-3168X, GO5-6133X, GO0-11140X, DD5-6031X, GO7-8125X, GO8-9118X]; U.S. Department of Energy [DE-AC02-76SF00515]; Stanford Graduate Fellowship; NASA FX We thank many incarnations of the Chandra peer-review panel and of the University of Hawaii's telescope time allocation committee for their support, trust and patience. HE gratefully acknowledges financial support from NASA LTSA grant NAG 5-8253 and SAO grants GO2-3168X, GO5-6133X and GO0-11140X. ACE thanks the Royal Society for generous support during the identification phase of the MACS project. Parts of this work received support from the U.S. Department of Energy under contract number DE-AC02-76SF00515 as well as from SAO grants DD5-6031X, GO7-8125X and GO8-9118X. AM was supported by a Stanford Graduate Fellowship and an appointment to the NASA Postdoctoral Program, administered by Oak Ridge Associated Universities through a contract with NASA. NR 68 TC 106 Z9 106 U1 0 U2 1 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD SEP 1 PY 2010 VL 407 IS 1 BP 83 EP 93 DI 10.1111/j.1365-2966.2010.16920.x PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 641PN UT WOS:000281140900007 ER PT J AU Kipping, DM AF Kipping, David M. TI Investigations of approximate expressions for the transit duration SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: analytical; techniques: photometric; celestial mechanics; eclipses; planetary systems ID LIGHT-CURVE; EXTRASOLAR PLANET; PERTURBATIONS; EXOMOON; ORBIT; STAR AB In this work, we investigate the accuracy of various approximate expressions for the transit duration of a detached binary against the exact solution, found through solving a quartic equation. Additionally, a new concise approximation is derived, which offers more accurate results than those currently in the literature. Numerical simulations are performed to test the accuracy of the various expressions. We find that our proposed expression yields a > 200 per cent improvement in accuracy relative to the most previously employed expression. We derive a new set of equations for retrieving the light-curve parameters and consider the effect of falsely using circular expressions for eccentric orbits, with particularly important consequences for transit surveys. The new expression also allows us to propose a new light-curve fitting parameter set, which minimizes the mutual correlations and thus improves computational efficiency. The equation is also readily differentiated to provide analytic expressions for the transit duration variation due to secular variations in the system parameters, for example due to apsidal precession induced by perturbing planets. C1 [Kipping, David M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kipping, David M.] UCL, Dept Phys & Astron, London WC1E 6BT, England. RP Kipping, DM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM d.kipping@ucl.ac.uk FU HAT-NET; HAT-South; Harvard-Smithsonsian Center for Astrophysics; Science Technology and Facilities Council (STFC) FX DMK has been supported by HAT-NET and HAT-South, the Harvard-Smithsonsian Center for Astrophysics pre-doctoral fellowships and the Science Technology and Facilities Council (STFC) studentships. Author is grateful to A. Pal for extremely helpful comments which improved the quality of this manuscript. Special thanks to G. Bakos for thought-provoking discussions on the subject. Thanks to G. Bakos and G. Tinetti for their continued support and advice. NR 29 TC 41 Z9 41 U1 0 U2 3 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD SEP 1 PY 2010 VL 407 IS 1 BP 301 EP 313 DI 10.1111/j.1365-2966.2010.16894.x PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 641PN UT WOS:000281140900024 ER PT J AU O'Sullivan, E Giacintucci, S David, LP Vrtilek, JM Raychaudhury, S AF O'Sullivan, Ewan Giacintucci, Simona David, Laurence P. Vrtilek, Jan M. Raychaudhury, Somak TI A deep Chandra observation of the poor cluster AWM 4-I. Properties of the central radio galaxy and its effects on the intracluster medium SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; galaxies: clusters: general; galaxies: clusters: individual: AWM 4; galaxies: clusters: intracluster medium; galaxies: individual: NGC 6051; X-rays: galaxies: clusters ID X-RAY LUMINOSITY; INVERSE-COMPTON EMISSION; XMM-NEWTON OBSERVATION; ELLIPTIC GALAXIES; INTERGALACTIC MEDIUM; GASEOUS ATMOSPHERE; COOLING CLUSTERS; PERSEUS CLUSTER; BLACK-HOLE; JET POWER AB Using observations from the Chandra X-ray Observatory and Giant Metrewave Radio Telescope, we examine the interaction between the intracluster medium and central radio source in the poor cluster AWM 4. In the Chandra observation a small cool core or galactic corona is resolved coincident with the radio core. This corona is capable of fuelling the active nucleus, but must be inefficiently heated by jet interactions or conduction, possibly precluding a feedback relationship between the radio source and cluster. A lack of clearly detected X-ray cavities suggests that the radio lobes are only partially filled by relativistic plasma. We estimate a filling factor of = 0.21 (3 Sigma upper limit < 0.42) for the better constrained east lobe. We consider the particle population in the jets and lobes, and find that the standard equipartition assumptions predict pressures and ages which agree poorly with X-ray estimates. Including an electron population extending to low Lorentz factors either reduces (gamma(min) = 100) or removes (gamma(min) = 10) the pressure imbalance between the lobes and their environment. Pressure balance can also be achieved by entrainment of thermal gas, probably in the first few kiloparsecs of the radio jets. We estimate the mechanical power output of the radio galaxy, and find it to be marginally capable of balancing radiative cooling. C1 [O'Sullivan, Ewan; Giacintucci, Simona; David, Laurence P.; Vrtilek, Jan M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [O'Sullivan, Ewan; Raychaudhury, Somak] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Giacintucci, Simona] INAF Inst Radioastron, I-40129 Bologna, Italy. RP O'Sullivan, E (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM ejos@star.sr.bham.ac.uk OI O'Sullivan, Ewan/0000-0002-5671-6900 FU National Aeronautics and Space Administration [GO8-9127X-R, NAS8-03060]; European Community under the Marie Curie Research Training Network FX The authors thank M. Sun and P. Mazzotta for informative discussions, and the anonymous referee for a number of useful suggestions. Support for this work was provided by the National Aeronautics and Space Administration through Chandra Award Number GO8-9127X-R 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. EO'S acknowledges the support of the European Community under the Marie Curie Research Training Network. We thank the staff of the GMRT for their help during the observations. GMRT is run by the National Centre for Radio Astrophysics of the Tata Institute of Fundamental Research. We acknowledge the usage of the HyperLeda data base (http://leda.univ-lyon1.fr). NR 69 TC 14 Z9 14 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD SEP 1 PY 2010 VL 407 IS 1 BP 321 EP 338 DI 10.1111/j.1365-2966.2010.16895.x PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 641PN UT WOS:000281140900026 ER PT J AU Hopkins, PF Hernquist, L AF Hopkins, Philip F. Hernquist, Lars TI A non-parametric estimate of mass 'scoured' in galaxy cores SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; galaxies: evolution; galaxies: formation; quasars: general; cosmology: theory ID SUPERMASSIVE BLACK-HOLES; HUBBLE-SPACE-TELESCOPE; CCD SURFACE PHOTOMETRY; HIGH-REDSHIFT GALAXIES; VIRGO-CLUSTER SURVEY; ELLIPTIC GALAXIES; MERGER REMNANTS; FUNDAMENTAL PLANE; BRIGHTNESS PROFILES; SAURON PROJECT AB We present a simple estimate of the mass 'deficits' in cored spheroids, as a function of galaxy mass and radius within the galaxy. Previous attempts to measure such deficits depended on fitting some functional form to the profile at large radii extrapolating inwards; this is sensitive to the assumed functional form and does not allow for variation in nuclear profile shapes. For example, we show that literally interpreting the residuals from a single/cored Sersic function fit as implied 'deficit' can be misleading. Instead, we take advantage of larger data sets to directly construct stellar mass profiles of observed systems and measure the stellar mass enclosed in a series of physical radii (M(*)(< R)), for samples of cusp and core spheroids at the same stellar mass. We show that there is a significant (model-independent) bimodality in this distribution of central structure for this sample at small radii. We non-parametrically measure the median offset between core and cusp populations (the 'deficit' delta M(*)(< R)). We can then construct the scoured mass profile as a function of radius, without reference to any assumed functional form. The mass deficit rises in power-law fashion (delta M(*)(< R) proportional to R1.3-1.8) from a significant but small mass at R less than or similar to 10 pc, to asymptote to a maximum similar to 0.5-2 M(BH) at similar to 100 pc, where M(BH) is the mass of the central, supermassive black hole (BH) hosted by the spheroid. At larger radii there is no statistically significant separation between populations; the upper limit to the cumulative scoured mass at similar to kpc is similar to 2-4 M(BH). This does not depend strongly on stellar mass. The dispersion in M(*)(< R) appears larger in the core population, possibly reflecting the fact that core scouring increases the scatter in central profile shapes. We measure this broadening effect as a function of radius. The relatively low mass deficits inferred, and characteristic radii, are in good agreement with models of 'scouring' from BH binary systems. C1 [Hopkins, Philip F.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Hopkins, PF (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. EM phopkins@astro.berkeley.edu FU Miller Institute for Basic Research in Science, University of California Berkeley; NASA [NNG06GI68G]; David and Lucile Packard Foundation FX We thank Hagai Perets for insightful comments in the development of this manuscript. We also thank John Kormendy, Tod Lauer, Eliot Quataert and Norm Murray for helpful discussions at various stages in this and related work. Support for PFH was provided by the Miller Institute for Basic Research in Science, University of California Berkeley. EQ is supported in part by NASA grant NNG06GI68G and the David and Lucile Packard Foundation. NR 94 TC 15 Z9 15 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD SEP 1 PY 2010 VL 407 IS 1 BP 447 EP 457 DI 10.1111/j.1365-2966.2010.16915.x PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 641PN UT WOS:000281140900037 ER PT J AU Jonker, PG Torres, MAP Fabian, AC Heida, M Miniutti, G Pooley, D AF Jonker, P. G. Torres, M. A. P. Fabian, A. C. Heida, M. Miniutti, G. Pooley, D. TI A bright off-nuclear X-ray source: a type IIn supernova, a bright ULX or a recoiling supermassive black hole in CXO J122518.6+144545 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: individual: SDSS J122518; 86+144547; 7; X-rays: binaries; X-rays: individual: CXO J122518; 6+144545 ID XMM-NEWTON OBSERVATIONS; ACTIVE GALACTIC NUCLEI; QUASAR SDSS J092712.65+294344.0; CHANDRA; GALAXY; CANDIDATE; EVOLUTION; EMISSION; BINARY; DWARF AB In this paper we report the discovery of CXO J122518.6+144545, a peculiar X-ray source with a position 3.6 +/- 0.2 arcsec off-nuclear from a Sloan Digital Sky Survey Data Release 7 (SDSS DR7) z = 0.0447 galaxy. The 3.6 arcsec offset corresponds to 3.2 kpc at the distance of the galaxy. The 0.3-8 keV X-ray flux of this source is 5 x 10-14 erg cm-2 s-1 and its 0.3-8 keV luminosity is 2.2 x 1041 erg s-1 (2.7 x 1041 erg s-1; 0.5-10 keV) assuming that the source belongs to the associated galaxy. We find a candidate optical counterpart in archival Hubble Space Telescope/Advanced Camera for Surveys g'-band observations of the field containing the galaxy obtained on 2003 June 16. The observed magnitude of g' = 26.4 +/- 0.1 corresponds to an absolute magnitude of -10.1. We discuss the possible nature of the X-ray source and its associated candidate optical counterpart and conclude that the source is either a very blue Type IIn supernova, an ultraluminous X-ray source with a very bright optical counterpart or a recoiling supermassive black hole. C1 [Jonker, P. G.] SRON, Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. [Jonker, P. G.; Torres, M. A. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Jonker, P. G.] Radboud Univ Nijmegen, Dept Astrophys, IMAPP, NL-6500 GL Nijmegen, Netherlands. [Fabian, A. C.] Inst Astron, Cambridge CB3 0HA, England. [Heida, M.] Sterrekundig Inst Utrecht, NL-3584 TA Utrecht, Netherlands. [Miniutti, G.] Ctr Astrobiol CSIC INTA LAEFF, LAEX, E-28691 Madrid, Spain. [Pooley, D.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. RP Jonker, PG (reprint author), SRON, Netherlands Inst Space Res, Sorbonnelaan 2, NL-3584 CA Utrecht, Netherlands. EM p.jonker@sron.nl RI Miniutti, Giovanni/L-2721-2014 OI Miniutti, Giovanni/0000-0003-0707-4531 FU Netherlands Organisation for Scientific Research FX PGJ acknowledges support from a VIDI grant from the Netherlands Organisation for Scientific Research. PGJ and MH acknowledge Cees Bassa for help with the bachelor thesis project of MH. We thank Andrew Dolphin for his help with dolphot. We thank the referees for their comments which helped improve the paper. This research has made use of data obtained from the Chandra Source Catalogue, provided by the Chandra X-ray Center (CXC) as part of the Chandra Data Archive (ADS/Sa.CXO#CSC). This paper is based on observations made with the HST obtained from the ESO/ST-ECF Science Archive Facility. NR 63 TC 35 Z9 35 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD SEP 1 PY 2010 VL 407 IS 1 BP 645 EP 650 DI 10.1111/j.1365-2966.2010.16943.x PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 641PN UT WOS:000281140900053 ER PT J AU Kong, AKH Heinke, CO Di Stefano, R Cohn, HN Lugger, PM Barmby, P Lewin, WHG Primini, FA AF Kong, A. K. H. Heinke, C. O. Di Stefano, R. Cohn, H. N. Lugger, P. M. Barmby, P. Lewin, W. H. G. Primini, F. A. TI Localization of the X-ray source in the globular cluster G1 with Chandra SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE binaries: close; globular clusters: individual: G1; X-rays: binaries ID MASS BLACK-HOLE; XMM-NEWTON; STRUCTURAL PARAMETERS; FUNDAMENTAL PLANE; MAYALL II=G1; RADIO; M31; POPULATION; QUIESCENCE; EMISSION AB We report the most accurate X-ray position of the X-ray source in the giant globular cluster G1 in M31 by using the Chandra X-ray Observatory, Hubble Space Telescope (HST) and Canada-France-Hawaii Telescope (CFHT). G1 is clearly detected with Chandra and by cross-registering with HST and CFHT images, we derive a 1 sigma error radius of 0.15 arcsec, significantly smaller than the previous measurement by XMM-Newton. We conclude that the X-ray emission of G1 is likely to come from within the core radius of the cluster. We have considered a number of possibilities for the origin of the X-ray emission but can rule all but two scenarios out: it could be due to either accretion on to a central intermediate-mass black hole (IMBH) or an ordinary low-mass X-ray binary (LMXB). Based on the X-ray luminosity and the Bondi accretion rate, an IMBH accreting from the cluster gas seems unlikely and we suggest that the X-rays are due to accretion from a companion. Alternatively, the probability that a 1.5M(circle dot) cluster LMXB lies within the 95 per cent X-ray error circle is about 0.7. Therefore we cannot rule out a single LMXB as the origin of the X-ray emission. While we cannot distinguish between different models with current observations, future high-resolution and high-sensitivity radio imaging observations will reveal whether there is an IMBH at the centre of G1. C1 [Kong, A. K. H.] Natl Tsing Hua Univ, Inst Astron, Hsinchu 30013, Taiwan. [Kong, A. K. H.] Natl Tsing Hua Univ, Dept Phys, Hsinchu 30013, Taiwan. [Heinke, C. O.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2G7, Canada. [Di Stefano, R.; Primini, F. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Cohn, H. N.; Lugger, P. M.] Indiana Univ, Dept Astron, Bloomington, IN 47405 USA. [Barmby, P.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [Lewin, W. H. G.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. RP Kong, AKH (reprint author), Natl Tsing Hua Univ, Inst Astron, Hsinchu 30013, Taiwan. EM akong@phys.nthu.edu.tw RI Barmby, Pauline/I-7194-2016; OI Barmby, Pauline/0000-0003-2767-0090; Primini, Francis/0000-0002-6077-0643; Heinke, Craig/0000-0003-3944-6109 FU National Science Council of the Republic of China (Taiwan) [NSC96-2112-M-007-037-MY3] FX This research has made use of data provided by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory on behalf of NASA, and is based on observations made with the NASA/ESA Hubble Space Telescope, and obtained from the Hubble Legacy Archive, which is a collaboration between the Space Telescope Science Institute (STScI/NASA), the Space Telescope European Coordinating Facility (ST-ECF/ESA) and the Canadian Astronomy Data Centre (CADC/NRC/CSA). Ground-based observations were obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA, at the Canada-France-Hawaii Telescope (CFHT) which is operated by the National Research Council (NRC) of Canada, the Institut National des Science de l'Univers of the Centre National de la Recherche Scientifique (CNRS) of France and the University of Hawaii. Access to the CFHT was made possible by the Institute of Astronomy and Astrophysics, Academia Sinica, Taiwan. The CFHT data products were produced at the TERAPIX data centre located at the Institut d'Astrophysique de Paris. AKHK thanks L. Sjouwerman for discussion. This project is supported by the National Science Council of the Republic of China (Taiwan) through grant NSC96-2112-M-007-037-MY3. NR 40 TC 11 Z9 11 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD SEP PY 2010 VL 407 IS 1 BP L84 EP L88 DI 10.1111/j.1745-3933.2010.00910.x PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 753UY UT WOS:000289806400015 ER PT J AU Madej, OK Jonker, PG Fabian, AC Pinto, C Verbunt, F de Plaa, J AF Madej, O. K. Jonker, P. G. Fabian, A. C. Pinto, C. Verbunt, F. de Plaa, J. TI A relativistically broadened O VIII Ly alpha line in the ultracompact X-ray binary 4U 0614+091 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; X-rays : individual : 4U 0614+091; binaries ID XMM-NEWTON; ACCRETION DISCS; EMISSION-LINES; SPECTROSCOPY; IRON; CONSTRAINTS; X0614+091; BURST; NEON AB Ultracompact X-ray binaries consist of a neutron star or black hole that accretes material from a white dwarf donor star. The ultracompact nature is expressed in very short orbital periods of less than 1 h. In the case of 4U 0614+091 oxygen-rich material from a CO or ONe white dwarf is flowing to the neutron star. This oxygen-rich disc can reflect X-rays emitted by the neutron star giving a characteristic emission spectrum. We have analysed high-resolution Reflection Grating Spectrometer and broad-band European Photon Imaging Camera (EPIC) spectra of 4U 0614+091 obtained by the XMM-Newton satellite. We detect a broad emission feature at similar to 0.7 keV in both instruments, which cannot be explained by unusual abundances of oxygen and neon in the line of sight, as proposed before in the literature. We interpret this feature as O VIII Ly alpha emission caused by reflection of X-rays off highly ionized oxygen, in the strong gravitational field close to the neutron star. C1 [Madej, O. K.; Pinto, C.; Verbunt, F.] Univ Utrecht, Astron Inst, NL-3508 TA Utrecht, Netherlands. [Madej, O. K.; Jonker, P. G.; Pinto, C.; de Plaa, J.] SRON Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. [Jonker, P. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Jonker, P. G.] Radboud Univ Nijmegen, NL-6500 HC Nijmegen, Netherlands. [Fabian, A. C.] Inst Astron, Cambridge CB3 OHA, England. RP Madej, OK (reprint author), Univ Utrecht, Astron Inst, POB 80000, NL-3508 TA Utrecht, Netherlands. EM o.madej@sron.nl FU Netherlands Organization for Scientific Research FX We thank Jelle Kaastra, Elisa Costantini and the referee for useful comments. PGJ acknowledges support from a VIDI grant from the Netherlands Organization for Scientific Research. NR 30 TC 18 Z9 18 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD SEP PY 2010 VL 407 IS 1 BP L11 EP L15 DI 10.1111/j.1745-3933.2010.00892.x PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 753UY UT WOS:000289806400022 ER PT J AU Melott, AL Bambach, RK AF Melott, Adrian L. Bambach, Richard K. TI Nemesis reconsidered SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE astrobiology; Oort Cloud; planets and satellites: general; binaries: general ID MASS EXTINCTIONS; SOLAR COMPANION; DIVERSITY; CATASTROPHISM; PERIODICITY; ORIGINATION; STABILITY; GALAXY AB The hypothesis of a companion object (Nemesis) orbiting the Sun was motivated by the claim of a terrestrial extinction periodicity, thought to be mediated by comet showers. The orbit of a distant companion to the Sun is expected to be perturbed by the Galactic tidal field and encounters with passing stars, which will induce variation in the period. We examine the evidence for the previously proposed periodicity, using two modern, greatly improved paleontological data sets of fossil biodiversity. We find that there is a narrow peak at 27 Myr in the cross-spectrum of extinction intensity time series between these independent data sets. This periodicity extends over a time period nearly twice that for which it was originally noted. An excess of extinction events is associated with this periodicity at 99 per cent confidence. In this sense we confirm the originally noted feature in the time series for extinction. However, we find that it displays extremely regular timing for about 0.5 Gyr. The regularity of the timing compared with earlier calculations of orbital perturbation would seem to exclude the Nemesis hypothesis as a causal factor. C1 [Melott, Adrian L.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA. [Bambach, Richard K.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. RP Melott, AL (reprint author), Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA. EM melott@ku.edu FU NASA [NNX09AM85G]; American Astronomical Society FX We thank J. Alroy for the Paleobiology Database extinction data, and R. Muller for his sort of the Sepkoski data and useful discussions about Nemesis. We are grateful to the American Astronomical Society for the sponsorship of the 2007 Honolulu multidisciplinary Splinter Meeting at which discussions leading to this project took place. J. Cornette and an anonymous referee provided useful input. Research support at the University of Kansas was provided by the NASA Program Astrobiology: Exobiology and Evolutionary Biology under grant number NNX09AM85G. NR 25 TC 16 Z9 16 U1 0 U2 8 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD SEP PY 2010 VL 407 IS 1 BP L99 EP L102 DI 10.1111/j.1745-3933.2010.00913.x PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 753UY UT WOS:000289806400018 ER PT J AU Rodriguez-Gil, P Santander-Garcia, M Knigge, C Corradi, RLM Gansicke, BT Barlow, MJ Drake, JJ Drew, J Miszalski, B Napiwotzki, R Steeghs, D Wesson, R Zijlstra, AA Jones, D Liimets, T Munoz-Darias, T Pyrzas, S Rubio-Diez, MM AF Rodriguez-Gil, P. Santander-Garcia, M. Knigge, C. Corradi, R. L. M. Gaensicke, B. T. Barlow, M. J. Drake, J. J. Drew, J. Miszalski, B. Napiwotzki, R. Steeghs, D. Wesson, R. Zijlstra, A. A. Jones, D. Liimets, T. Munoz-Darias, T. Pyrzas, S. Rubio-Diez, M. M. TI The orbital period of V458 Vulpeculae, a post-double common-envelope nova SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; binaries: close; stars: individual: V458 Vul; novae, cataclysmic variables ID INTERMEDIATE-MASS STARS; X-RAY BINARIES; GRAVITATIONAL-RADIATION; CATACLYSMIC BINARIES; STELLAR EVOLUTION; PLANETARY-NEBULA; MAGNETIC BRAKING; PROGENITOR; CANDIDATE; MODELS AB We present time-resolved optical spectroscopy of V458 Vulpeculae (Nova Vul 2007 No. 1) spread over a period of 15 months starting 301 d after its discovery. Our data reveal radial-velocity variations in the He II lambda 5412 and He II lambda 4686 emission lines. A period analysis of the radial-velocity curves resulted in a period of 98.096 47 +/- 0.000 25 min (0.068 122 55 +/- 0.000 000 17 d) which we identify with the orbital period of the binary system. V458 Vul is therefore the planetary nebula central binary star with the shortest period known. We explore the possibility of the system being composed of a relatively massive white dwarf (M-1 greater than or similar to 1.0 M-circle dot) accreting matter from a post-asymptotic giant branch star which produced the planetary nebula observed. In this scenario, the central binary system therefore underwent two common-envelope episodes. A combination of previous photoionization modelling of the nebular spectra, post-asymptotic giant branch evolutionary tracks and the orbital period favour amass of M-2 similar to 0.6 M-circle dot for the donor star. Therefore, the total mass of the system may exceed the Chandrasekhar mass, which makes V458 Vul a Type Ia supernova progenitor candidate. C1 [Rodriguez-Gil, P.; Santander-Garcia, M.; Pyrzas, S.; Rubio-Diez, M. M.] Isaac Newton Grp Telescopes, E-38700 Santa Cruz De La Palma, Spain. [Rodriguez-Gil, P.; Santander-Garcia, M.; Corradi, R. L. M.] Inst Astrofis Canarias, E-38205 San Cristobal la Laguna, Santa Cruz Tene, Spain. [Rodriguez-Gil, P.; Santander-Garcia, M.; Corradi, R. L. M.] Univ La Laguna, Dept Astrofis, E-38205 San Cristobal la Laguna, Santa Cruz Tene, Spain. [Knigge, C.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Gaensicke, B. T.; Steeghs, D.; Pyrzas, S.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Barlow, M. J.; Wesson, R.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Drake, J. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Drew, J.; Miszalski, B.; Napiwotzki, R.] Univ Hertfordshire, STRI, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Zijlstra, A. A.; Liimets, T.] Tartu Observ, EE-61602 Toravere, Estonia. [Jones, D.] Univ Manchester, Jodrell Bank, Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Munoz-Darias, T.] INAF Osservatorio Astron Brera, I-23807 Merate, LC, Italy. [Rubio-Diez, M. M.] CSIC, Ctr Astrobiol, INTA, E-28850 Madrid, Spain. RP Rodriguez-Gil, P (reprint author), Isaac Newton Grp Telescopes, Apartado Correos 321, E-38700 Santa Cruz De La Palma, Spain. EM prguez@ing.iac.es RI Gaensicke, Boris/A-9421-2012; Barlow, Michael/A-5638-2009; Steeghs, Danny/C-5468-2009; Jones, David/G-8109-2014; Rodriguez-Gil, Pablo/H-7709-2015; OI Gaensicke, Boris/0000-0002-2761-3005; Barlow, Michael/0000-0002-3875-1171; Steeghs, Danny/0000-0003-0771-4746; Jones, David/0000-0003-3947-5946; Rodriguez-Gil, Pablo/0000-0002-4717-5102; Drew, Janet/0000-0003-1192-7082 FU STFC FX We thank the referee, Nye Evans, for his comments. The use of Tom Marsh's MOLLY package is gratefully acknowledged. DS acknowledges a STFC Advanced Fellowship. The WHT and the INT are operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. NR 22 TC 24 Z9 24 U1 0 U2 1 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD SEP PY 2010 VL 407 IS 1 BP L21 EP L25 DI 10.1111/j.1745-3933.2010.00895.x PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 753UY UT WOS:000289806400003 ER PT J AU Scannapieco, C Gadotti, DA Jonsson, P White, SDM AF Scannapieco, Cecilia Gadotti, Dimitri A. Jonsson, Patrik White, Simon D. M. TI An observer's view of simulated galaxies: disc-to-total ratios, bars and (pseudo-)bulges SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: numerical; galaxies: formation; galaxies: fundamental parameters; galaxies: photometry; galaxies: structure ID DARK-MATTER UNIVERSE; PARTICLE HYDRODYNAMICS SIMULATIONS; DIGITAL SKY SURVEY; RADIATIVE-TRANSFER; METAL ENRICHMENT; MULTIPHASE MODEL; STAR-FORMATION; FEEDBACK; BULGES; DUST AB We use cosmological hydrodynamical simulations of the formation of Milky Way-mass galaxies to study the relative importance of the main stellar components, i.e. discs, bulges and bars, at redshift zero. The main aim of this Letter is to understand if estimates of the structural parameters of these components determined from kinematics (as is usually done in simulations) agree well with those obtained using a photometric bulge/disc/bar decomposition (as done in observations). To perform such a comparison, we have produced synthetic observations of the simulation outputs with the Monte Carlo radiative transfer code SUNRISE and used the BUDDA code to make 2D photometric decompositions of the resulting images (in the i and g bands). We find that the kinematic disc-to-total (D/T) ratio estimates are systematically and significantly lower than the photometric ones. While the maximum D/T ratios obtained with the former method are of the order of 0.2, they are typically > 0.4, and can be as high as 0.7, according to the latter. The photometric decomposition shows that many of the simulated galaxies have bars, with Bar/T ratios in the range 0.2-0.4, and that bulges have in all cases low Sersic indices, resembling observed pseudo-bulges instead of classical ones. Simulated discs, bulges and bars generally have similar g - i colours, which are in the blue tail of the distribution of observed colours. This is not due to the presence of young stars, but rather due to low metallicities and poor gas content in the simulated galaxies, which makes dust extinction low. Photometric decompositions thus match the component ratios usually quoted for spiral galaxies better than kinematic decompositions, but the shift is insufficient to make the simulations consistent with observed late-type systems. C1 [Scannapieco, Cecilia] Astrophys Inst Potsdam, D-14482 Potsdam, Germany. [Scannapieco, Cecilia; Gadotti, Dimitri A.; White, Simon D. M.] Max Planck Inst Astrophys, D-85748 Garching, Germany. [Gadotti, Dimitri A.] European So Observ, Santiago 19, Chile. [Jonsson, Patrik] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. RP Scannapieco, C (reprint author), Astrophys Inst Potsdam, Sternwarte 16, D-14482 Potsdam, Germany. EM cscannapieco@aip.de NR 21 TC 58 Z9 58 U1 0 U2 1 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD SEP PY 2010 VL 407 IS 1 BP L41 EP L45 DI 10.1111/j.1745-3933.2010.00900.x PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 753UY UT WOS:000289806400006 ER PT J AU Brooks, TM Helgen, KM AF Brooks, Thomas M. Helgen, Kristofer M. TI BIODIVERSITY A standard for species SO NATURE LA English DT Editorial Material C1 [Brooks, Thomas M.] NatureServe, Arlington, VA 22209 USA. [Brooks, Thomas M.] Univ Tasmania, Sch Geog & Environm Studies, Hobart, Tas 7001, Australia. [Helgen, Kristofer M.] Smithsonian Inst, Natl Museum Nat Hist, Div Mammals, Washington, DC 20013 USA. RP Brooks, TM (reprint author), NatureServe, 1101 Wilson Blvd, Arlington, VA 22209 USA. EM tbrooks@natureserve.org; helgenk@si.edu OI Brooks, Thomas/0000-0001-8159-3116 NR 11 TC 8 Z9 8 U1 0 U2 3 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD SEP PY 2010 VL 467 IS 7315 BP 540 EP 541 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 655TT UT WOS:000282273100026 PM 20882005 ER PT J AU Maloof, AC Rose, CV Beach, R Samuels, BM Calmet, CC Erwin, DH Poirier, GR Yao, N Simons, FJ AF Maloof, Adam C. Rose, Catherine V. Beach, Robert Samuels, Bradley M. Calmet, Claire C. Erwin, Douglas H. Poirier, Gerald R. Yao, Nan Simons, Frederik J. TI Possible animal-body fossils in pre-Marinoan limestones from South Australia SO NATURE GEOSCIENCE LA English DT Article ID PROTEROZOIC-NAMA-GROUP; ALGAE; RECORD; GLACIATION; BIOFILMS; SPONGES; PRESERVATION; PHYLOGENY; CARBONATE; EVOLUTION AB The Neoproterozoic era was punctuated by the Sturtian (about 710 million years ago) and Marinoan (about 635 million years ago) intervals of glaciation. In South Australia, the rocks left behind by the glaciations are separated by a succession of limestones and shales, which were deposited at tropical latitudes. Here we describe millimetre- to centimetre-scale fossils from the Trezona Formation, which pre-dates the Marinoan glaciation. These weakly calcified fossils occur as anvil, wishbone, ring and perforated slab shapes and are contained within stromatolitic limestones. The Trezona Formation fossils pre-date the oldest known calcified fossils of this size by 90 million years, and cannot be separated from the surrounding calcite matrix or imaged by traditional X-ray-based tomographic scanning methods. Instead, we have traced cross-sections of individual fossils by serially grinding and scanning each sample at a resolution of 50.8 mu m. From these images we constructed three-dimensional digital models of the fossils. Our reconstructions show a population of ellipsoidal organisms without symmetry and with a network of interior canals that lead to circular apertures on the fossil surface. We suggest that several characteristics of these reef-dwelling fossils are best explained if the fossils are identified as sponge-grade metazoans. C1 [Maloof, Adam C.; Rose, Catherine V.; Calmet, Claire C.; Simons, Frederik J.] Princeton Univ, Dept Geosci, Princeton, NJ 08544 USA. [Beach, Robert; Samuels, Bradley M.] Situ Studio, Brooklyn, NY 11201 USA. [Erwin, Douglas H.] Smithsonian Inst, Dept Paleobiol, Washington, DC 20013 USA. [Poirier, Gerald R.; Yao, Nan] Princeton Univ, Princeton Inst Sci & Technol Mat, Princeton, NJ 08544 USA. RP Maloof, AC (reprint author), Princeton Univ, Dept Geosci, Princeton, NJ 08544 USA. EM maloof@princeton.edu RI Simons, Frederik/A-3427-2008; Yao, Nan/H-2423-2011; OI Simons, Frederik/0000-0003-2021-6645; Rose, Catherine/0000-0001-8149-0977 FU [NSF-EAR0842946]; [NSF-DMR-0819860] FX W. Watters provided us with example imagery, and, along with J. Hawthorne, gave us helpful Matlab advice. B. Evans allowed us to use his precision grinding machine at MIT, E. Feldman provided useful advice about machine design and machine code and S. Myneni helped us with the ATR-FTIR spectroscopy. We would like to thank B. E. Girit, W. A. Rozen, S. Briedfjord and A. Lukyanov of Situ Studio. B. Dyer, J. Strauss, N. Swanson-Hysell and N. Xu assisted with field work. S. Bowring, T. Duffy, J. Grotzinger, A. Knoll, M. Manuel, S. Porter, E. Sperling, G. Subsol and S. Xiao provided stimulating discussion. Flinders National Park and numerous pastoralists graciously allowed us to conduct field work on their land. The research was financially supported by NSF-EAR0842946 to A.C.M. and NSF-DMR-0819860 to the Princeton Center for Complex Materials. NR 45 TC 98 Z9 102 U1 3 U2 33 PU NATURE PUBLISHING GROUP PI NEW YORK PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA SN 1752-0894 J9 NAT GEOSCI JI Nat. Geosci. PD SEP PY 2010 VL 3 IS 9 BP 653 EP 659 DI 10.1038/NGEO934 PG 7 WC Geosciences, Multidisciplinary SC Geology GA 645NL UT WOS:000281467600021 ER PT J AU Donoso, DA Johnston, MK Kaspari, M AF Donoso, David A. Johnston, Mary K. Kaspari, Michael TI Trees as templates for tropical litter arthropod diversity SO OECOLOGIA LA English DT Article DE Tree specialization hypothesis; Abundance; Leaf litter; Arthropods ID MONTANE RAIN-FOREST; HERBIVOROUS INSECTS; HOST-SPECIFICITY; ORIBATID MITES; SOIL FAUNA; ANTS; HABITAT; DECOMPOSITION; BIODIVERSITY; ASSEMBLAGES AB Increased tree species diversity in the tropics is associated with even greater herbivore diversity, but few tests of tree effects on litter arthropod diversity exist. We studied whether tree species influence patchiness in diversity and abundance of three common soil arthropod taxa (ants, gamasid mites, and oribatid mites) in a Panama forest. The tree specialization hypothesis proposes that tree-driven habitat heterogeneity maintains litter arthropod diversity. We tested whether tree species differed in resource quality and quantity of their leaf litter and whether more heterogeneous litter supports more arthropod species. Alternatively, the abundance-extinction hypothesis states that arthropod diversity increases with arthropod abundance, which in turn tracks resource quantity (e.g., litter depth). We found little support for the hypothesis that tropical trees are templates for litter arthropod diversity. Ten tree species differed in litter depth, chemistry, and structural variability. However, the extent of specialization of invertebrates on particular tree taxa was low and the more heterogeneous litter between trees failed to support higher arthropod diversity. Furthermore, arthropod diversity did not track abundance or litter depth. The lack of association between tree species and litter arthropods suggests that factors other than tree species diversity may better explain the high arthropod diversity in tropical forests. C1 [Donoso, David A.; Johnston, Mary K.; Kaspari, Michael] Univ Oklahoma, Dept Zool, Grad Program Ecol & Evolutionary Biol, Norman, OK 73019 USA. [Donoso, David A.] Pontificia Univ Catolica Ecuador, Museo Zool QCAZ, Escuela Ciencias Biol, Quito, Ecuador. [Johnston, Mary K.] Univ Texas Austin, Sect Integrat Biol, Austin, TX 78712 USA. [Kaspari, Michael] Smithsonian Trop Res Inst, Balboa, Panama. RP Donoso, DA (reprint author), Univ Oklahoma, Dept Zool, Grad Program Ecol & Evolutionary Biol, Norman, OK 73019 USA. EM david_donosov@yahoo.com RI Donoso, David/A-2059-2016; OI Donoso, David/0000-0002-3408-1457; Kaspari, Michael/0000-0002-9717-5768 FU NSF [0212386]; Adams scholarship FX We thank L. Vitt, M. Yuan, R. Broughton, Y. Luo, L. Weider, and G. Wellborn for serving in our graduate committee. We thank S. Hubbel, R. Foster, R. Condit, and J. Wright for allowing access to the CTFS plot. We thank O. Dangles, O. Lewis, C. Riehl, J. Shik, L. Williams, and the ZEEB Journal Club for comments in this manuscript. We thank professor H. Schatz for mite identification. An Adams scholarship supported D.A.D. during the writing of this paper. This research was supported by NSF Grant No. 0212386 to M. K. O. Acevedo and H. Castaneda provided logistic support at BCI. NR 74 TC 22 Z9 28 U1 7 U2 53 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0029-8549 J9 OECOLOGIA JI Oecologia PD SEP PY 2010 VL 164 IS 1 BP 201 EP 211 DI 10.1007/s00442-010-1607-3 PG 11 WC Ecology SC Environmental Sciences & Ecology GA 639GV UT WOS:000280962200019 PM 20349247 ER PT J AU Falcon-Lang, HJ Dimichele, WA AF Falcon-Lang, Howard J. Dimichele, William A. TI WHAT HAPPENED TO THE COAL FORESTS DURING PENNSYLVANIAN GLACIAL PHASES? SO PALAIOS LA English DT Article ID PALEOZOIC ICE-AGE; CARBONIFEROUS TROPICAL VEGETATION; SEA-LEVEL CHANGES; NOVA-SCOTIA; SWAMP VEGETATION; ILLINOIS BASIN; PEAT FORMATION; RAIN-FOREST; CLIMATE; RECORD AB Sequence stratigraphic analysis of Pennsylvanian coal-bearing strata suggests that glacial-interglacial fluctuations at high latitudes drove cyclic changes in tropical biomes. A literature review of plant assemblages in this paleoclimatic context suggests that coal forests dominated during humid interglacial phases, but were replaced by seasonally dry vegetation during glacial phases. After each glacial event, coal forests reassembled with largely the same species composition. This remarkable stasis implies that coal-forest refugia existed across the equatorial landscape during glacial phases, expanding to repopulate lowlands during and following deglaciation. One possibility is that refugia comprised small pockets of wetland forest strung Out along valleys at some sites, but data are currently insufficient to test this hypothesis. The model presented here, if accepted, dramatically alters our understanding of the coal forests and helps explain aspects of their dynamics. C1 [Falcon-Lang, Howard J.] Univ London, Dept Earth Sci, Egham TW20 0EX, Surrey, England. [Dimichele, William A.] NMNH Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. RP Falcon-Lang, HJ (reprint author), Univ London, Dept Earth Sci, Egham TW20 0EX, Surrey, England. EM h.falcon-lang@es.rhul.ac.uk RI Falcon-Lang, Howard/D-8465-2011; DiMichele, William/K-4301-2012 FU NERC [NE/F014120/2] FX HFL acknowledges a NERC Advanced Fellowship (NE/F014120/2). We thank Kirk Johnson and the Denver Museum of Nature and Science for kindly giving permission to reproduce the image in Figure 4. The manuscript was improved by the comments of Dr. John Isbell and an anonymous reviewer. NR 64 TC 52 Z9 53 U1 2 U2 27 PU SEPM-SOC SEDIMENTARY GEOLOGY PI TULSA PA 6128 EAST 38TH ST, STE 308, TULSA, OK 74135-5814 USA SN 0883-1351 J9 PALAIOS JI Palaios PD SEP-OCT PY 2010 VL 25 IS 9-10 BP 611 EP 617 DI 10.2110/palo.2009.p09-162r PG 7 WC Geology; Paleontology SC Geology; Paleontology GA 657CK UT WOS:000282389200007 ER PT J AU Geary, DH Hunt, G Magyar, I Schreiber, H AF Geary, Dana H. Hunt, Gene Magyar, Imre Schreiber, Holly TI The paradox of gradualism: phyletic evolution in two lineages of lymnocardiid bivalves (Lake Pannon, central Europe) SO PALEOBIOLOGY LA English DT Article ID LATE-MIOCENE; PHENOTYPIC EVOLUTION; NATURAL-POPULATIONS; RANDOM-WALKS; CONTEMPORARY MICROEVOLUTION; MORPHOLOGICAL EVOLUTION; CLIMATIC CHANGES; RAPID EVOLUTION; FOSSIL RECORD; MODERN LIFE AB Patterns preserved in the fossil record are of the highest importance in addressing questions about long-term evolutionary processes, yet both the description of pattern and its translation into process can be difficult. With respect to gradual phyletic change, we know that randomly generated sequences may exhibit characteristics of a "trend"; apparent patterns, therefore, must be interpreted with caution. Furthermore, even when the claim of a gradual trend can be statistically justified, interpretation of the underlying mechanisms may be challenging. Given that we can observe populations changing rapidly over tens or hundreds of years, it is now more difficult to explain instances of geologically gradual (as opposed to punctuated) change. Here we describe morphologic change in two bivalve lineages from the late Miocene Lake Pannon. We evaluate change according to the model-based methods of Hunt. Both lineages exhibit size increases and shape changes over an interval of nearly 4 million years. Size and two shape variables in the conjungens lineage are best fit by a model of directional evolution; remaining shape variables mostly conform to unbiased random walks. Body-size evolution in the diprosopum lineage is also significantly directional but all shape variables are best fit by the unbiased random walk model; the small number of sampling intervals available for this lineage (n = 6) makes determination of the actual pattern more difficult. Model-fitting results indicate that the parallel trajectories of increasing log shell height over time in the two lineages can be accounted for by an underlying trend shared by both lineages, suggesting that the size increases may be a shared response to the same cause. The pace of phenotypic change, measured as Lynch's A, is slower than the neutral expectation for all size and shape traits. Our examples illustrate well the paradox of gradualism; the sequences exhibit significant directional morphological evolution, but rates of change as measured over the long-term are apparently too slow for directional selection or even drift to be the cause. Viewing long-term phenotypic evolution in terms of populations tracking peaks on adaptive landscapes is useful in this context. Such a view allows for intervals of directional selection (during times of peak movement resulting in the overall trends we can detect) interspersed with intervals of stasis (during times of peak stability resulting in overall changes that appear to proceed more slowly than the neutral expectation). The paradox of gradualism thus reduces to (1) peak movements and their drivers, which are not restricted in rate as are population-genetic drivers, and (2) the maintenance of stasis, on which no consensus exists. We can identify no environmental parameter in the central European Neogene that exhibits consistent change across the interval of gradual morphologic change. It may be that in Lake Pannon the long-term persistence of generally ameliorating conditions (plentiful resources and habitat space, few predators or competitors) resulted in geologically slow but consistent peak shifts, which in turn facilitated size increase and shape change in these lineages. C1 [Geary, Dana H.; Magyar, Imre; Schreiber, Holly] Univ Wisconsin, Dept Geosci, Madison, WI 53706 USA. [Hunt, Gene] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. RP Geary, DH (reprint author), Univ Wisconsin, Dept Geosci, Madison, WI 53706 USA. EM dana@geology.wisc.edu RI Hunt, Gene/B-3783-2010 OI Hunt, Gene/0000-0001-6430-5020 NR 112 TC 10 Z9 11 U1 0 U2 31 PU PALEONTOLOGICAL SOC INC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044 USA SN 0094-8373 J9 PALEOBIOLOGY JI Paleobiology PD FAL PY 2010 VL 36 IS 4 BP 592 EP 614 PG 23 WC Biodiversity Conservation; Ecology; Evolutionary Biology; Paleontology SC Biodiversity & Conservation; Environmental Sciences & Ecology; Evolutionary Biology; Paleontology GA 675EA UT WOS:000283807800005 ER PT J AU Suen, G Scott, JJ Aylward, FO Adams, SM Tringe, SG Pinto-Tomas, AA Foster, CE Pauly, M Weimer, PJ Barry, KW Goodwin, LA Bouffard, P Li, L Osterberger, J Harkins, TT Slater, SC Donohue, TJ Currie, CR AF Suen, Garret Scott, Jarrod J. Aylward, Frank O. Adams, Sandra M. Tringe, Susannah G. Pinto-Tomas, Adrian A. Foster, Clifton E. Pauly, Markus Weimer, Paul J. Barry, Kerrie W. Goodwin, Lynne A. Bouffard, Pascal Li, Lewyn Osterberger, Jolene Harkins, Timothy T. Slater, Steven C. Donohue, Timothy J. Currie, Cameron R. TI An Insect Herbivore Microbiome with High Plant Biomass-Degrading Capacity SO PLOS GENETICS LA English DT Article ID LEAF-CUTTING ANTS; COMPARATIVE METAGENOMICS; BACTERIAL COMMUNITY; FUNGUS GARDENS; GUT MICROBIOME; SEQUENCE DATA; GENE; DATABASE; DIVERSITY; CELLULOSE AB Herbivores can gain indirect access to recalcitrant carbon present in plant cell walls through symbiotic associations with lignocellulolytic microbes. A paradigmatic example is the leaf-cutter ant (Tribe:Attini), which uses fresh leaves to cultivate a fungus for food in specialized gardens. Using a combination of sugar composition analyses, metagenomics, and whole-genome sequencing, we reveal that the fungus garden microbiome of leaf-cutter ants is composed of a diverse community of bacteria with high plant biomass-degrading capacity. Comparison of this microbiome's predicted carbohydrate-degrading enzyme profile with other metagenomes shows closest similarity to the bovine rumen, indicating evolutionary convergence of plant biomass degrading potential between two important herbivorous animals. Genomic and physiological characterization of two dominant bacteria in the fungus garden microbiome provides evidence of their capacity to degrade cellulose. Given the recent interest in cellulosic biofuels, understanding how large-scale and rapid plant biomass degradation occurs in a highly evolved insect herbivore is of particular relevance for bioenergy. C1 [Suen, Garret; Scott, Jarrod J.; Aylward, Frank O.; Adams, Sandra M.; Foster, Clifton E.; Pauly, Markus; Slater, Steven C.; Donohue, Timothy J.; Currie, Cameron R.] Univ Wisconsin Madison, Dept Energy, Great Lakes Bioenergy Res Ctr, Madison, WI 53706 USA. [Suen, Garret; Scott, Jarrod J.; Aylward, Frank O.; Adams, Sandra M.; Donohue, Timothy J.; Currie, Cameron R.] Univ Wisconsin Madison, Dept Bacteriol, Madison, WI USA. [Scott, Jarrod J.; Currie, Cameron R.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Tringe, Susannah G.; Barry, Kerrie W.; Goodwin, Lynne A.] Joint Genome Inst, Dept Energy, Walnut Creek, CA USA. [Pinto-Tomas, Adrian A.] Univ Costa Rica, Dept Bioquim, Fac Med, San Jose, Costa Rica. [Pinto-Tomas, Adrian A.] Univ Costa Rica, Ctr Invest Estruct Microscopicas, San Jose, Costa Rica. [Foster, Clifton E.] Michigan State Univ, Dept Biochem & Mol Biol, E Lansing, MI 48824 USA. [Pauly, Markus] Michigan State Univ, Dept Energy, Plant Res Lab, E Lansing, MI 48824 USA. [Weimer, Paul J.] USDA ARS, US Dairy Forage Res Ctr, Madison, WI 53706 USA. [Goodwin, Lynne A.] Los Alamos Natl Lab, Biosci Div, Los Alamos, NM USA. [Bouffard, Pascal; Li, Lewyn] 454 Life Sci, Branford, CT USA. [Osterberger, Jolene; Harkins, Timothy T.] Roche Appl Sci, Roche Diagnost, Indianapolis, IN USA. RP Suen, G (reprint author), Univ Wisconsin Madison, Dept Energy, Great Lakes Bioenergy Res Ctr, Madison, WI 53706 USA. EM currie@bact.wisc.edu RI Pauly, Markus/B-5895-2008; OI Pauly, Markus/0000-0002-3116-2198; Suen, Garret/0000-0002-6170-711X; Tringe, Susannah/0000-0001-6479-8427; Donohue, Timothy/0000-0001-8738-2467 FU DOE Great Lakes Bioenergy Research Center [DE-FC02-07ER64494]; National Science Foundation [DEB-0747002, MCB-0702025, MCB-0731822]; Smithsonian Institution Predoctoral Fellowship; Organization for Tropical Studies Research Fellowship; USDA-ARS [3655-41000-005-00D]; US Department of Energy Joint Genome Institute; Office of Science of the US Department of Energy [DE-AC02-05CH11231]; Roche Diagnostics FX This work was funded by the DOE Great Lakes Bioenergy Research Center (DOE BER Office of Science DE-FC02-07ER64494) supporting GS, JJS, FOA, SMA, CEF, MP, SCS, TJD, and CRC. This work was also supported by the National Science Foundation grants DEB-0747002, MCB-0702025, and MCB-0731822 to CRC; a Smithsonian Institution Predoctoral Fellowship supporting JJS; an Organization for Tropical Studies Research Fellowship supporting AAP-T; and a USDA-ARS CRIS project 3655-41000-005-00D supporting PJW. The work conducted by the US Department of Energy Joint Genome Institute is supported by the Office of Science of the US Department of Energy under Contract No. DE-AC02-05CH11231. This work was made possible by a small sequencing grant from Roche Diagnostics. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 62 TC 77 Z9 77 U1 10 U2 79 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1553-7404 J9 PLOS GENET JI PLoS Genet. PD SEP PY 2010 VL 6 IS 9 AR e1001129 DI 10.1371/journal.pgen.1001129 PG 14 WC Genetics & Heredity SC Genetics & Heredity GA 656VM UT WOS:000282369200010 PM 20885794 ER PT J AU Pfrender, ME Hawkins, CP Bagley, M Courtney, GW Creutzburg, BR Epler, JH Fend, S Ferrington, LC Hartzell, PL Jackson, S Larsen, DP Levesque, CA Morse, JC Petersen, MJ Ruiter, D Schindel, D Whiting, M AF Pfrender, Michael E. Hawkins, Charles P. Bagley, Mark Courtney, Gregory W. Creutzburg, Brian R. Epler, John H. Fend, Steve Ferrington, Leonard C., Jr. Hartzell, Paula L. Jackson, Suzanne Larsen, David P. Levesque, C. Andre Morse, John C. Petersen, Matthew J. Ruiter, Dave Schindel, David Whiting, Michael TI ASSESSING MACROINVERTEBRATE BIODIVERSITY IN FRESHWATER ECOSYSTEMS: ADVANCES AND CHALLENGES IN DNA-BASED APPROACHES SO QUARTERLY REVIEW OF BIOLOGY LA English DT Review DE barcoding; invertebrates; bioassessment; biodiversity; freshwater; next-generation sequencing ID TAXONOMIC RESOLUTION; OLIGONUCLEOTIDE ARRAY; MOLECULAR-IDENTIFICATION; BIOLOGICAL INTEGRITY; CHIRONOMIDS DIPTERA; GENUS-LEVEL; MICROARRAY; BARCODES; DIVERSITY; HYBRIDIZATION AB Assessing the biodiversity of macroinvertebrate fauna in freshwater ecosystems is an essential component of both basic ecological inquiry and applied ecological assessments. Aspects of taxonomic diversity and composition in freshwater communities are widely used to quantify water quality and measure the efficacy of remediation and restoration efforts. The accuracy and precision of biodiversity assessments based on standard morphological identifications are often limited by taxonomic resolution and sample size. Morphologically based identifications are laborious and costly, significantly constraining the sample sizes that can be processed. We suggest that the development of an assay platform based on DNA signatures wilt increase the precision and ease of quantifying biodiversity in freshwater ecosystems. Advances in this area will be particularly relevant for benthic and planktonic invertebrates, which are often monitored by regulatory agencies. Adopting a genetic assessment platform will alleviate some of the current limitations to biodiversity assessment strategies. We discuss the benefits and challenges associated with DNA-based assessments and the methods that are currently available. As recent advances in microarray and next-generation sequencing technologies will facilitate a transition to DNA-based assessment approaches, future research efforts should focus on methods for data collection, assay platform development, establishing linkages between DNA signatures and well-resolved taxonomies, and bioinformatics. C1 [Pfrender, Michael E.] Utah State Univ, Dept Biol, Logan, UT 84322 USA. [Hawkins, Charles P.; Creutzburg, Brian R.] Utah State Univ, Western Ctr Monitoring & Assessment Freshwater Ec, Dept Watershed Sci, Logan, UT 84322 USA. [Bagley, Mark; Jackson, Suzanne] US EPA, Natl Exposure Res Lab, Cincinnati, OH 45268 USA. [Courtney, Gregory W.; Petersen, Matthew J.] Iowa State Univ, Dept Entomol, Ames, IA 50011 USA. [Fend, Steve] US Geol Survey, Menlo Pk, CA 94025 USA. [Ferrington, Leonard C., Jr.] Univ Minnesota, Dept Entomol, St Paul, MN 55108 USA. [Hartzell, Paula L.] Univ Hawaii Manoa, Pacific Cooperat Studies Unit, Honolulu, HI 96822 USA. [Hartzell, Paula L.] Hawaii Dept Land & Nat Resources, Honolulu, HI USA. [Larsen, David P.] Pacific States Marine Fisheries Commiss, Corvallis, OR 97333 USA. [Levesque, C. Andre] Agr & Agri Food Canada, Ottawa, ON K1A 0C6, Canada. [Morse, John C.] Clemson Univ, Dept Entomol Soils & Plant Sci, Clemson, SC 29634 USA. [Schindel, David] Smithsonian Inst, Consortium Barcode Life, Natl Museum Nat Hist, Washington, DC 20013 USA. [Whiting, Michael] Brigham Young Univ, Dept Biol, Provo, UT 84602 USA. RP Pfrender, ME (reprint author), Univ Notre Dame, Dept Biol Sci, Notre Dame, IN 46556 USA. EM MICHAEL.PFRENDER.1@ND.EDU; CHUCK.HAWKINS@USU.EDU; BAGLEY.MARK@EPAMAIL.EPA.GOV; GWCOURT@IASTATE.EDU; BRIAN.CREUTZBURG@AGGIEMAIL.USU.EDU; JOHNEPLER3@COMCAST.NET; SVFEND@USGS.GOV; FERRI016@UMN.EDU; PAULAHARTZELL@HOTMAIL.COM; JACKSON.SUZANNE@EPAMAIL.EPA.GOV; LARSEN.PHIL@EPAMAIL.EPA.GOV; ANDRE.LEVESQUE@AGR.GC.CA; JMORSE@CLEMSON.EDU; MJP266@CORNELL.EDU; DRUITER@MSN.COM; SCHINDELD@SI.EDU; MICHAEL_WHITING@BYU.EDU RI Hawkins, Charles/A-4530-2008 OI Hawkins, Charles/0000-0003-1247-0248 FU USU Center for Integrated BioSystems; USU Ecology Center; USU Office of Research FX The ideas and synthesis in this article were fostered by a workshop organized by MEP and CPH at Utah State University. The workshop was supported by funds from the USU Center for Integrated BioSystems, the USU Ecology Center, and the USU Office of Research. Although this work was reviewed by EPA and approved for publication, it may not necessarily reflect official Agency policy. NR 95 TC 28 Z9 29 U1 1 U2 51 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0033-5770 EI 1539-7718 J9 Q REV BIOL JI Q. Rev. Biol. PD SEP PY 2010 VL 85 IS 3 BP 319 EP 340 PG 22 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 643EE UT WOS:000281277600003 PM 20919633 ER PT J AU Moini, M AF Moini, Mehdi TI Metal displacement and stoichiometry of protein-metal complexes under native conditions using capillary electrophoresis/mass spectrometry SO RAPID COMMUNICATIONS IN MASS SPECTROMETRY LA English DT Article ID ELECTROSPRAY MASS-SPECTROMETRY; INDUCTIVELY-COUPLED PLASMA; BACILLUS-THURINGIENSIS; ZONE-ELECTROPHORESIS; METALLOTHIONEIN ISOFORMS; CIRCULAR-DICHROISM; ION INTERACTIONS; BINDING; LACTONASE; MS AB Increases in the study of protein-metal complexes, as well as in metal displacement in protein-metal complexes under native conditions for optimum catalytic properties in drug research and catalyst design, demands a separation/detection technology that can accurately measure metal displacement and stoichiometry in protein-metal complexes. Both nuclear magnetic resonance (NMR) and X-ray diffraction techniques have been used for this purpose; however, these techniques lack sensitivity. Electrospray ionization mass spectrometry (ESI-MS) using direct infusion offers higher sensitivity than the former techniques and provides molecular distribution of various protein-metal complexes. However, since protein-metal complexes under native conditions usually are dissolved in salt solutions, their direct ESI-MS analysis requires off-line sample clean-up prior to MS analysis to avoid sample suppression during ESI. Moreover, direct infusion of the salty solution promotes nonspecific salt adduct formation by the protein-metal complexes under ESI-MS, which complicates the identification and stoichiometry measurements of the protein-metal complexes. Because of the high mass of protein-metal complexes and lack of sufficient resolution by most mass spectrometers to separate non-specific from specific metal-protein complexes, accurate protein-metal stoichiometry measurements require some form of sample clean up prior to ESI-MS analysis. In this study, we demonstrate that capillary electrophoresis/electrospray ionization in conjunction with a medium-resolution (similar to 10 000) mass spectrometer is an efficient and fast method for the measurement of the stoichiometry of the protein-metal complexes under physiological conditions (pH similar to 7). The metal displacement of Co(2+) to Cd(2+), two metal ions necessary for activation in the monomeric AHL lactonase produced by B. thuringiensis, has been used as a proof of concept. Copyright (c) 2010 John Wiley & Sons, Ltd. C1 Smithsonian Inst, Museum Conservat Inst, Suitland, MD 20746 USA. RP Moini, M (reprint author), Smithsonian Inst, Museum Conservat Inst, 4210 Silver Hill Rd, Suitland, MD 20746 USA. EM MoiniM@SI.edu NR 40 TC 23 Z9 23 U1 2 U2 23 PU JOHN WILEY & SONS LTD PI CHICHESTER PA THE ATRIUM, SOUTHERN GATE, CHICHESTER PO19 8SQ, W SUSSEX, ENGLAND SN 0951-4198 J9 RAPID COMMUN MASS SP JI Rapid Commun. Mass Spectrom. PD SEP PY 2010 VL 24 IS 18 BP 2730 EP 2734 DI 10.1002/rcm.4702 PG 5 WC Biochemical Research Methods; Chemistry, Analytical; Spectroscopy SC Biochemistry & Molecular Biology; Chemistry; Spectroscopy GA 653IN UT WOS:000282082800006 ER PT J AU McGowan, T Cunningham, SL Guzman, HM Mair, JM Guevara, JM Betts, T AF McGowan, Tom Cunningham, Sarah L. Guzman, Hector M. Mair, James M. Guevara, Jose M. Betts, Tanja TI Mangrove forest composition and structure in Las Per las Archipelago, Pacific Panama SO REVISTA DE BIOLOGIA TROPICAL LA English DT Article DE mangrove structure; Rhizophora; Lagtmcularia; Pacific Panama; Las Perlas Archipelago ID CONSERVATION; MANAGEMENT; SEEDLINGS; ECOSYSTEMS; HYPOTHESIS; RESOURCES; DISPERSAL; ECOLOGY; FLORIDA; IMPACT AB Mangrove forest is an important ecosystem that provides many services, but in Panama, as in other countries, they are under threat due to a variety of human activities. Nowadays, large areas of mangroves continue to be lost without been described and lack of management strategies. This study focused on the mangrove structure in the two largest islands, Isla del Rey and Isla San Jose, of Las Perlas Archipelago (LPA), Pacific Panama. Assessment of Landsat satellite imagery revealed loss of mangroves in the LPA of 965ha in the period 1974-1986, and 248ha in the period 1986-2000. The majority of the loss (>77%) from the two study islands was due to timber extraction and agricultural development. In May 2006, permanent plots following the CA RICOMP protocol were established at two sites on Isla del Rey (RI and R2) and one site on Isla San Jose (SJ) where standardized metrics such as species, height and diameter at breast height of adult trees and seedlings were recorded. Forest structure differed at the three sites, although RI and R2 were most similar. At RI. Laguncularia racemosa was the important species and R2 was dominated by Pelliciera rhizophorae. Examination of the forest structure and classified imagery indicated that these sites are spatially dynamic and appear to be rejuvenating. The forest structure would indicate that the sites have been growth-limited previously by human activities and possibly by other factors. SJ was dominated by Rhizophora mangle and appears to have a mature forest with large adult trees and few seedlings. It does not appear to have shown the same extent of spatial regrowth as the other two sites between 1986 and 2000 and is relatively static. The establishment of permanent plots and monitoring will be useful as part of the management plan, as the LPA shows a variety of mangrove structures and could be subject to further coastal development. Rev. Biol. Trop. 58 (3): 857-869. Epub 2010 September 01. C1 [McGowan, Tom; Mair, James M.; Betts, Tanja] Heriot Watt Univ, Sch Life Sci, Ctr Marine Biodivers & Biotechnol, Edinburgh EH14 4AS, Midlothian, Scotland. [Cunningham, Sarah L.] Argyll & Bute Council, Marine & Coastal Dev Unit, Oban PA34 4LF, Argyll, Scotland. [Guzman, Hector M.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Guevara, Jose M.] World Trade Ctr, Environm Resources Management Panama SA, Wtc 08320588, Panama. RP McGowan, T (reprint author), Heriot Watt Univ, Sch Life Sci, Ctr Marine Biodivers & Biotechnol, Edinburgh EH14 4AS, Midlothian, Scotland. EM j.m.mair@hw.ac.uk; sarah.cunningham@argyll-bute.gov.uk; guzmanh@si.edu; waisy2000@yahoo.com NR 54 TC 4 Z9 4 U1 1 U2 9 PU REVISTA DE BIOLOGIA TROPICAL PI SAN JOSE PA UNIVERSIDAD DE COSTA RICA CIUDAD UNIVERSITARIA, SAN JOSE, 00000, COSTA RICA SN 0034-7744 EI 2215-2075 J9 REV BIOL TROP JI Rev. Biol. Trop. PD SEP PY 2010 VL 58 IS 3 BP 857 EP 869 PG 13 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 640SF UT WOS:000281071900006 PM 20737843 ER PT J AU Wernicke, B Davis, JL AF Wernicke, Brian Davis, James L. TI Detecting Large-scale Intracontinental Slow-slip Events (SSEs) Using Geodograms SO SEISMOLOGICAL RESEARCH LETTERS LA English DT Article ID GEODETIC MEASUREMENTS; PLATE BOUNDARY; CONTINUOUS GPS; DEFORMATION; CALIFORNIA C1 [Wernicke, Brian] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Davis, James L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Wernicke, B (reprint author), CALTECH, Div Geol & Planetary Sci, Mail Code 100-23, Pasadena, CA 91125 USA. EM brian@gps.caltech.edu; jdavis@cfa.harvard.edu RI Davis, James/D-8766-2013 OI Davis, James/0000-0003-3057-477X FU NSF [EAR-0810328, EAR-0809195]; Caltech Tectonics Observatory FX This research was supported by NSF Grants EAR-0810328 (BW) and EAR-0809195 (JLD), and by the Caltech Tectonics Observatory. We are grateful to D. L. Anderson and D. J. Stevenson for alerting us to the TBO as a plausible origin of the quasi-biennial signal on the geodogram. NR 16 TC 5 Z9 5 U1 0 U2 5 PU SEISMOLOGICAL SOC AMER PI ALBANY PA 400 EVELYN AVE, SUITE 201, ALBANY, CA 94706-1375 USA SN 0895-0695 EI 1938-2057 J9 SEISMOL RES LETT JI Seismol. Res. Lett. PD SEP-OCT PY 2010 VL 81 IS 5 BP 694 EP 698 DI 10.1785/gssrl.81.5.694 PG 5 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 644ID UT WOS:000281367500003 ER PT J AU Adamski, D Li, H AF Adamski, D. Li, H. TI Three new species of Blastobasinae moths from Beijing, China (Lepidoptera: Gelechioidea, Coleophoridae) SO SHILAP-REVISTA DE LEPIDOPTEROLOGIA LA English DT Article DE Lepidoptera; Gelechioidea; Coleophoridae; Blastobasinae; Holcocerini; morphology; Taxonomy; China AB Three new species of Blastobasinae (Lepidoptera: Gelechioidea: Coleophoridae) are described from Beijing. China as Pseudohypatopa ramusella Adamski & Li, sp. n., Blastobasis sinica Adamski & Li, sp. n., and B. drymosa Adamski & Li, sp. n.. A lectotype for Holcocera anthracographa Meyrick, 1937, is designated. This species is redescribed and is transferred to Pseudohypatopa Sinev, 1986. Photographs of the imagos and illustrations of the male and female genitalia are provided for the identification of these species. C1 [Adamski, D.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. [Li, H.] Nankai Univ, Coll Life Sci, Tianjin 300071, Peoples R China. RP Adamski, D (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, POB 37012,MRC-168, Washington, DC 20013 USA. EM adamskid@si.edu; lihouhun@nankai.edu.cn NR 26 TC 1 Z9 1 U1 0 U2 0 PU SOC HISPANO-LUSO-AMER LEPIDOPTEROLOGIA-SHILAP PI MADRID PA APARTADO DE CORREOS, 331, MADRID, 28080, SPAIN SN 0300-5267 J9 SHILAP-REV. LEPIDOPT JI Shilap-Revista Lepidopterol. PD SEP PY 2010 VL 38 IS 151 BP 341 EP 351 PG 11 WC Entomology SC Entomology GA 673BF UT WOS:000283632500010 ER PT J AU Hacker, BC AF Hacker, Barton C. TI The Complete Soldier: Military Books and Military Culture in Early Stuart England, 1603-1645 SO SIXTEENTH CENTURY JOURNAL LA English DT Book Review C1 [Hacker, Barton C.] Smithsonian Inst, Washington, DC 20560 USA. RP Hacker, BC (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU SIXTEENTH CENTURY JOURNAL PUBL PI KIRKSVILLE PA MC111-L, TRUMAN STATE UNIV, 100 E NORMAL ST, KIRKSVILLE, MO 63501-4211 USA SN 0361-0160 J9 SIXTEENTH CENT J JI Sixt. Century J. PD FAL PY 2010 VL 41 IS 3 BP 838 EP 840 PG 3 WC History SC History GA 678ZX UT WOS:000284130300030 ER PT J AU Clough, GW AF Clough, G. Wayne TI Lest We Forget 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 SEP PY 2010 VL 41 IS 5 BP 28 EP 28 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 641BO UT WOS:000281099300015 ER PT J AU Cheesman, AW Turner, BL Reddy, KR AF Cheesman, Alexander W. Turner, Benjamin L. Reddy, K. Ramesh TI Interaction of Phosphorus Compounds with Anion-Exchange Membranes: Implications for Soil Analysis SO SOIL SCIENCE SOCIETY OF AMERICA JOURNAL LA English DT Article ID MICROBIAL BIOMASS PHOSPHORUS; ORGANIC PHOSPHORUS; EXTRACTION METHODS; RESIN METHODS; SHORT-TERM; ION-SINK; LABILE; FOREST AB Anion exchange membranes are commonly used to measure readily exchangeable and microbial P in soil, yet there is little information on their interactions with organic and condensed inorganic P compounds, which can interfere with interpretation of the results. We addressed this by quantifying the sorption of a range of P compounds to a commonly used anion exchange membrane (551642S, BDH-Prolabo, VWR International, Lutterworth, UK). Sorption and recovery of orthophosphate by the membranes was complete up to 1.17 g P m(-2). The membranes also completely recovered sodium pyrophosphate, glucose 6-phosphate, and adenosine 5'-monophosphate, as well as significant levels (20-60%) of 2-aminoethylphosphonic acid, sodium hexametaphosphate, and sodium phytate. Only sodium pyrophosphate, sodium hexametaphosphate, and D-glucose 6-phosphate were detected subsequently as molybdate-reactive P after elution with 0.25 mol L(-1) H(2)SO(4), however, indicating their hydrolysis in the acid eluant. Solution (31)P nuclear magnetic resonance spectroscopy was used to confirm the stability of the tested compounds when exposed to the membrane and the absence of significant concentrations of orthophosphate as trace contaminants in the compound preparations. Finally, for a series of tropical wetland soils from the Republic of Panama, we found negligible difference in eluted P concentrations determined by molybdate colorimetry and inductively coupled plasma optical emission spectrometry for both unfumigated and hexanol-fumigated samples. We therefore conclude that although organic and condensed inorganic P compounds can be recovered by anion exchange membranes, this is likely to have limited impact on the analysis of soil samples. C1 [Cheesman, Alexander W.; Reddy, K. Ramesh] Univ Florida, Dept Soil & Water Sci, Gainesville, FL 32611 USA. [Turner, Benjamin L.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Cheesman, AW (reprint author), Univ Florida, Dept Soil & Water Sci, 106 Newell Hall, Gainesville, FL 32611 USA. EM cheesman@ufl.edu RI Turner, Benjamin/E-5940-2011; Cheesman, Alexander/H-5918-2013 OI Turner, Benjamin/0000-0002-6585-0722; Cheesman, Alexander/0000-0003-3931-5766 NR 33 TC 17 Z9 17 U1 1 U2 30 PU SOIL SCI SOC AMER PI MADISON PA 677 SOUTH SEGOE ROAD, MADISON, WI 53711 USA SN 0361-5995 J9 SOIL SCI SOC AM J JI Soil Sci. Soc. Am. J. PD SEP-OCT PY 2010 VL 74 IS 5 BP 1607 EP 1612 DI 10.2136/sssaj2009.0295 PG 6 WC Soil Science SC Agriculture GA 650BS UT WOS:000281823100019 ER PT J AU Reef, R Feller, IC Lovelock, CE AF Reef, Ruth Feller, Ilka C. Lovelock, Catherine E. TI Nutrition of mangroves SO TREE PHYSIOLOGY LA English DT Review DE Avicennia; fertilization; nutrient resorption efficiency; Rhizophora; sewage treatment; soil redox potential ID ARBUSCULAR MYCORRHIZAL FUNGI; WATER SULFIDE CONCENTRATIONS; ARID-ZONE FORESTS; RISING SEA-LEVEL; RHIZOPHORA-MANGLE; AVICENNIA-MARINA; NUTRIENT ENRICHMENT; TROPICAL MANGROVE; NITROUS-OXIDE; ORGANIC-CARBON AB Mangrove forests dominate the world's tropical and subtropical coastlines. Similar to other plant communities, nutrient availability is one of the major factors influencing mangrove forest structure and productivity. Many mangrove soils have extremely low nutrient availability, although nutrient availability can vary greatly among and within mangrove forests. Nutrient-conserving processes in mangroves are well developed and include evergreeness, resorption of nutrients prior to leaf fall, the immobilization of nutrients in leaf litter during decomposition, high root/shoot ratios and the repeated use of old root channels. Both nitrogen-use efficiency and nutrient resorption efficiencies in mangroves are amongst the highest recorded for angiosperms. A complex range of interacting abiotic and biotic factors controls the availability of nutrients to mangrove trees, and mangroves are characteristically plastic in their ability to opportunistically utilize nutrients when these become available. Nitrogen and phosphorus have been implicated as the nutrients most likely to limit growth in mangroves. Ammonium is the primary form of nitrogen in mangrove soils, in part as a result of anoxic soil conditions, and tree growth is supported mainly by ammonium uptake. Nutrient enrichment is a major threat to marine ecosystems. Although mangroves have been proposed to protect the marine environment from land-derived nutrient pollution, nutrient enrichment can have negative consequences for mangrove forests and their capacity for retention of nutrients may be limited. C1 [Reef, Ruth; Lovelock, Catherine E.] Univ Queensland, Ctr Marine Studies, St Lucia, Qld 4072, Australia. [Reef, Ruth; Lovelock, Catherine E.] Univ Queensland, Sch Biol Sci, St Lucia, Qld 4072, Australia. [Feller, Ilka C.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Reef, R (reprint author), Univ Queensland, Ctr Marine Studies, St Lucia, Qld 4072, Australia. EM r.reef@uq.edu.au RI Lovelock, Catherine/G-7370-2012; OI Lovelock, Catherine/0000-0002-2219-6855; Feller, Ilka/0000-0002-6391-1608 FU Australian Research Council [DP0774491, DP0986170]; UQ FX This work was supported by awards DP0774491 and DP0986170 from the Australian Research Council and by a UQ Early Career Researcher award to R. R. We thank Prof. Marilyn Ball. NR 184 TC 84 Z9 88 U1 13 U2 114 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0829-318X J9 TREE PHYSIOL JI Tree Physiol. PD SEP PY 2010 VL 30 IS 9 BP 1148 EP 1160 DI 10.1093/treephys/tpq048 PG 13 WC Forestry SC Forestry GA 638UY UT WOS:000280923800010 PM 20566581 ER PT J AU Boedeker, NC Walsh, T Murray, S Bromberg, N AF Boedeker, Nancy C. Walsh, Timothy Murray, Suzan Bromberg, Nancy TI Medical and surgical management of severe inflammation of the nictitating membrane in a Giant Panda (Ailuropoda melanoleuca) SO VETERINARY OPHTHALMOLOGY LA English DT Article DE Ailuropoda melanoleuca; giant panda; membrana nictitans; nictitating membrane; Ursid ID NODULAR FASCIITIS; DOG AB A 10-year-old male giant panda (Ailuropoda melanoleuca) presented for severe, acute swelling and protrusion of the right nictitating membrane, unresponsive to topical therapy. Excisional biopsy of the nictitating membrane and its associated lacrimal gland was elected due to necrosis and friability of the tissue. Histopathology revealed suppurative, necrotizing conjunctivitis and dacryoadenitis. Culture grew Stenotrophomonas maltophila and Enterococcus spp with extensive antibiotic resistance. Treatment with topical and systemic antibiotics based on sensitivity results was initiated. All treatments were well tolerated. Healing was uncomplicated with no recurrence of the lesion and no clinical evidence of keratoconjunctivitis sicca. Ophthalmic exams and Schirmer tear tests performed opportunistically during postoperative anesthetic procedures were unremarkable, confirming that excision of the nictitating membrane had not caused clinically significant detrimental effects. The etiology of this lesion remains undetermined, but trauma is suspected. To the authors' knowledge, this is the first report of nictitating membrane pathology and excision in the giant panda. C1 [Boedeker, Nancy C.; Walsh, Timothy; Murray, Suzan] Smithsonian Inst, Natl Zool Pk, Washington, DC 20008 USA. [Bromberg, Nancy] SouthPaws Vet Specialists & Emergency Ctr, Fairfax, VA 22031 USA. RP Boedeker, NC (reprint author), Smithsonian Inst, Natl Zool Pk, Washington, DC 20008 USA. EM boedekern@si.edu NR 23 TC 0 Z9 0 U1 0 U2 4 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1463-5216 J9 VET OPHTHALMOL JI Vet. Ophthalmol. PD SEP PY 2010 VL 13 SU 1 BP 109 EP 115 PG 7 WC Veterinary Sciences SC Veterinary Sciences GA 646PD UT WOS:000281553600018 PM 20840099 ER PT J AU Mah, C Nizinski, M Lundsten, L AF Mah, Christopher Nizinski, Martha Lundsten, Lonny TI Phylogenetic revision of the Hippasterinae (Goniasteridae; Asteroidea): systematics of deep sea corallivores, including one new genus and three new species (vol 160, pg 266, 2010) SO ZOOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Correction C1 [Mah, Christopher] Natl Museum Nat Hist, Smithsonian Inst Invertebrate Zool, Washington, DC 20013 USA. [Nizinski, Martha] Natl Museum Nat Hist, Natl Marine Fisheries Serv, Natl Systemat Lab, Washington, DC 20013 USA. [Lundsten, Lonny] Monterey Bay Aquarium Res Inst, Video Lab, Moss Landing, CA 95039 USA. RP Mah, C (reprint author), Natl Museum Nat Hist, Smithsonian Inst Invertebrate Zool, MRC 163,POB 37012, Washington, DC 20013 USA. NR 1 TC 0 Z9 0 U1 0 U2 2 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0024-4082 J9 ZOOL J LINN SOC-LOND JI Zool. J. Linn. Soc. PD SEP PY 2010 VL 160 IS 3 BP 620 EP 620 DI 10.1111/j.1096-3642.2010.00703.x PG 1 WC Zoology SC Zoology GA 672QH UT WOS:000283601500010 ER PT J AU Sues, HD AF Sues, Hans-Dieter TI An unusual dinosaur from the Late Cretaceous of Romania and the island rule SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Editorial Material ID HADROSAUROID DINOSAUR C1 Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Sues, HD (reprint author), Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, Washington, DC 20560 USA. EM suesh@si.edu NR 15 TC 1 Z9 1 U1 2 U2 6 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD AUG 31 PY 2010 VL 107 IS 35 BP 15310 EP 15311 DI 10.1073/pnas.1010366107 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 645NT UT WOS:000281468500003 PM 20805479 ER PT J AU Chamorro, ML Holzenthal, RW AF Chamorro, Maria Lourdes Holzenthal, Ralph W. TI Taxonomy and phylogeny of New World Polyplectropus Ulmer, 1905 (Trichoptera: Psychomyioidea: Polycentropodidae) with the description of 39 new species SO ZOOTAXA LA English DT Article DE phylogeny; taxonomy; Neotropics; Nearctric; Bayesian methods; parsimony; classification; cladistics; morphology; Trichoptera; Polycentropodidae; Polyplectropus; new species ID MISSING DATA; COSTA-RICA; TEXAS CADDISFLIES; RECONSTRUCTION; CHARACTERS; AUTAPOMORPHIES; LEPTOCERIDAE; PARSIMONY; INFERENCE; FOSSILS AB The taxonomy of the New World species of Polyplectropus (Ulmer, 1905a) is revised to include detailed male and female diagnoses, descriptions, illustrations, distribution records, and keys to males of all species and species groups. A phylogenetic analysis based on 59 morphological characters, 89 of 92 (97%) New World Polyplectropus species, and 2 outgroup taxa was inferred using parsimony and Bayesian methods, which resulted in minor topological differences. Conflicting estimates of relationship among and within most species groups led to a less resolved Bayesian tree (vs. parsimony tree) due to high variation in rates of change among characters and an overall low number of characters. A new classification for New World Polyplectropus is proposed with revised characterization of 10 recognized species groups, 6 newly established. Four species remain unassigned to species group. A key to genera of New World Polycentropodidae, including a redescription of Polyplectropus is provided. The homology of the male genitalia of Polyplectropus is discussed. Ninety-two species are treated. The following 39 new species are described: Polyplectropus adamsae (Peru), P. alatespinus (Brazil), P. amazonicus (Brazil), P. andinensis (Argentina, Bolivia), P. blahniki (Venezuela), P. bolivianus (Bolivia), P. brasilensis (Brazil), P. brborichorum (Ecuador), P. cressae (Venezuela), P. colombianus (Colombia), P. corniculatus (Peru), P. cuzcoensis (Peru), P. ecuadoriensis (Ecuador), P. flintorum (Venezuela), P. gaesum (Brazil), P. guyanae (Guyana, Venezuela), P. hollyae (Brazil), P. hystricosus (Brazil), P. insularis (Panama), P. juliae (Brazil), P. kanukarum (Guyana), P. maculatus (Venezuela), P. manuensis (Peru), P. matatlanticus (Brazil), P. minensium (Brazil), P. novafriburgensis (Brazil), P. peruvianus (Peru), P. petrae (Brazil), P. pratherae (Brazil), P. puyoensis (Ecuador), P. robertsonae (Bolivia), P. rodmani (Brazil), P. rondoniensis (Brazil), P. tragularius (Brazil), P. tripunctatum (Peru), P. venezolanus (Venezuela), P. woldai (Panama), P. zamoranoensis (Honduras), and P. zuliae (Venezuela). Polyplectropus buchwaldi (Ulmer, 1911) is designated as a nomen dubium. C1 [Chamorro, Maria Lourdes; Holzenthal, Ralph W.] Univ Minnesota, Dept Entomol, St Paul, MN 55108 USA. RP Chamorro, ML (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, MRC 187,POB 37012, Washington, DC 20013 USA. EM lourdes.chamorro@gmail.com; holze001@umn.edu FU University of Minnesota, Graduate School; University of Minnesota Bell Museum of Natural History; University of Minnesota Institute for Global Studies; National Museum of Natural History, Smithsonian Institution; National Science Foundation [DEB-0117772] FX MLC is grateful for the financial support awarded to her as a graduate student: Doctoral Dissertation Fellowship, Educational Opportunity Fellowship (University of Minnesota, Graduate School), Dayton Wilkie Funds, (University of Minnesota Bell Museum of Natural History), Foreign Language Area Scholarship (University of Minnesota Institute for Global Studies), and 10-Week Graduate Student Fellowship (National Museum of Natural History, Smithsonian Institution). This material is based upon work supported by the National Science Foundation Grant No. DEB-0117772 to Holzenthal and Blahnik. NR 123 TC 11 Z9 12 U1 0 U2 1 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD AUG 31 PY 2010 IS 2582 BP 1 EP 252 PG 252 WC Zoology SC Zoology GA 646AL UT WOS:000281507200001 ER PT J AU Benedick, AJ Chang, GQ Birge, JR Chen, LJ Glenday, AG Li, CH Phillips, DF Szentgyorgyi, A Korzennik, S Furesz, G Walsworth, RL Kartner, FX AF Benedick, Andrew J. Chang, Guoqing Birge, Jonathan R. Chen, Li-Jin Glenday, Alexander G. Li, Chih-Hao Phillips, David F. Szentgyorgyi, Andrew Korzennik, Sylvain Furesz, Gabor Walsworth, Ronald L. Kaertner, Franz X. TI Visible wavelength astro-comb SO OPTICS EXPRESS LA English DT Article ID RADIAL-VELOCITY MEASUREMENTS; LASER FREQUENCY COMBS; CM S(-1); PRECISION; CALIBRATION; GHZ; SPECTROGRAPHS; DECELERATION AB We demonstrate a tunable laser frequency comb operating near 420 nm with mode spacing of 20-50 GHz, usable bandwidth of 15 nm and output power per line of similar to 20 nW. Using the TRES spectrograph at the Fred Lawrence Whipple Observatory, we characterize this system to an accuracy below 1m/s, suitable for calibrating high-resolution astrophysical spectrographs used, e.g., in exoplanet studies. (c) 2010 Optical Society of America C1 [Benedick, Andrew J.; Chang, Guoqing; Birge, Jonathan R.; Chen, Li-Jin; Kaertner, Franz X.] MIT, Elect Res Lab, Cambridge, MA 02139 USA. [Glenday, Alexander G.; Li, Chih-Hao; Phillips, David F.; Szentgyorgyi, Andrew; Korzennik, Sylvain; Furesz, Gabor; Walsworth, Ronald L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Glenday, Alexander G.; Walsworth, Ronald L.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. RP Benedick, AJ (reprint author), MIT, Elect Res Lab, 77 Mass Ave, Cambridge, MA 02139 USA. EM andrew_b@mit.edu FU NASA [NNX09AC92G]; NSF [AST-0905214, 0905592] FX This work was funded under NASA award number NNX09AC92G and NSF grants AST-0905214 and 0905592. Andrew J. Benedick and Guoqing Chang contributed equally to this work. NR 21 TC 22 Z9 23 U1 1 U2 17 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1094-4087 J9 OPT EXPRESS JI Opt. Express PD AUG 30 PY 2010 VL 18 IS 18 BP 19175 EP 19184 DI 10.1364/OE.18.019175 PG 10 WC Optics SC Optics GA 653PE UT WOS:000282107900072 PM 20940813 ER PT J AU Banks, ME Byrne, S Galla, K McEwen, AS Bray, VJ Dundas, CM Fishbaugh, KE Herkenhoff, KE Murray, BC AF Banks, Maria E. Byrne, Shane Galla, Kapil McEwen, Alfred S. Bray, Veronica J. Dundas, Colin M. Fishbaugh, Kathryn E. Herkenhoff, Kenneth E. Murray, Bruce C. TI Crater population and resurfacing of the Martian north polar layered deposits SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID MARS; ATMOSPHERE; CAP; EVOLUTION; HISTORY AB Present-day accumulation in the north polar layered deposits (NPLD) is thought to occur via deposition on the north polar residual cap. Understanding current mass balance in relation to current climate would provide insight into the climatic record of the NPLD. To constrain processes and rates of NPLD resurfacing, a search for craters was conducted using images from the Mars Reconnaissance Orbiter Context Camera. One hundred thirty craters have been identified on the NPLD, 95 of which are located within a region defined to represent recent accumulation. High Resolution Imaging Science Experiment images of craters in this region reveal a morphological sequence of crater degradation that provides a qualitative understanding of processes involved in crater removal. A classification system for these craters was developed based on the amount of apparent degradation and infilling and where possible depth/diameter ratios were determined. The temporal and spatial distribution of crater degradation is interpreted to be close to uniform. Through comparison of the size-frequency distribution of these craters with the expected production function, the craters are interpreted to be an equilibrium population with a crater of diameter D meters having a lifetime of similar to 30.75D(1.14) years. Accumulation rates within these craters are estimated at 7.2D(-0.14) mm/yr, which corresponds to values of similar to 3-4 mm/yr and are much higher than rates thought to apply to the surrounding flat terrain. The current crater population is estimated to have accumulated in the last similar to 20 kyr or less. C1 [Banks, Maria E.; Byrne, Shane; Galla, Kapil; McEwen, Alfred S.; Bray, Veronica J.; Dundas, Colin M.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Herkenhoff, Kenneth E.] US Geol Survey, Astrogeol Team, Flagstaff, AZ 86001 USA. [Murray, Bruce C.] CALTECH, Pasadena, CA 91125 USA. RP Banks, ME (reprint author), Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, MRC 315 POB 37012,4th & Independence SW, Washington, DC 20560 USA. EM shane@lpl.arizona.edu RI Byrne, Shane/B-8104-2012; OI Dundas, Colin/0000-0003-2343-7224 FU [NNG06GA48G] FX This work was enabled by Mars Data Analysis grant NNG06GA48G. We gratefully acknowledge the invaluable assistance of the entire HiRISE team, P. S. Russell, K. Tanaka, and B. Ivanov for helpful suggestions, and S. S. Mattson who produced the HiRISE DTMs used in this study. Thoughtful reviews from Asmin Pathare and Nadine Barlow greatly improved the manuscript. NR 39 TC 19 Z9 19 U1 0 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD AUG 28 PY 2010 VL 115 AR E08006 DI 10.1029/2009JE003523 PG 11 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 644XV UT WOS:000281416400001 ER PT J AU Yoo, J Miralda-Escude, J AF Yoo, Jaiyul Miralda-Escude, Jordi TI Gravitational lensing effects on the baryonic acoustic oscillation signature in the redshift-space correlation function SO PHYSICAL REVIEW D LA English DT Article ID LUMINOUS RED GALAXIES; DIGITAL SKY SURVEY; DARK ENERGY; COSMOLOGICAL PARAMETERS; SDSS; EVOLUTION; SCALE; LIGHT; BIAS AB Measurements of the baryonic acoustic oscillation (BAO) peak in the redshift-space correlation function yield the angular diameter distance D-A(z) and the Hubble parameter H(z) as a function of redshift, constraining the properties of dark energy and space curvature. We discuss the perturbations introduced in the galaxy correlation function by gravitational lensing through the effect of magnification bias and its cross correlation with the galaxy density. At the BAO scale, gravitational lensing adds a small and slowly varying component to the galaxy correlation function and does not change its shape significantly, through which the BAO peak is measured. The relative shift in the position of the BAO peak caused by gravitational lensing in the angle-averaged correlation function is 10(-4) at z = 1, rising to 10(-3) at z = 5. Lensing effects are stronger near the line of sight; however, the relative peak shift increases only to 10(-3.3) and 10(-2.4) at z = 1 and z = 2.5, when the galaxy correlation is averaged within 5 degrees of the line of sight (containing only 0.4% of the galaxy pairs in a survey). Furthermore, the lensing contribution can be measured separately and subtracted from the observed correlation at the BAO scale. C1 [Yoo, Jaiyul] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Miralda-Escude, Jordi] Inst Catalana Recerca & Estudis Avancats, Barcelona, Catalonia, Spain. [Miralda-Escude, Jordi] Univ Barcelona, IEEC, Inst Ciencies Cosmos, Barcelona, Catalonia, Spain. RP Yoo, J (reprint author), Harvard Univ, Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jyoo@cfa.harvard.edu OI Miralda-Escude, Jordi/0000-0002-2316-8370 FU Harvard College Observatory; [AYA2006-06341]; [AYA2006-15623-C02-01]; [AYA2009-09745]; [MEC-CSD2007-00060] FX We thank A. Lidz, D. Eisenstein, D. Weinberg, and U. Seljak for useful discussions. J. Y. is supported by the Harvard College Observatory under the Donald H. Menzel fund. J. M. is supported by Spanish Grant Nos. AYA2006-06341, AYA2006-15623-C02-01, AYA2009-09745 and MEC-CSD2007-00060. NR 36 TC 3 Z9 3 U1 0 U2 0 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1550-7998 EI 1550-2368 J9 PHYS REV D JI Phys. Rev. D PD AUG 25 PY 2010 VL 82 IS 4 AR 043527 DI 10.1103/PhysRevD.82.043527 PG 7 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 642OZ UT WOS:000281226900001 ER PT J AU Vidal, N Marin, J Morini, M Donnellan, S Branch, WR Thomas, R Vences, M Wynn, A Cruaud, C Hedges, SB AF Vidal, Nicolas Marin, Julie Morini, Marina Donnellan, Steve Branch, William R. Thomas, Richard Vences, Miguel Wynn, Addison Cruaud, Corinne Hedges, S. Blair TI Blindsnake evolutionary tree reveals long history on Gondwana SO BIOLOGY LETTERS LA English DT Article DE biogeography; squamates; snakes; dispersal; vicariance ID ORIGIN; PALEOGEOGRAPHY; TYPHLOPIDAE; HYPOTHESES; PHYLOGENY; SERPENTES; SNAKES; FAMILY AB Worm-like snakes (scolecophidians) are small, burrowing species with reduced vision. Although largely neglected in vertebrate research, knowledge of their biogeographical history is crucial for evaluating hypotheses of snake origins. We constructed a molecular dataset for scolecophidians with detailed sampling within the largest family, Typhlopidae (blindsnakes). Our results demonstrate that scolecophidians have had a long Gondwanan history, and that their initial diversification followed a vicariant event: the separation of East and West Gondwana approximately 150 Ma. We find that the earliest blindsnake lineages, representing two new families described here, were distributed on the palaeolandmass of India+Madagascar named here as Indigascar. Their later evolution out of Indigascar involved vicariance and several oceanic dispersal events, including a westward transatlantic one, unexpected for burrowing animals. The exceptional diversification of scolecophidians in the Cenozoic was probably linked to a parallel radiation of prey (ants and termites) as well as increased isolation of populations facilitated by their fossorial habits. C1 [Vidal, Nicolas; Marin, Julie; Morini, Marina] Museum Natl Hist Nat, Dept Systemat & Evolut, UMR 7138, F-75231 Paris, France. [Donnellan, Steve] S Australian Museum, Adelaide, SA 5000, Australia. [Donnellan, Steve] Univ Adelaide, Australian Ctr Evolutionary Biol & Biodivers, Adelaide, SA 5005, Australia. [Branch, William R.] Bayworld, ZA-6013 Humewood, South Africa. [Thomas, Richard] Univ Puerto Rico, Dept Biol, San Juan, PR 00931 USA. [Vences, Miguel] Tech Univ Carolo Wilhelmina Braunschweig, Inst Zool, D-38106 Braunschweig, Germany. [Wynn, Addison] Smithsonian Inst, Natl Museum Amer Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. [Cruaud, Corinne] Genoscope, Ctr Natl Sequencage, F-91057 Evry, France. [Hedges, S. Blair] Penn State Univ, Dept Biol, Mueller Lab 208, University Pk, PA 16802 USA. RP Vidal, N (reprint author), Museum Natl Hist Nat, Dept Systemat & Evolut, UMR 7138, CP 26,57 Rue Cuvier, F-75231 Paris, France. EM nvidal@mnhn.fr; sbh1@psu.edu RI Donnellan, Stephen/F-2442-2013; OI Donnellan, Stephen/0000-0002-5448-3226; Vences, Miguel/0000-0003-0747-0817 FU Service de Systematique moleculaire du Museum National d'Histoire Naturelle; NASA Astrobiology Institute; US National Science Foundation; Australian Department for the Environment, Water, Heritage; Arts' CERF; Consortium National de Recherche en Genomique, Genoscope FX This work was funded by grants from the Service de Systematique moleculaire du Museum National d'Histoire Naturelle to N.V., the NASA Astrobiology Institute and US National Science Foundation to S. B. H., the Australian Department for the Environment, Water, Heritage and the Arts' CERF programme to S. C. D. and by the Consortium National de Recherche en Genomique, Genoscope. We thank E. Rochel for laboratory assistance and those persons and institutions who contributed some of the tissue and DNA samples used in this study, or assisted us in the field: K. Aplin, A. Bauer, C. Austin, L. Chirio, C. Cicero (MVZ), K. Coate, R. Crombie, K. Daoues, D. Dittmann (LSUMZ), P. Doughty, J. Feinstein (AMNH, Ambrose-Monnell), E. Greenbaum, C. Hass, T. Heger, J. Lazell, C. Marty, G. Mayer, R. Murphy (ROM), R. Platenberg, N. Puillandre, S. Richards, C. Ross, S. Thomson, S. Trape, USNM, J. Vindum (CAS), L. Vitt, L. Whitsed and E. Wikramanayake. K. P. Schliep helped with Multidivtime and J. S. Keogh commented on the manuscript. NR 21 TC 55 Z9 59 U1 1 U2 11 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 1744-9561 EI 1744-957X J9 BIOL LETTERS JI Biol. Lett. PD AUG 23 PY 2010 VL 6 IS 4 BP 558 EP 561 DI 10.1098/rsbl.2010.0220 PG 4 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 623GB UT WOS:000279725700033 PM 20356885 ER PT J AU Staines, CL AF Staines, C. L. TI A review of the genus Oxychalepus Uhmann, 1937 (Coleoptera: Chrysomelidae: Cassidinae) SO ZOOTAXA LA English DT Article DE Oxychalepus; Chrysomelidae; Cassidinae; key to species; new species ID BEETLES COLEOPTERA; COMMUNITY AB The species of Oxychalepus Uhmann, 1937 are reviewed. Thirteen species are treated as valid. Oxychalepus alienus (Baly, 1885) is removed from synonymy; O. angulatus from Argentina and Bolivia is described as new; O. insignatus (Chapuis, 1877) is reinstated to full species status; O. trispinosus (Pic, 1931) is treated as incertae sedis. All species are illustrated and a key to the species is presented. C1 Natl Museum Nat Hist, Dept Entomol, Smithsonian Inst, Washington, DC 20013 USA. RP Staines, CL (reprint author), Natl Museum Nat Hist, Dept Entomol, Smithsonian Inst, MRC 187,POB 37012, Washington, DC 20013 USA. EM stainesc@si.edu NR 88 TC 0 Z9 0 U1 0 U2 0 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD AUG 23 PY 2010 IS 2573 BP 35 EP 56 PG 22 WC Zoology SC Zoology GA 641ZP UT WOS:000281172600002 ER PT J AU Oppenheimer, BD Dave, R Keres, D Fardal, M Katz, N Kollmeier, JA Weinberg, DH AF Oppenheimer, Benjamin D. Dave, Romeel Keres, Dusan Fardal, Mark Katz, Neal Kollmeier, Juna A. Weinberg, David H. TI Feedback and recycled wind accretion: assembling the z=0 galaxy mass function SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Review DE hydrodynamics; methods: numerical; galaxies: evolution; galaxies: formation; intergalactic medium; galaxies: luminosity function; mass function ID STAR-FORMING GALAXIES; ACTIVE GALACTIC NUCLEI; LYMAN BREAK GALAXIES; LAMBDA-CDM UNIVERSE; DARK-MATTER HALOES; LUMINOSITY FUNCTION; INTERGALACTIC MEDIUM; BLACK-HOLES; COSMOLOGICAL SIMULATIONS; METALLICITY RELATION AB We analyse cosmological hydrodynamic simulations that include theoretically and observationally motivated prescriptions for galactic outflows. If these simulated winds accurately represent winds in the real Universe, then material previously ejected in winds provides the dominant source of gas infall for new star formation at redshifts z < 1. This recycled wind accretion, or wind mode, provides a third physically distinct accretion channel in addition to the 'hot' and 'cold' modes emphasized in recent theoretical studies. The recycling time of wind material (t(rec)) is shorter in higher mass systems owing to the interaction between outflows and the increasingly higher gas densities in and around higher mass haloes. This differential recycling plays a central role in shaping the present-day galaxy stellar mass function (GSMF), because declining t(rec) leads to increasing wind mode galaxy growth in more massive haloes. For the three feedback models explored, the wind mode dominates above a threshold mass that primarily depends on wind velocity; the shape of the GSMF therefore can be directly traced back to the feedback prescription used. If we remove all particles that were ever ejected in a wind, then the predicted GSMFs are much steeper than observed. In this case, galaxy masses are suppressed both by the ejection of gas from galaxies and by the hydrodynamic heating of their surroundings, which reduces subsequent infall. With wind recycling included, the simulation that incorporates our favoured momentum-driven wind scalings reproduces the observed GSMF for stellar masses 109 M(circle dot) < M < 5 x 1010 M(circle dot). At higher masses, wind recycling leads to excessive galaxy masses and star formation rates relative to observations. In these massive systems, some quenching mechanism must suppress not only the direct accretion from the primordial intergalactic medium but the re-accretion of gas ejected from star-forming galaxies. In short, as has long been anticipated, the form of the GSMF is governed by outflows; the unexpected twist here for our simulated winds is that it is not primarily the ejection of material but how the ejected material is re-accreted that governs the GSMF. C1 [Oppenheimer, Benjamin D.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Oppenheimer, Benjamin D.; Dave, Romeel] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. [Fardal, Mark; Katz, Neal] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Kollmeier, Juna A.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [Weinberg, David H.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Weinberg, David H.] Inst Adv Study, Princeton, NJ 08450 USA. [Keres, Dusan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Oppenheimer, BD (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. EM oppenheimer@strw.leidenuniv.nl FU NASA [HST-AR-10946]; AMIAS FX We thank the referee, Avishai Dekel, for numerous suggestions that improved and clarified the paper. The authors also wish to thank Ari Maller, Kristian Finlator, Jared Gabor, Molly Peeples, Joop Schaye, Craig Booth, Marcel Haas, Ryan Quadri, Rob Wiersma, George Becker and Richard Bower for encouraging discussion related to this research. The simulations run on the Intel 64 Linux Cluster Abe Supercluster at the National Center for Supercomputing Applications were greatly aided by the support staff there by providing us with dedicated nodes. We also thank the support staff for the ICE SGI cluster at the University of Arizona and Craig West at the Eagle Opteron cluster at the University of Massachusetts. Support for this work was provided by NASA through grant number HST-AR-10946 from the Space Telescope Science Institute. DHW acknowledges the hospitality of the Institute for Advanced Study and the support of an AMIAS Membership. NR 101 TC 215 Z9 215 U1 0 U2 1 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD AUG 21 PY 2010 VL 406 IS 4 BP 2325 EP 2338 DI 10.1111/j.1365-2966.2010.16872.x PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 635RA UT WOS:000280672600015 ER PT J AU Coe, MJ Bird, AJ Buckley, DAH Corbet, RHD Dean, AJ Finger, M Galache, JL Haberl, F McBride, VA Negueruela, I Schurch, M Townsend, LJ Udalski, A Wilms, J Zezas, A AF Coe, M. J. Bird, A. J. Buckley, D. A. H. Corbet, R. H. D. Dean, A. J. Finger, M. Galache, J. L. Haberl, F. McBride, V. A. Negueruela, I. Schurch, M. Townsend, L. J. Udalski, A. Wilms, J. Zezas, A. TI INTEGRAL deep observations of the Small Magellanic Cloud SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: neutron; X-rays: binaries ID X-RAY BINARIES; STAR-FORMATION; SMC REGION; CATALOG; POPULATION; GALAXIES; SMC-X-1; LONG AB Deep observations of the Small Magellanic Cloud (SMC) and region were carried out in the hard X-ray band by the INTEGRAL observatory in 2008-2009. The field of view of the instrument permitted simultaneous coverage of the entire SMC and the eastern end of the Magellanic Bridge. In total, INTEGRAL detected seven sources in the SMC and five in the Magellanic Bridge; the majority of the sources were previously unknown systems. Several of the new sources were detected undergoing bright X-ray outbursts and all the sources exhibited transient behaviour except the supergiant system SMC X-1. They are all thought to be high-mass X-ray binary systems in which the compact object is a neutron star. C1 [Coe, M. J.; Bird, A. J.; Dean, A. J.; McBride, V. A.; Schurch, M.; Townsend, L. J.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Buckley, D. A. H.] S African Astron Observ, ZA-7935 Cape Town, South Africa. [Corbet, R. H. D.] Univ Maryland Baltimore Cty, Dept Astron, NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Finger, M.] Natl Space Sci & Technol Ctr, Huntsville, AL 35805 USA. [Galache, J. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Haberl, F.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Negueruela, I.] Univ Alicante, Dept Fis Ingn Sistemas & Teoria Seal, E-03080 Alicante, Spain. [Schurch, M.] Univ Cape Town, ACGC, ZA-7701 Rondebosch, South Africa. [Udalski, A.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. [Wilms, J.] Univ Erlangen Nurnberg, Dr Karl Remeis Observ, D-96049 Bamberg, Germany. [Wilms, J.] Univ Erlangen Nurnberg, ECAP, D-96049 Bamberg, Germany. [Zezas, A.] Fdn Res & Technol, IESL, Iraklion 71110, Crete, Greece. RP Coe, MJ (reprint author), Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. EM mjcoe@soton.ac.uk RI Wilms, Joern/C-8116-2013; Negueruela, Ignacio/L-5483-2014; Zezas, Andreas/C-7543-2011; OI Wilms, Joern/0000-0003-2065-5410; Negueruela, Ignacio/0000-0003-1952-3680; Zezas, Andreas/0000-0001-8952-676X; Haberl, Frank/0000-0002-0107-5237 FU Polish MNiSW [N20303032/4275]; University of Southampton FX The OGLE project was partially supported by the Polish MNiSW grant N20303032/4275. LJT is supported by a Mayflower Scholarship from the University of Southampton. NR 32 TC 7 Z9 7 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD AUG 21 PY 2010 VL 406 IS 4 BP 2533 EP 2539 DI 10.1111/j.1365-2966.2010.16844.x PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 635RA UT WOS:000280672600030 ER PT J AU Lueker, M Reichardt, CL Schaffer, KK Zahn, O Ade, PAR Aird, KA Benson, BA Bleem, LE Carlstrom, JE Chang, CL Cho, HM Crawford, TM Crites, AT de Haan, T Dobbs, MA George, EM Hall, NR Halverson, NW Holder, GP Holzapfel, WL Hrubes, JD Joy, M Keisler, R Knox, L Lee, AT Leitch, EM McMahon, JJ Mehl, J Meyer, SS Mohr, JJ Montroy, TE Padin, S Plagge, T Pryke, C Ruhl, JE Shaw, L Shirokoff, E Spieler, HG Stalder, B Staniszewski, Z Stark, AA Vanderlinde, K Vieira, JD Williamson, R AF Lueker, M. Reichardt, C. L. Schaffer, K. K. Zahn, O. Ade, P. A. R. Aird, K. A. Benson, B. A. Bleem, L. E. Carlstrom, J. E. Chang, C. L. Cho, H. -M. Crawford, T. M. Crites, A. T. de Haan, T. Dobbs, M. A. George, E. M. Hall, N. R. Halverson, N. W. Holder, G. P. Holzapfel, W. L. Hrubes, J. D. Joy, M. Keisler, R. Knox, L. Lee, A. T. Leitch, E. M. McMahon, J. J. Mehl, J. Meyer, S. S. Mohr, J. J. Montroy, T. E. Padin, S. Plagge, T. Pryke, C. Ruhl, J. E. Shaw, L. Shirokoff, E. Spieler, H. G. Stalder, B. Staniszewski, Z. Stark, A. A. Vanderlinde, K. Vieira, J. D. Williamson, R. TI MEASUREMENTS OF SECONDARY COSMIC MICROWAVE BACKGROUND ANISOTROPIES WITH THE SOUTH POLE TELESCOPE SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic background radiation; cosmological parameters; cosmology: observations; galaxies: clusters: intracluster medium; large-scale structure of universe ID ANGULAR POWER SPECTRUM; STAR-FORMING GALAXIES; EXTRAGALACTIC SOURCES; DUST EMISSION; CLUSTERS; PROBE; CMB; SUBMILLIMETER; CAMERA; TEMPERATURE AB We report cosmic microwave background (CMB) power-spectrum measurements from the first 100 deg(2) field observed by the South Pole Telescope (SPT) at 150 and 220 GHz. On angular scales where the primary CMB anisotropy is dominant, l less than or similar to 3000, the SPT power spectrum is consistent with the standard Lambda CDM cosmology. On smaller scales, we see strong evidence for a point-source contribution, consistent with a population of dusty, star-forming galaxies. After we mask bright point sources, anisotropy power on angular scales of 3000 < l < 9500 is detected with a signal-to-noise ratio greater than or similar to 50 at both frequencies. We combine the 150 and 220 GHz data to remove the majority of the point-source power and use the point-source-subtracted spectrum to detect Sunyaev-Zel'dovich (SZ) power at 2.6 sigma. At l = 3000, the SZ power in the subtracted bandpowers is 4.2 +/- 1.5 mu K-2, which is significantly lower than the power predicted by a fiducial model using WMAP5 cosmological parameters. This discrepancy may suggest that contemporary galaxy cluster models overestimate the thermal pressure of intracluster gas. Alternatively, this result can be interpreted as evidence for lower values of sigma(8). When combined with an estimate of the kinetic SZ contribution, the measured SZ amplitude shifts sigma(8) from the primary CMB anisotropy derived constraint of 0.794 +/- 0.028 down to 0.773 +/- 0.025. The uncertainty in the constraint on sigma(8) from this analysis is dominated by uncertainties in the theoretical modeling required to predict the amplitude of the SZ power spectrum for a given set of cosmological parameters. C1 [Lueker, M.; Reichardt, C. L.; Benson, B. A.; Cho, H. -M.; George, E. M.; Holzapfel, W. L.; Lee, A. T.; Mehl, J.; Plagge, T.; Shirokoff, E.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Schaffer, K. K.; Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Crawford, T. M.; Crites, A. T.; Keisler, R.; Leitch, E. M.; McMahon, J. J.; Meyer, S. S.; Padin, S.; Pryke, C.; Vieira, J. D.; Williamson, R.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Schaffer, K. K.; Benson, B. A.; Carlstrom, J. E.; Chang, C. L.; McMahon, J. J.; Meyer, S. S.; Pryke, C.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Zahn, O.] Univ Calif Berkeley, Lawrence Berkeley Natl Labs, Dept Phys, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA. [Ade, P. A. R.] Cardiff Univ, Dept Phys & Astron, Cardiff CF24 3YB, S Glam, Wales. [Bleem, L. E.; Carlstrom, J. E.; Keisler, R.; Meyer, S. S.; Vieira, J. D.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. [Carlstrom, J. E.; Crawford, T. M.; Crites, A. T.; Leitch, E. M.; Meyer, S. S.; Padin, S.; Pryke, C.; Williamson, R.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [de Haan, T.; Dobbs, M. A.; Holder, G. P.; Shaw, L.; Vanderlinde, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Hall, N. R.; Knox, L.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Halverson, N. W.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Halverson, N. W.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA. [Joy, M.] NASA, George C Marshall Space Flight Ctr, Dept Space Sci, Huntsville, AL 35812 USA. [Lee, A. T.; Spieler, H. G.] Univ Calif Berkeley, Lawrence Berkeley Lab, Div Phys, Berkeley, CA 94720 USA. [McMahon, J. J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Mohr, J. J.] Univ Munich, Dept Phys, D-81679 Munich, Germany. [Mohr, J. J.] Excellence Cluster Univ, D-85748 Garching, Germany. [Mohr, J. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Montroy, T. E.; Ruhl, J. E.; Staniszewski, Z.] Case Western Reserve Univ, Ctr Educ & Res Cosmol & Astrophys, Dept Phys, Cleveland, OH 44106 USA. [Shaw, L.] Yale Univ, Dept Phys, New Haven, CT 06520 USA. [Stalder, B.; Stark, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Lueker, M (reprint author), Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. EM lueker@socrates.berkeley.edu RI Williamson, Ross/H-1734-2015; Holzapfel, William/I-4836-2015; OI Williamson, Ross/0000-0002-6945-2975; Aird, Kenneth/0000-0003-1441-9518; Reichardt, Christian/0000-0003-2226-9169; Stark, Antony/0000-0002-2718-9996 FU National Science Foundation (NSF) Office of Polar Programs; United States Antarctic Program; Raytheon Polar Services Company; National Science Foundation [ANT-0638937, ANT-0130612]; NSF Physics Frontier Center [PHY-0114422]; Kavli Foundation; Gordon and Betty Moore Foundation; National Sciences and Engineering Research Council of Canada; Quebec Fonds de recherche sur la nature et les technologies; Canadian Institute for Advanced Research; KICP; Berkeley Center for Cosmological Physics; Fermi; GAAN; Miller Institute for Basic Research in Science, University of California Berkeley; Alfred P. Sloan; Office of Science of the U.S. Department of Energy [DE-AC02-05CH11231]; NASA Office of Space Science FX The SPT team gratefully acknowledges the contributions to the design and construction of the telescope by S. Busetti, E. Chauvin, T. Hughes, P. Huntley, and E. Nichols and his team of iron workers. We also thank the National Science Foundation (NSF) Office of Polar Programs, the United States Antarctic Program, and the Raytheon Polar Services Company for their support of the project. We are grateful for professional support from the staff of the South Pole station. We thank T. M. Lanting, J. Leong, A. Loehr, W. Lu, M. Runyan, D. Schwan, M. Sharp, and C. Greer for their early contributions to the SPT project, J. Joseph and C. Vu for their contributions to the electronics, and P. Ralph for his useful discussions and insights.; The SPT is supported by the National Science Foundation through grants ANT-0638937 and ANT-0130612. Partial support is also provided by the NSF Physics Frontier Center grant PHY-0114422 to the Kavli Institute of Cosmological Physics at the University of Chicago, the Kavli Foundation, and the Gordon and Betty Moore Foundation. The McGill group acknowledges funding from the National Sciences and Engineering Research Council of Canada, the Quebec Fonds de recherche sur la nature et les technologies, and the Canadian Institute for Advanced Research. The following individuals acknowledge additional support: K.K.S. and B.A.B. from a KICP Fellowship, O.Z. from a Berkeley Center for Cosmological Physics Fellowship, J.J.M. from a Fermi Fellowship, Z.S. from a GAAN Fellowship, and A.T.L. from the Miller Institute for Basic Research in Science, University of California Berkeley. N.W.H. acknowledges support from an Alfred P. Sloan Research Fellowship.; This research used resources of the National Energy Research Scientific Computing Center, which is supported by the Office of Science of the U. S. Department of Energy under Contract no. DE-AC02-05CH11231. Some of the results in this paper have been derived using the HEALPix (Gorski et al. 2005) package. We acknowledge the use of the Legacy Archive for Microwave Background Data Analysis (LAMBDA). Support for LAMBDA is provided by the NASA Office of Space Science. NR 60 TC 117 Z9 117 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 AUG 20 PY 2010 VL 719 IS 2 BP 1045 EP 1066 DI 10.1088/0004-637X/719/2/1045 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 635LU UT WOS:000280658000005 ER PT J AU Kelly, BC Vestergaard, M Fan, XH Hopkins, P Hernquist, L Siemiginowska, A AF Kelly, Brandon C. Vestergaard, Marianne Fan, Xiaohui Hopkins, Philip Hernquist, Lars Siemiginowska, Aneta TI CONSTRAINTS ON BLACK HOLE GROWTH, QUASAR LIFETIMES, AND EDDINGTON RATIO DISTRIBUTIONS FROM THE SDSS BROAD-LINE QUASAR BLACK HOLE MASS FUNCTION SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; galaxies: active; galaxies: luminosity function, mass function; galaxies: nuclei; galaxies: statistics; quasars: general ID ACTIVE GALACTIC NUCLEI; DIGITAL-SKY-SURVEY; ACCRETION-DISK INSTABILITIES; HOST GALAXY MORPHOLOGIES; MICROQUASAR GRS 1915+105; FALL EQUATORIAL STRIPE; SELF-REGULATED GROWTH; COLOR-SELECTED SAMPLE; SINGLE-EPOCH SPECTRA; RAY SELECTED AGN AB We present an estimate of the black hole mass function of broad-line quasars (BLQSOs) that self-consistently corrects for incompleteness and the statistical uncertainty in the mass estimates, based on a sample of 9886 quasars at 1 < z < 4.5 drawn from the Sloan Digital Sky Survey (SDSS). We find evidence for "cosmic downsizing" of black holes in BLQSOs, where the peak in their number density shifts to higher redshift with increasing black hole mass. The cosmic mass density for black holes seen as BLQSOs peaks at z similar to 2. We estimate the completeness of the SDSS as a function of the black hole mass and Eddington ratio, and find that at z > 1 it is highly incomplete at MBH less than or similar to 10(9) M-circle dot and L/L-Edd less than or similar to 0.5. We estimate a lower limit on the lifetime of a single BLQSO phase to be t(BL) > 150 +/- 15 Myr for black holes at z = 1 with a mass of M-BH = 10(9) M-circle dot, and we constrain the maximum mass of a black hole in a BLQSO to be similar to 3 x 10(10) M-circle dot. Our estimated distribution of BLQSO Eddington ratios peaks at L/L-Edd similar to 0.05 and has a dispersion of similar to 0.4 dex, implying that most BLQSOs are not radiating at or near the Eddington limit; however, the location of the peak is subject to considerable uncertainty. The steep increase in number density of BLQSOs toward lower Eddington ratios is expected if the BLQSO accretion rate monotonically decays with time. Furthermore, our estimated lifetime and Eddington ratio distributions imply that the majority of the most massive black holes spend a significant amount of time growing in an earlier obscured phase, a conclusion which is independent of the unknown obscured fraction. These results are consistent with models for self-regulated black hole growth, at least for massive systems at z > 1, where the BLQSO phase occurs at the end of a fueling event when black hole feedback unbinds the accreting gas, halting the accretion flow. C1 [Kelly, Brandon C.; Hernquist, Lars; Siemiginowska, Aneta] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Vestergaard, Marianne; Fan, Xiaohui] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. [Fan, Xiaohui] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Hopkins, Philip] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Vestergaard, Marianne] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-1168 Copenhagen, Denmark. RP Kelly, BC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM bckelly@cfa.harvard.edu RI Vestergaard, Marianne/M-5247-2014 OI Vestergaard, Marianne/0000-0001-9191-9837 FU NASA [HF-01220.01, HF-51243.01, NAS 5-26555]; Space Telescope Science Institute; NSF [AST-0806861]; Packard Fellowship for Science and Engineering; John Simon Guggenheim Memorial Fellowship; Max Planck Society; Danish National Research Foundation FX We thank Yue Shen, Priyamvada Natarajan, Martin Elvis, and Charles Steinhardt for helpful discussions and comments on this paper, Mark Ammons and Aleks Diamond-Stanic for helpful discussions, and the anonymous referee for a careful reading and comments that lead to improvement of this work. B.K. acknowledges support by NASA through Hubble Fellowship grants HF-01220.01 and HF-51243.01 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. M.V. acknowledges financial support through grants HST-AR-10691, HST-GO-10417, and HST-GO-10833 from NASA through the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. X.F. acknowledges support by NSF grant AST-0806861, a Packard Fellowship for Science and Engineering, a John Simon Guggenheim Memorial Fellowship and the Max Planck Society. The Dark Cosmology Centre is funded by the Danish National Research Foundation. NR 164 TC 108 Z9 110 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2010 VL 719 IS 2 BP 1315 EP 1334 DI 10.1088/0004-637X/719/2/1315 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 635LU UT WOS:000280658000022 ER PT J AU Grady, CA Hamaguchi, K Schneider, G Stecklum, B Woodgate, BE McCleary, JE Williger, GM Sitko, ML Menard, F Henning, T Brittain, S Troutmann, M Donehew, B Hines, D Wisniewski, JP Lynch, DK Russell, RW Rudy, RJ Day, AN Shenoy, A Wilner, D Silverstone, M Bouret, JC Meusinger, H Clampin, M Kim, S Petre, R Sahu, M Endres, M Collins, KA AF Grady, C. A. Hamaguchi, K. Schneider, G. Stecklum, B. Woodgate, B. E. McCleary, J. E. Williger, G. M. Sitko, M. L. Menard, F. Henning, Th Brittain, S. Troutmann, M. Donehew, B. Hines, D. Wisniewski, J. P. Lynch, D. K. Russell, R. W. Rudy, R. J. Day, A. N. Shenoy, A. Wilner, D. Silverstone, M. Bouret, J. -C. Meusinger, H. Clampin, M. Kim, S. Petre, R. Sahu, M. Endres, M. Collins, K. A. TI LOCATING THE ACCRETION FOOTPRINT ON A HERBIG Ae STAR: MWC 480 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: jets and outflows; protoplanetary disks; stars: individual (MWC 480); ultraviolet: stars; X-rays: stars ID T-TAURI-STARS; X-RAY-EMISSION; PRE-MAIN-SEQUENCE; 2-DIMENSIONAL RADIATIVE-TRANSFER; YOUNG STELLAR OBJECTS; INFRARED FILTER SET; ULTRAVIOLET-SPECTROSCOPIC-EXPLORER; AE/BE STARS; PROTOSTELLAR ENVELOPES; PROTOPLANETARY DISKS AB Accretion is a fundamental process which establishes the dynamics of the protoplanetary disk and the final properties of the forming star. In solar-type stars, the star-disk coupling is determined by the magnetic field structure, which is responsible for funneling material from the disk midplane to higher latitudes on the star. Here, we use pan-chromatic data for the Herbig Ae star MWC 480 to address whether similar processes occur in intermediate-mass stars. MWC 480 has X-ray emission typical of actively accreting Herbig Ae stars, but with similar to 10x more photoelectric absorption than expected from optical and FUV data. We consider three sources for the absorption: the disk, absorption in a wind or jet, and accretion. While we detect the disk in scattered light in a re-analysis of archival Hubble Space Telescope data, the data are consistent with grazing illumination of the dust disk. We find that MWC 480's disk is stratified, geometrically thin, and is not responsible for the observed photoelectric absorption. MWC 480 drives a bipolar jet, but with a mass-loss rate that is low compared to other Herbig Ae stars, where the outflow is more favorably oriented and enhanced photoelectric absorption is not seen. This excludes a jet or wind origin for the enhanced photoelectric absorption. We compare MWC 480's OVI emission with other Herbig Ae stars. The distribution of the emission in inclination, and lack of a correlation of profile shape and system inclination excludes equatorially confined accretion for the FUSE Herbig Ae stars. The photoelectric absorption data further suggest that the accretion footprint on MWC 480 and other Herbig Ae stars is located at high-temperate, rather than polar, latitudes. These findings support the presence of funneled accretion in MWC 480 and Herbig Ae stars, strengthening the parallel to T Tauri stars. C1 [Grady, C. A.; Silverstone, M.] Eureka Sci, Oakland, CA 96002 USA. [Hamaguchi, K.] NASA, GSFC, CRESST, Greenbelt, MD 20771 USA. [Hamaguchi, K.] NASA, GSFC, Xray Astrophys Lab, Greenbelt, MD 20771 USA. [Hamaguchi, K.] Univ Maryland, Dept Phys, Baltimore, MD 21250 USA. [Hamaguchi, K.] NASA, Goddard Space Flight Ctr, Goddard Ctr Astrobiol, Greenbelt, MD 20771 USA. [Schneider, G.; Kim, S.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Stecklum, B.; Meusinger, H.] Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany. [Grady, C. A.; Woodgate, B. E.; Clampin, M.] NASA, Goddard Space Flight Ctr, ExoPlanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA. [McCleary, J. E.] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA. [Williger, G. M.; Collins, K. A.] Univ Louisville, Dept Phys, Louisville, KY 40292 USA. [Williger, G. M.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Williger, G. M.] Univ Nice, UMR 6525, Lab Fizeau, F-06108 Nice 2, France. [Sitko, M. L.; Hines, D.] Space Sci Inst, Boulder, CO 80301 USA. [Sitko, M. L.] Univ Cincinnati, Dept Phys, Cincinnati, OH 45221 USA. [Menard, F.] UJF, CNRS, UMR 5571, Lab Astrophys Grenoble, Paris, France. [Henning, Th] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Brittain, S.; Troutmann, M.; Donehew, B.] Clemson Univ, Dept Phys & Astron, Clemson, SC 29634 USA. [Wisniewski, J. P.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Lynch, D. K.; Russell, R. W.; Rudy, R. J.] Aerosp Corp, Los Angeles, CA 90009 USA. [Shenoy, A.] NASA, Goddard Space Flight Ctr, Summer High Sch Intern, Rockville, MD 20850 USA. [Shenoy, A.] NASA, Goddard Space Flight Ctr, Thomas Wootton High Sch, Rockville, MD 20850 USA. [Wilner, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bouret, J. -C.] NASA, Goddard Space Flight Ctr, Lab Observat Cosmol, Greenbelt, MD 20771 USA. [Bouret, J. -C.] Univ Provence, CNRS, Lab Astrophy Marseille, F-13376 Marseille 12, France. [Petre, R.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA. [Sahu, M.] US Patent & Trademark Off, Alexandria, VA 22314 USA. [Endres, M.] Wyle Informat Syst, Mclean, VA 22102 USA. [Endres, M.] Endres Gamebit Ltd, London SE5 7HS, England. RP Grady, CA (reprint author), Eureka Sci, 2452 Delmer,Suite 100, Oakland, CA 96002 USA. EM jwisnie@u.washington.edu RI Brittain, Sean/K-9001-2012; Woodgate, Bruce/D-2970-2012; Clampin, mark/D-2738-2012 OI Brittain, Sean/0000-0001-5638-1330; FU Kentucky Space Grant Consortium; NASA [NAS5-26555, NNG05EA89P, NAS5-32985, NAS8-03060, HST-GO-10177, NAS 5-26555, 399131.02.06.02.32, NNX08AH90G, NNH06CC28C, NNX09AC73G]; Chandra X-ray Observatory Center [09200520]; NASA Astrobiology Center [CAN 03-OSS-02]; NSF [AST 08-02230, AST-0708899]; Hubble Space Telescope [HST-GO-10764, HST-GO-10864]; University of Cincinnati; Aerospace Corporation; [D065]; [E510] FX Supported by the Kentucky Space Grant Consortium and NASA.; We thank the staff of the Chandra X-ray Center who tracked down the Aspect Camera Array Data used in target acquisition of MWC 480, and the anonymous referee for excellent comments and suggestions. This study is based on observations made with the Chandra X-Ray Observatory which is operated by the Smithsonian Astrophysical Observatory under NAS8-03060. It is also based on observations made with the NASA/ESA Hubble Space Telescope, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA Contract NAS5-26555. FUV spectroscopy used in this study was based on observations made with the NASA-CNES-CSA Far Ultraviolet Spectroscopic Explorer, and was supported under NASA contract NNG05EA89P to Eureka Scientific. FUSE was operated for NASA by the Johns Hopkins University under NASA contract NAS5-32985. We acknowledge support for analysis of those observations through Chandra Award Number 09200520 issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8-03060, and HST-GO-10177 from the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS 5-26555. FUSE data included in this study were obtained under programs D065 and E510. The Goddard Fabry-Perot Interferometer is supported under NASA RTOP 399131.02.06.02.32 to Goddard Space Flight Center. K. H. was supported under NASA Astrobiology Center funding under CAN 03-OSS-02. J.P.W. acknowledges support from NSF Astronomy & Astrophysics Postdoctoral Fellowship AST 08-02230. S. D. B. acknowledges support for this work from the National Science Foundation under grant number AST-0708899 and NASA Origins of Solar Systems under grant number NNX08AH90G. M. R. T. performed this work under contract with the Jet Propulsion Laboratory (JPL) funded by NASA through the Michelson Fellowship Program. JPL is managed for NASA by the California Institute of Technology. M. L. S. was supported under NASA ADP grants NNH06CC28C & NNX09AC73G, and Hubble Space Telescope grants HST-GO-10764 and HST-GO-10864. A. N. Day acknowledges support from the Women in Science and Engineering program at the University of Cincinnati. Support for this work was also provided by the IR&D program at The Aerospace Corporation. NR 92 TC 20 Z9 20 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 AUG 20 PY 2010 VL 719 IS 2 BP 1565 EP 1581 DI 10.1088/0004-637X/719/2/1565 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 635LU UT WOS:000280658000043 ER PT J AU Shen, Y Hennawi, JF Shankar, F Myers, AD Strauss, MA Djorgovski, SG Fan, XH Giocoli, C Mahabal, A Schneider, DP Weinberg, DH AF Shen, Yue Hennawi, Joseph F. Shankar, Francesco Myers, Adam D. Strauss, Michael A. Djorgovski, S. G. Fan, Xiaohui Giocoli, Carlo Mahabal, Ashish Schneider, Donald P. Weinberg, David H. TI BINARY QUASARS AT HIGH REDSHIFT. II. SUB-Mpc CLUSTERING AT z similar to 3-4 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; SUPERMASSIVE BLACK-HOLES; PHOTOMETRICALLY CLASSIFIED QUASARS; LUMINOSITY FUNCTION; GALAXY FORMATION; DATA RELEASE; SMALL SCALES; EVOLUTION; MASS; FRAMEWORK AB We present measurements of the small-scale (0.1 less than or similar to r less than or similar to 1 h(-1) Mpc) quasar two-point correlation function at z > 2.9, for a flux-limited (i < 21) sample of 15 binary quasars compiled by Hennawi et al. The amplitude of the small-scale clustering increases from z similar to 3 to z similar to 4. The small-scale clustering amplitude is comparable to or lower than power-law extrapolations (assuming a fixed slope gamma = 2) from the large-scale correlation function of the i < 20.2 quasar sample from the Sloan Digital Sky Survey. Using simple prescriptions relating quasars to dark matter halos, we model the observed small-scale clustering with halo occupation models. We found that the level of small-scale clustering favors an active fraction of black holes in (M greater than or similar to 1013 h(-1) M(circle dot)) satellite halos fs greater than or similar to 0.1 at z greater than or similar to 3. C1 [Shen, Yue; Strauss, Michael A.] Princeton Univ Observ, Princeton, NJ 08544 USA. [Shen, Yue] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hennawi, Joseph F.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Hennawi, Joseph F.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Shankar, Francesco] Max Planck Inst Astrophys, D-85748 Garching, Germany. [Myers, Adam D.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Djorgovski, S. G.; Mahabal, Ashish] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Fan, Xiaohui] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Giocoli, Carlo] Univ Heidelberg, Zentrum Astron, Inst Theoret Astrophys, D-69120 Heidelberg, Germany. [Schneider, Donald P.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Weinberg, David H.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. RP Shen, Y (reprint author), Princeton Univ Observ, Peyton Hall, Princeton, NJ 08544 USA. FU NSF [AST-0707266, AST-0607634, AST-0407448]; Smithsonian Astrophysical Observatory; NASA [NNG05GH77G]; Alexander von Humboldt Foundation; Ajax Foundation FX We thank the anonymous referee for useful comments and Silvia Bonoli, Charlie Conroy, Phil Hopkins, and Linhua Jiang for helpful discussions. This work was partially supported by NSF grants AST-0707266 (Y.S. and M.A.S.) and AST-0607634 (D.P.S.). Y.S. acknowledges partial support from a Clay Post-doctoral Fellowship through the Smithsonian Astrophysical Observatory (SAO). F.S. acknowledges partial support from NASA grant NNG05GH77G and from the Alexander von Humboldt Foundation. S.G.D. and A.M. acknowledge partial support from NSF grant AST-0407448 and the Ajax Foundation. NR 47 TC 38 Z9 38 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2010 VL 719 IS 2 BP 1693 EP 1698 DI 10.1088/0004-637X/719/2/1693 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 635LU UT WOS:000280658000051 ER PT J AU Naoz, S Perets, HB Ragozzine, D AF Naoz, Smadar Perets, Hagai B. Ragozzine, Darin TI THE OBSERVED ORBITAL PROPERTIES OF BINARY MINOR PLANETS SO ASTROPHYSICAL JOURNAL LA English DT Article DE Kuiper belt: general; minor planets, asteroids: general; planets and satellites: dynamical evolution and stability; planets and satellites: fundamental parameters ID KUIPER-BELT BINARIES; TRANS-NEPTUNIAN BINARIES; ADAPTIVE OPTICS; MUTUAL ORBITS; 2003 EL61; TRANSNEPTUNIAN BINARIES; ASTEROIDAL SYSTEMS; TIDAL FRICTION; SATELLITES; EVOLUTION AB Many binary minor planets (BMPs; both binary asteroids and binary trans-Neptunian objects) are known to exist in the solar system. The currently observed orbital and physical properties of BMPs hold essential information and clues about their origin, their evolution, and the conditions under which they evolved. Here, we study the orbital properties of BMPs with currently known mutual orbits. We find that BMPs are typically highly inclined relative to their orbit around the Sun, with a distribution consistent with an isotropic distribution. BMPs not affected by tidal forces are found to have high eccentricities with non-thermal eccentricity distribution peaking at intermediate eccentricities (typically 0.4-0.6). The high inclinations and eccentricities of the BMPs suggest that BMPs evolved in a dense collisional environment, in which gravitational encounters in addition to tidal and secular Kozai effects played an important role in their orbital evolution. C1 [Naoz, Smadar] Northwestern Univ, CIERA, Evanston, IL 60208 USA. [Naoz, Smadar] Tel Aviv Univ, Raymond & Beverly Sackler Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Perets, Hagai B.; Ragozzine, Darin] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Naoz, S (reprint author), Northwestern Univ, CIERA, Evanston, IL 60208 USA. RI Ragozzine, Darin/C-4926-2013; Perets, Hagai/K-9605-2015; OI Perets, Hagai/0000-0002-5004-199X; Naoz, Smadar/0000-0002-9802-9279 FU Israel Science Foundation [629/05]; U.S.-Israel Binational Science Foundation [2004386]; NASA FX We would like to thank Will Grundy for pointing out an incorrect transformation from the ecliptic plane to the equatorial frame of reference. We thank Eran Ofek for useful discussion regarding this issue. We also thank the anonymous referee for helpful comments. S.N. acknowledges the partial support by Israel Science Foundation grant 629/05 and U.S.-Israel Binational Science Foundation grant 2004386. S.N. and H.B.P. acknowledge the generous support of the Dan David Fellowship. H.B.P. is a CfA, Rothschild, FIRST, and Fullbright fellow. H.B.P. also acknowledges the Israeli commercial and industrial club for their support through the Ilan-Ramon-Fullbright fellowship. D.R. is grateful for the support by NASA Headquarters under the Earth and Space Sciences Fellowship. NR 62 TC 13 Z9 13 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2010 VL 719 IS 2 BP 1775 EP 1783 DI 10.1088/0004-637X/719/2/1775 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 635LU UT WOS:000280658000058 ER PT J AU Burke, CJ McCullough, PR Bergeron, LE Long, D Gilliland, RL Nelan, EP Johns-Krull, CM Valenti, JA Janes, KA AF Burke, Christopher J. McCullough, P. R. Bergeron, L. E. Long, Douglas Gilliland, Ronald L. Nelan, Edmund P. Johns-Krull, Christopher M. Valenti, Jeff A. Janes, Kenneth A. TI NICMOS OBSERVATIONS OF THE TRANSITING HOT JUPITER XO-1b SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars: individual (GSC 02041-01657) ID HUBBLE-SPACE-TELESCOPE; GIANT PLANET TRANSITS; SUN-LIKE STAR; EXTRASOLAR PLANETS; TRANSMISSION SPECTRA; EXOPLANET XO-1B; HD 209458B; ATMOSPHERES; SPECTROSCOPY; PHOTOMETRY AB We refine the physical parameters of the transiting hot Jupiter planet XO-1b and its stellar host XO-1 using Hubble Space Telescope (HST) NICMOS observations. XO-1b has a radius R-p = 1.21 +/- 0.03 R-J, and XO-1 has a radius R* = 0.94 +/- 0.02 R-circle dot, where the uncertainty in the mass of XO-1 dominates the uncertainty of R-p and R*. There are no significant differences in the XO-1 system properties between these broadband NIR observations and previous determinations based upon ground-based optical observations. We measure two transit timings from these observations with 9 s and 15 s precision. As a residual to a linear ephemeris model, there is a 2.0 sigma timing difference between the two HST visits that are separated by three transit events (11.8 days). These two transit timings and additional timings from the literature are sufficient to rule out the presence of an Earth mass planet orbiting in 2:1 mean motion resonance coplanar with XO-1b. We identify and correct for poorly understood "gain-like" variations present in NICMOS time series data. This correction reduces the effective noise in time series photometry by a factor of 2 for the case of XO-1. C1 [Burke, Christopher J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [McCullough, P. R.; Bergeron, L. E.; Long, Douglas; Gilliland, Ronald L.; Nelan, Edmund P.; Valenti, Jeff A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Johns-Krull, Christopher M.] Rice Univ, Dept Phys & Astron, Houston, TX 77005 USA. [Janes, Kenneth A.] Boston Univ, Dept Astron, Boston, MA 02215 USA. RP Burke, CJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM cburke@cfa.harvard.edu OI Long, Douglas/0000-0002-2508-9211 FU HST [10998]; NASA [NNG06GG92G] FX We thank the referee for the helpful comments and improvements to this work. This work benefited from discussions with Philip Nutzman, Dan Fabrycky, Joe Hora, David Charbonneau, and Jeff Stys. We thank Mark Swain and Pieter Dieroo for conversations about spectrophotometry with NICMOS. We thank Josh Winn and Valentin Ivanov for discussing their published transit timings, and the following observers for their generosity in making their transit timing measurements publicly available: Anthony Ayiomamitis, Cindy Foote, Bruce Gary, Joao Gregorio, Bill Norby, Gregor Srdoc, Jaroslav Trnka, and Tonny Vanmunster. This work was supported in part by HST program 10998 and by NASA grant NNG06GG92G. NR 54 TC 15 Z9 15 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 AUG 20 PY 2010 VL 719 IS 2 BP 1796 EP 1806 DI 10.1088/0004-637X/719/2/1796 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 635LU UT WOS:000280658000060 ER PT J AU Stauffer, JR Rebull, LM James, D Noriega-Crespo, A Strom, S Wolk, S Carpenter, JM Navascues, DBY Micela, G Backman, D Cargile, PA AF Stauffer, John R. Rebull, Luisa M. James, David Noriega-Crespo, Alberto Strom, Steven Wolk, Scott Carpenter, John M. Barrado y Navascues, David Micela, Giusi Backman, Dana Cargile, P. A. TI DEBRIS DISKS OF MEMBERS OF THE BLANCO 1 OPEN CLUSTER SO ASTROPHYSICAL JOURNAL LA English DT Article DE open clusters and associations: individual (Blanco 1); stars: low-mass ID SPITZER-SPACE-TELESCOPE; SOLAR-TYPE STARS; MULTIBAND IMAGING PHOTOMETER; RADIATION-DRIVEN IMPLOSION; ZETA-SCULPTORIS CLUSTER; PLANETARY SYSTEMS; MOLECULAR CLOUD; MIPS SURVEY; YOUNG; EVOLUTION AB We have used the Spitzer Space Telescope to obtain Multiband Imaging Photometer for Spitzer (MIPS) 24 mu m photometry for 37 members of the similar to 100 Myr old open cluster Blanco 1. For the brightest 25 of these stars (where we have 3 sigma uncertainties less than 15%), we find significant mid-IR excesses for eight stars, corresponding to a debris disk detection frequency of about 32%. The stars with excesses include two A stars, four F dwarfs, and two G dwarfs. The most significant linkage between 24 mu m excess and any other stellar property for our Blanco 1 sample of stars is with binarity. Blanco 1 members that are photometric binaries show few or no detected 24 mu m excesses whereas a quarter of the apparently single Blanco 1 members do have excesses. We have examined the MIPS data for two other clusters of similar age to Blanco 1-NGC 2547 and the Pleiades. The AFGK photometric binary star members of both of these clusters also show a much lower frequency of 24 mu m excesses compared to stars that lie near the single-star main sequence. We provide a new determination of the relation between the V - K(s) color and K(s) - [24] color for main sequence photospheres based on Hyades members observed with MIPS. As a result of our analysis of the Hyades data, we identify three low mass Hyades members as candidates for having debris disks near the MIPS detection limit. C1 [Stauffer, John R.; Noriega-Crespo, Alberto] Caltech 314 6, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Rebull, Luisa M.] Caltech 220 6, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [James, David] Univ Hawaii, Dept Phys & Astron, Hilo, HI 96720 USA. [Strom, Steven] Natl Opt Astron Observ, Tucson, AZ 85721 USA. [Wolk, Scott] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Carpenter, John M.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Barrado y Navascues, David] Ctr Astron Hispano Aleman, Calar Alto Observ, E-04004 Almeria, Spain. [Barrado y Navascues, David] CSIC, Ctr Astrobiol INTA, Dept Astrofis, LAEX, E-28691 Villanueva De La Canada, Spain. [Micela, Giusi] INAF Osservatorio Astron Palermo Giuseppe S Vaian, I-90134 Palermo, Italy. [Backman, Dana] Stratospher Observ Infrared Astron, Mountain View, CA 94043 USA. [Backman, Dana] SETI Inst, Mountain View, CA 94043 USA. [Cargile, P. A.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. RP Stauffer, JR (reprint author), Caltech 314 6, Spitzer Sci Ctr, Pasadena, CA 91125 USA. RI Barrado Navascues, David/C-1439-2017; OI Barrado Navascues, David/0000-0002-5971-9242; Micela, Giuseppina/0000-0002-9900-4751; Wolk, Scott/0000-0002-0826-9261; Rebull, Luisa/0000-0001-6381-515X FU NASA [1407]; National Science Foundation FX This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. Most of the support for this work was provided by the Jet Propulsion Laboratory, California Institute of Technology, under NASA contract 1407. This research has made use of NASA's Star and Exoplanet Database (NStED) and the Astrophysics Data System (ADS) Abstract Service, and of the SIMBAD database, operated at CDS, Strasbourg, France. This research has made use of data products from the 2MASS, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center, funded by the National Aeronautics and Space Administration and the National Science Foundation. These data were served by 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. The research described in this paper was partially carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration.; This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. NR 59 TC 9 Z9 9 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2010 VL 719 IS 2 BP 1859 EP 1871 DI 10.1088/0004-637X/719/2/1859 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 635LU UT WOS:000280658000065 ER PT J AU Frisch, PC Heerikhuisen, J Pogorelov, NV DeMajistre, B Crew, GB Funsten, HO Janzen, P McComas, DJ Moebius, E Mueller, HR Reisenfeld, DB Schwadron, NA Slavin, JD Zank, GP AF Frisch, Priscilla C. Heerikhuisen, Jacob Pogorelov, Nikolai V. DeMajistre, Bob Crew, Geoffrey B. Funsten, Herbert O. Janzen, Paul McComas, David J. Moebius, Eberhard Mueller, Hans-Reinhard Reisenfeld, Daniel Brett Schwadron, Nathan A. Slavin, Jonathan D. Zank, Gary Paul TI CAN IBEX IDENTIFY VARIATIONS IN THE GALACTIC ENVIRONMENT OF THE SUN USING ENERGETIC NEUTRAL ATOMS? SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: clouds; ISM: kinematics and dynamics; ISM: magnetic fields; ISM: structure; plasmas; Sun: heliosphere ID INTERSTELLAR BOUNDARY EXPLORER; OUTER HELIOSPHERE; MAGNETIC-FIELD; SOLAR-CYCLE; PHYSICAL-PROPERTIES; TERMINATION SHOCK; LOCAL CLOUD; GAS; HYDROGEN; RIBBON AB The Interstellar Boundary Explorer (IBEX) spacecraft is providing the first all-sky maps of the energetic neutral atoms (ENAs) produced by charge exchange between interstellar neutral H degrees atoms and heliospheric solar wind and pickup ions in the heliosphere boundary regions. The "edge" of the interstellar cloud presently surrounding the heliosphere extends less than 0.1 pc in the upwind direction, terminating at an unknown distance, indicating that the outer boundary conditions of the heliosphere could change during the lifetime of the IBEX satellite. Using reasonable values for future outer heliosphere boundary conditions, ENA fluxes are predicted for one possible source of ENAs coming from outside of the heliopause. The ENA-production simulations use three-dimensional MHD plasma models of the heliosphere that include a kinetic description of neutrals and a Lorentzian distribution for ions. Based on this ENA-production model, it is then shown that the sensitivities of the IBEX 1.1 keV skymaps are sufficient to detect the variations in ENA fluxes that are expected to accompany the solar transition into the next upwind cloud. Approximately 20% of the IBEX 1.1 keV pixels appear capable of detecting the predicted model differences at the 3 sigma level, with these pixels concentrated in the Ribbon region. Regardless of the detailed ENA production model, the success of the modeled B . R similar to 0 directions in reproducing the Ribbon locus, together with our results, indicates that the Ribbon phenomenon traces the variations in the heliosphere distortion caused by the relative pressures of the interstellar magnetic and gaseous components. C1 [Frisch, Priscilla C.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Heerikhuisen, Jacob; Pogorelov, Nikolai V.; Zank, Gary Paul] Univ Alabama, CSPAR, Huntsville, AL 35899 USA. [DeMajistre, Bob] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Crew, Geoffrey B.] MIT, Cambridge, MA 02142 USA. [Funsten, Herbert O.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Janzen, Paul; Reisenfeld, Daniel Brett] Univ Montana, Dept Phys & Astron, Missoula, MT 59812 USA. [McComas, David J.] SW Res Inst, San Antonio, TX 78227 USA. [Moebius, Eberhard] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. [Mueller, Hans-Reinhard] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA. [Schwadron, Nathan A.] Boston Univ, Boston, MA 02215 USA. [Slavin, Jonathan D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Frisch, PC (reprint author), Univ Chicago, Dept Astron & Astrophys, 5640 S Ellis Ave, Chicago, IL 60637 USA. EM frisch@oddjob.uchicago.edu; jacobh@ucr.edu; nikolaip@ucr.edu; Bob.DeMajistre@jhuapl.edu; gbc@haystack.mit.edu; hfunsten@lanl.gov; paul.janzen@umontana.edu; DMcComas@swri.edu; eberhard.moebius@unh.edu; Hans-Reinhard.Mueller@Dartmouth.edu; dan.reisenfeld@umontana.edu; nathanas@bu.edu; jslavin@cfa.harvard.edu; zank@email.cspar.uah.edu RI Funsten, Herbert/A-5702-2015; Reisenfeld, Daniel/F-7614-2015; OI Funsten, Herbert/0000-0002-6817-1039; Mueller, Hans-Reinhard/0000-0001-7364-5377; Slavin, Jonathan/0000-0002-7597-6935; Moebius, Eberhard/0000-0002-2745-6978; Heerikhuisen, Jacob/0000-0001-7867-3633 FU IBEX mission; NASA [NNX09AG63G] FX We thank the IBEX team members. This work was funded through the IBEX mission, as a part of NASA's Explorer Program. J.H. acknowledges support from the NASA IBEX program through the grant NNX09AG63G. We thank Ed Roelof for his help with the CG corrections. NR 46 TC 14 Z9 14 U1 1 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2010 VL 719 IS 2 BP 1984 EP 1992 DI 10.1088/0004-637X/719/2/1984 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 635LU UT WOS:000280658000078 ER PT J AU Sell, PH Heinz, S Calvelo, DE Tudose, V Soleri, P Fender, RP Jonker, PG Schulz, NS Brandt, WN Nowak, MA Wijnands, R Van der Klis, M Casella, P AF Sell, P. H. Heinz, S. Calvelo, D. E. Tudose, V. Soleri, P. Fender, R. P. Jonker, P. G. Schulz, N. S. Brandt, W. N. Nowak, M. A. Wijnands, R. Van der Klis, M. Casella, P. TI PARSEC-SCALE BIPOLAR X-RAY SHOCKS PRODUCED BY POWERFUL JETS FROM THE NEUTRON STAR CIRCINUS X-1 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE ISM: jets and outflows; X-rays: binaries; X-rays: individual (Circinus X-1) ID RELATIVISTIC OUTFLOW; RADIO JETS; BINARY; SS-433; VARIABILITY; DISCOVERY; COMPANION; SPECTRUM AB We report the discovery of multi-scale X-ray jets from the accreting neutron star X-ray binary, Circinus X-1. The bipolar outflows show wide opening angles and are spatially coincident with the radio jets seen in new high-resolution radio images of the region. The morphology of the emission regions suggests that the jets from Circinus X-1 are running into a terminal shock with the interstellar medium, as is seen in powerful radio galaxies. This and other observations indicate that the jets have a wide opening angle, suggesting that the jets are either not very well collimated or precessing. We interpret the spectra from the shocks as cooled synchrotron emission and derive a cooling age of similar to 1600 yr. This allows us to constrain the jet power to be 3 x 10(35) erg s(-1) less than or similar to P(jet) less than or similar to 2 x 10(37) erg s(-1), making this one of a few microquasars with a direct measurement of its jet power and the only known microquasar that exhibits stationary large-scale X-ray emission. C1 [Sell, P. H.; Heinz, S.] Univ Wisconsin Madison, Dept Astron, Madison, WI 54706 USA. [Calvelo, D. E.; Fender, R. P.; Casella, P.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Tudose, V.] Netherlands Inst Radio Astron, NL-7990 AA Dwingeloo, Netherlands. [Tudose, V.] Acad Romana, Astron Inst, RO-040557 Bucharest, Romania. [Tudose, V.] Res Ctr Atom Phys & Astrophys, RO-077125 Bucharest, Romania. [Soleri, P.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Jonker, P. G.] SRON, Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. [Jonker, P. G.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands. [Jonker, P. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Schulz, N. S.; Nowak, M. A.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Brandt, W. N.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Wijnands, R.; Van der Klis, M.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XM Amsterdam, Netherlands. RP Sell, PH (reprint author), Univ Wisconsin Madison, Dept Astron, Madison, WI 54706 USA. RI Tudose, Valeriu/F-8976-2010; Brandt, William/N-2844-2015; Sell, Paul/B-1283-2017; OI Brandt, William/0000-0002-0167-2453; Sell, Paul/0000-0003-1771-5531; Heinz, Sebastian/0000-0002-8433-8652; Casella, Piergiorgio/0000-0002-0752-3301 FU NASA [GO9-0056X] FX S.H. and P.S. acknowledge support from NASA grant GO9-0056X. NR 26 TC 14 Z9 14 U1 0 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD AUG 20 PY 2010 VL 719 IS 2 BP L194 EP L198 DI 10.1088/2041-8205/719/2/L194 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 642HP UT WOS:000281199900019 ER PT J AU Tran, KVH Papovich, C Saintonge, A Brodwin, M Dunlop, JS Farrah, D Finkelstein, KD Finkelstein, SL Lotz, J McLure, RJ Momcheva, I Willmer, CNA AF Tran, Kim-Vy H. Papovich, Casey Saintonge, Amelie Brodwin, Mark Dunlop, James S. Farrah, Duncan Finkelstein, Keely D. Finkelstein, Steven L. Lotz, Jennifer McLure, Ross J. Momcheva, Ivelina Willmer, Christopher N. A. TI REVERSAL OF FORTUNE: CONFIRMATION OF AN INCREASING STAR FORMATION-DENSITY RELATION IN A CLUSTER AT z=1.62 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: clusters: individual (ClG J0218.3-0510); galaxies: evolution; galaxies: starburst; infrared: galaxies ID EARLY-TYPE GALAXIES; FORMATION RATES; RICH CLUSTERS; SKY SURVEY; EVOLUTION; ENVIRONMENT; REDSHIFT; SEQUENCE; Z=0.83; FIELD AB We measure the rest-frame colors (dust-corrected), infrared luminosities, star formation rates, and stellar masses of 92 galaxies in a Spitzer-selected cluster at z = 1.62. By fitting spectral energy distributions (SEDs) to 10-band photometry (0.4 mu m < lambda(obs) < 8 mu m) and measuring 24 mu m fluxes for the 12 spectroscopically confirmed and 80 photometrically selected members, we discover an exceptionally high level of star formation in the cluster core of similar to 1700 M(circle dot) yr(-1) Mpc(-2). The cluster galaxies define a strong blue sequence in (U-V) color and span a range in color. We identify 17 members with L(IR) > 10(11) L(circle dot), and these IR luminous members follow the same trend of increasing star formation with stellar mass that is observed in the field at z similar to 2. Using rates derived from both the 24 mu m imaging and SED fitting, we find that the relative fraction of star-forming members triples from the lowest to highest galaxy density regions; e.g., the IR luminous fraction increases from similar to 8% at Sigma similar to 10 gal Mpc(-2) to similar to 25% at Sigma greater than or similar to 100 gal Mpc(-2). The observed increase is a reversal of the well-documented trend at z < 1 and signals that we have reached the epoch when massive cluster galaxies are still forming a substantial fraction of their stars. C1 [Tran, Kim-Vy H.; Papovich, Casey; Finkelstein, Keely D.; Finkelstein, Steven L.] Texas A&M Univ, Dept Phys, George P & Cynthia W Mitchell Inst Fundamental Ph, College Stn, TX 77843 USA. [Tran, Kim-Vy H.] Univ Zurich, Inst Theoret Phys, CH-8057 Zurich, Switzerland. [Saintonge, Amelie] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Brodwin, Mark] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Dunlop, James S.; McLure, Ross J.] Univ Edinburgh, Inst Astron, SUPA, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Farrah, Duncan] Univ Sussex, Ctr Astron, Brighton BN1 9QH, E Sussex, England. [Lotz, Jennifer] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Momcheva, Ivelina] Carnegie Inst Washington, Pasadena, CA 91101 USA. [Willmer, Christopher N. A.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Tran, KVH (reprint author), Texas A&M Univ, Dept Phys, George P & Cynthia W Mitchell Inst Fundamental Ph, College Stn, TX 77843 USA. EM vy@physics.tamu.edu FU Swiss National Science Foundation [PP002-110576]; Royal Society; European Research Council; NOAO, NSF FX K.T. acknowledges generous support from the Swiss National Science Foundation (grant PP002-110576). J.S.D. acknowledges the support of the Royal Society via a Wolfson Research Merit award, and also the support of the European Research Council via the award of an Advanced Grant. This work is based in part on data obtained as part of the UKIRT Infrared Deep Sky Survey. A portion of the Magellan telescope time was granted by NOAO, through the Telescope System Instrumentation Program (TSIP; funded by NSF). NR 43 TC 113 Z9 113 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD AUG 20 PY 2010 VL 719 IS 2 BP L126 EP L129 DI 10.1088/2041-8205/719/2/L126 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 642HP UT WOS:000281199900004 ER PT J AU Wang, JF Fabbiano, G Risaliti, G Elvis, M Mundell, CG Dumas, G Schinnerer, E Zezas, A AF Wang, Junfeng Fabbiano, Giuseppina Risaliti, Guido Elvis, Martin Mundell, Carole G. Dumas, Gaelle Schinnerer, Eva Zezas, Andreas TI EXTENDED X-RAY EMISSION IN THE HI CAVITY OF NGC 4151: GALAXY-SCALE ACTIVE GALACTIC NUCLEUS FEEDBACK? SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: individual (NGC 4151); galaxies: jets; galaxies: Seyfert; X-rays: galaxies ID NARROW-LINE REGION; BLACK-HOLES; NEUTRAL HYDROGEN; STAR-FORMATION; DISK GALAXIES; GAS-DYNAMICS; GEMINI NIFS; NGC-4151; CHANDRA; QUASARS AB We present the Chandra discovery of soft diffuse X-ray emission in NGC 4151 (L(0.5-2keV) similar to 10(39) ergs(-1)), extending similar to 2 kpc from the active nucleus and filling in the cavity of the HI material. The best fit to the X-ray spectrum requires either a kT similar to 0.25 keV thermal plasma or a photoionized component. In the thermal scenario, hot gas heated by the nuclear outflow would be confined by the thermal pressure of the HI gas and the dynamic pressure of inflowing neutral material in the galactic disk. In the case of photoionization, the nucleus must have experienced an Eddington limit outburst. For both scenarios, the active galactic nucleus (AGN)-host interaction in NGC 4151 must have occurred relatively recently (some 10(4) yr ago). This very short timescale to the last episode of high activity phase may imply such outbursts occupy greater than or similar to 1% of AGN lifetime. C1 [Wang, Junfeng; Fabbiano, Giuseppina; Risaliti, Guido; Elvis, Martin; Zezas, Andreas] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Risaliti, Guido] INAF Arcetri Observ, I-50125 Florence, Italy. [Mundell, Carole G.] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England. [Dumas, Gaelle; Schinnerer, Eva] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Zezas, Andreas] Univ Crete, Dept Phys, GR-71003 Iraklion, Crete, Greece. RP Wang, JF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Wang, Junfeng/A-1476-2011; Zezas, Andreas/C-7543-2011; OI Zezas, Andreas/0000-0001-8952-676X; Risaliti, Guido/0000-0002-3556-977X; Schinnerer, Eva/0000-0002-3933-7677 FU NASA [GO8-9101X, NAS8-39073 (CXC)]; DFG [SCH 536/4-1, SCH 536/4-2, SPP 1177] FX We thank the anonymous referee for helpful comments. This work is partially supported by the NASA grant GO8-9101X and the NASA Contract NAS8-39073 (CXC). G. D. acknowledges support from DFG grants SCH 536/4-1 and SCH 536/4-2 as part of the SPP 1177. NR 50 TC 10 Z9 10 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD AUG 20 PY 2010 VL 719 IS 2 BP L208 EP L212 DI 10.1088/2041-8205/719/2/L208 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 642HP UT WOS:000281199900022 ER PT J AU Watters, TR Robinson, MS Beyer, RA Banks, ME Bell, JF Pritchard, ME Hiesinger, H van der Bogert, CH Thomas, PC Turtle, EP Williams, NR AF Watters, Thomas R. Robinson, Mark S. Beyer, Ross A. Banks, Maria E. Bell, James F., III Pritchard, Matthew E. Hiesinger, Harald van der Bogert, Carolyn H. Thomas, Peter C. Turtle, Elizabeth P. Williams, Nathan R. TI Evidence of Recent Thrust Faulting on the Moon Revealed by the Lunar Reconnaissance Orbiter Camera SO SCIENCE LA English DT Article ID THERMAL HISTORY; TECTONICS; MERCURY; ORIGIN AB Lunar Reconnaissance Orbiter Camera images reveal previously undetected lobate thrust-fault scarps and associated meter-scale secondary tectonic landforms that include narrow extensional troughs or graben, splay faults, and multiple low-relief terraces. Lobate scarps are among the youngest landforms on the Moon, based on their generally crisp appearance, lack of superposed large-diameter impact craters, and the existence of crosscut small-diameter impact craters. Identification of previously known scarps was limited to high-resolution Apollo Panoramic Camera images confined to the equatorial zone. Fourteen lobate scarps were identified, seven of which are at latitudes greater than +/- 60 degrees, indicating that the thrust faults are globally distributed. This detection, coupled with the very young apparent age of the faults, suggests global late-stage contraction of the Moon. C1 [Watters, Thomas R.; Banks, Maria E.] Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. [Robinson, Mark S.] Arizona State Univ, Sch Earth & Space Explorat, Scottsdale, AZ 85251 USA. [Beyer, Ross A.] SETI Inst, Carl Sagan Ctr, Mountain View, CA 94043 USA. [Beyer, Ross A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Bell, James F., III] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Pritchard, Matthew E.; Williams, Nathan R.] Cornell Univ, Dept Earth & Atmospher Sci, Ithaca, NY 14853 USA. [Hiesinger, Harald; van der Bogert, Carolyn H.] Univ Munster, Inst Planetol, D-48149 Munster, Germany. [Hiesinger, Harald] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. [Thomas, Peter C.] Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA. [Turtle, Elizabeth P.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. RP Watters, TR (reprint author), Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. EM watterst@si.edu RI Turtle, Elizabeth/K-8673-2012; Pritchard, Matthew/L-5892-2015; OI Turtle, Elizabeth/0000-0003-1423-5751; Pritchard, Matthew/0000-0003-3616-3373; Beyer, Ross/0000-0003-4503-3335 FU NASA [NNX08AM73G, NNG07EK00C]; Deutsches Zentrum fur Luft- und Raumfahrt [50 OW 0901] FX We thank the three anonymous reviewers for helpful comments that improved the manuscript. We gratefully acknowledge the Lunar Orbiter Laser Altimeter team for the lunar topographic model and the LRO and LROC engineers and technical support personnel. This work was supported by the LRO Project, NASA grants NNX08AM73G and NNG07EK00C, and through Deutsches Zentrum fur Luft- und Raumfahrt grant 50 OW 0901. NR 34 TC 34 Z9 39 U1 0 U2 14 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD AUG 20 PY 2010 VL 329 IS 5994 BP 936 EP 940 DI 10.1126/science.1189590 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 640WN UT WOS:000281084800032 PM 20724632 ER PT J AU Vanderelst, D De Mey, F Peremans, H Geipel, I Kalko, E Firzlaff, U AF Vanderelst, Dieter De Mey, Fons Peremans, Herbert Geipel, Inga Kalko, Elisabeth Firzlaff, Uwe TI What Noseleaves Do for FM Bats Depends on Their Degree of Sensorial Specialization SO PLOS ONE LA English DT Article ID BOUNDARY-ELEMENT METHOD; BIG BROWN BAT; EPTESICUS-FUSCUS; ECHOLOCATING BATS; EXTERNAL EAR; PHYLLOSTOMUS-DISCOLOR; SOUND LOCALIZATION; HORSESHOE BAT; EMISSION; SYSTEM AB Background: Many bats vocalizing through their nose carry a prominent noseleaf that is involved in shaping the emission beam of these animals. To our knowledge, the exact role of these appendages has not been thoroughly investigated as for no single species both the hearing and the emission spatial sensitivities have been obtained. In this paper, we set out to evaluate the complete spatial sensitivity of two species of New World leaf-nosed bats: Micronycteris microtis and Phyllostomus discolor. From an ecological point of view, these species are interesting as they belong to the same family (Phyllostomidae) and their noseleaves are morphologically similar. They differ vastly in the niche they occupy. Comparing these species allows us to relate differences in function of the noseleaf to the ecological background of bat species. Methodology/Principal Findings: We simulate the spatial sensitivity of both the hearing and the emission subsystems of two species, M. microtis and P. discolor. This technique allows us to evaluate the respective roles played by the noseleaf in the echolocation system of these species. We find that the noseleaf of M. microtis focuses the radiated energy better and yields better control over the emission beam. Conclusions: From the evidence presented we conclude that the noseleaves serve quantitatively different functions for different bats. The main function of the noseleaf is to serve as an energy focusing mechanism that increases the difference between the reflected energy from objects in the focal area and objects in the periphery. However, despite the gross morphological similarities between the noseleaves of the two Phyllostomid species they focus the energy to a different extent, a capability that can be linked to the different ecological niches occupied by the two species. C1 [Vanderelst, Dieter; De Mey, Fons; Peremans, Herbert] Univ Antwerp, Act Percept Lab, B-2020 Antwerp, Belgium. [Geipel, Inga; Kalko, Elisabeth] Univ Ulm, Inst Expt Ecol, Ulm, Germany. [Kalko, Elisabeth] Smithsonian Trop Res Inst, Balboa, Panama. [Firzlaff, Uwe] Tech Univ Munich, Lehrstuhl Zool, D-8050 Freising Weihenstephan, Germany. RP Vanderelst, D (reprint author), Univ Antwerp, Act Percept Lab, B-2020 Antwerp, Belgium. EM dieter.vanderelst@ua.ac.be FU EU FX This work was funded by the EU CHIROPING (Chiroptera, Robots, Sonar) and CILIA (Customized Intelligent Life-inspired Arrays) projects. These projects are funded by the Seventh Framework Programme ICT Challenge 2: "Cognitive Systems, Interaction, Robotics" and the Future and Emergent Technologies arm of the IST Programme in the 6th Framework Programme respectively. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 42 TC 37 Z9 38 U1 1 U2 12 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 AUG 16 PY 2010 VL 5 IS 8 AR e11893 DI 10.1371/journal.pone.0011893 PG 13 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 639IH UT WOS:000280968000001 PM 20808438 ER PT J AU Dieter, D Elsenbeer, H Turner, BL AF Dieter, Daniela Elsenbeer, Helmut Turner, Benjamin L. TI Phosphorus fractionation in lowland tropical rainforest soils in central Panama SO CATENA LA English DT Article DE Barro Colorado Island; Hedley sequential fractionation; Inorganic phosphorus; Organic phosphorus; Panama; Phosphorus cycle ID BARRO COLORADO ISLAND; ORGANIC PHOSPHORUS; HEDLEY FRACTIONATION; EXTRACTION; DYNAMICS; NUTRIENT; MATTER; SPECTROSCOPY; CULTIVATION AB Phosphorus availability is commonly assumed to limit productivity in lowland tropical rainforests, yet there is relatively little information on the chemical forms of soil phosphorus in such ecosystems. We used the Hedley sequential fractionation scheme to assess phosphorus chemistry in five soils supporting tropical rainforest on Barro Colorado Island, Republic of Panama. The soils represented a range of orders (Inceptisols, Alfisols, and Oxisols) formed on contrasting geological substrates and topography, but under uniform climate and vegetation. Total phosphorus in surface horizons ranged between 315 and 1114 mg P kg(-1), being lowest on a soil derived from marine sediments and highest on soils derived from andesite. The majority of the phosphorus occurred in recalcitrant forms, although between 14% and 39% occurred as organic phosphorus. Readily-available phosphate, as extracted by anion-exchange membranes, occurred in small concentrations (4-13 mg P kg(-1)), although labile phosphorus, defined as phosphate extracted by anion-exchange membrane plus inorganic and organic phosphorus extracted by 0.5 M NaHCO(3), accounted for between 4.7% and 11.4% of the total soil phosphorus. Our results indicate a strong control of geology and topography on soil phosphorus in tropical rainforests, which may have important implications for understanding the diversity and distribution of plant species in such ecosystems. Further, some of the most common soils on Barro Colorado Island, including those on the 50 ha forest dynamics plot, are rich in phosphorus despite their relatively advanced stage of pedogenesis. (C) 2010 Elsevier B.V. All rights reserved. C1 [Dieter, Daniela; Elsenbeer, Helmut] Univ Potsdam, Dept Earth & Environm Sci, D-14476 Potsdam, Germany. [Elsenbeer, Helmut; Turner, Benjamin L.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Dieter, D (reprint author), Univ Potsdam, Dept Earth & Environm Sci, Karl Liebknecht Str 24-25, D-14476 Potsdam, Germany. EM Daniela.Dieter@igb-berlin.de RI Turner, Benjamin/E-5940-2011; Dieter, Daniela/G-2105-2012 OI Turner, Benjamin/0000-0002-6585-0722; FU German Academic Exchange Service (DAAD) FX Daniela Dieter and Helmut Elsenbeer acknowledge partial financial support from the German Academic Exchange Service (DAAD). We thank Tania Romero, Frauke Barthold, and staff on Barro Colorado Island for their contribution to the study. NR 46 TC 34 Z9 37 U1 3 U2 47 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0341-8162 J9 CATENA JI Catena PD AUG 15 PY 2010 VL 82 IS 2 BP 118 EP 125 DI 10.1016/j.catena.2010.05.010 PG 8 WC Geosciences, Multidisciplinary; Soil Science; Water Resources SC Geology; Agriculture; Water Resources GA 632WN UT WOS:000280460100008 ER PT J AU Rittenhouse, ST Mehta, NP Greene, CH AF Rittenhouse, Seth T. Mehta, N. P. Greene, Chris H. TI Green's functions and the adiabatic hyperspherical method SO PHYSICAL REVIEW A LA English DT Article ID BOUND-STATES; INTERACTING PARTICLES; ENERGY-LEVELS; DYNAMICS; ATOMS; RECOMBINATION; UNIVERSALITY; COLLISIONS; SYSTEMS AB We address the few-body problem using the adiabatic hyperspherical representation. A general form for the hyperangular Green's function in d dimensions is derived. The resulting Lippmann-Schwinger equation is solved for the case of three particles with s-wave zero-range interactions. Identical particle symmetry is incorporated in a general and intuitive way. Complete semianalytic expressions for the nonadiabatic channel couplings are derived. Finally, a model to describe the atom loss due to three-body recombination for a three-component Fermi gas of (6)Li atoms is presented. C1 [Rittenhouse, Seth T.; Mehta, N. P.; Greene, Chris H.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA. [Rittenhouse, Seth T.; Mehta, N. P.; Greene, Chris H.] Univ Colorado, Joint Inst Lab Astrophys, Boulder, CO 80309 USA. [Rittenhouse, Seth T.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. [Mehta, N. P.] Grinnell Coll, Dept Phys, Grinnell, IA 50112 USA. RP Rittenhouse, ST (reprint author), Univ Colorado, Dept Phys, Boulder, CO 80309 USA. RI Greene, Chris/C-3821-2011; Rittenhouse, Seth/E-7688-2011 OI Greene, Chris/0000-0002-2096-6385; FU National Science Foundation; Harvard University; Smithsonian Astrophysical Observatory FX The authors would like to thank D. Blume and J. P. D'Incao for many useful discussions. This research was supported in part by funding from the National Science Foundation. S. T. R. acknowledges support from a NSF grant to ITAMP at Harvard University and the Smithsonian Astrophysical Observatory. NR 39 TC 20 Z9 20 U1 0 U2 2 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD AUG 12 PY 2010 VL 82 IS 2 AR 022706 DI 10.1103/PhysRevA.82.022706 PG 12 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 637WL UT WOS:000280849300005 ER PT J AU Tauber, CA Flint, OS AF Tauber, Catherine A. Flint, Oliver S., Jr. TI Resolution of some taxonomic and nomenclatural issues in a recent revision of Ceraeochrysa (Neuroptera: Chrysopidae) SO ZOOTAXA LA English DT Article DE Ceraeochrysa; Chrysopodes; Ungla; synonymy; generic assignment ID GENERIC CHARACTERISTICS; CHRYSOPODES NEUROPTERA; LARVAL DESCRIPTIONS; CANADA; MEXICO; ADULTS AB With the purpose of promoting nomenclatural stability, this paper addresses a number of errors, omissions, and controversial conclusions in a recent revision of the green lacewing genus Ceraeochrysa by Freitas et al. (2009). 1. Valid species, new combinations and synonymies: (a) We identified Ceraeochrysa chiricahuae Freitas and Penny (in Freitas et al. 2009), Chrysopa forreri Navas, and Chrysopa intacta Navas as subjective synonyms. Thus, Ceraeochrysa intacta, a species that was previously synonymized under Ceraeochrysa placita (Banks), becomes the valid name of the species [New status, new combination]. Chrysopa forreri is now synonymized under Cer. intacta, not Cer. placita [New synonymy]. And, Cer. chiricahuae becomes a junior synonym of Cer. intacta, not a valid species of Ceraeochrysa [New synonymy]. (b) We enumerate specific internal and external features of the Chrysopa cornuta Navas type that identify it as conspecific with Ceraeochrysa caligata (Banks), not Ceraeochrysa cincta (Schneider) as proposed by Freitas et al. (2009). Thus, Ceraeochrysa cornuta (Navas), which has priority, is reinstated as the valid name [Reinstated status, reinstated combination], and Ceraeochrysa caligata (Banks) is reinstated as a junior subjective synonym of Cer. cornuta, not a valid species [Reinstated synonymy]. (c) We provide documented evidence for reinstating three synonymies that Freitas et al. had reversed [Reinstated synonymies]: (i) Allochrysa parvula Banks is a junior subjective synonym of Ceraeochrysa lineaticornis (Fitch); (ii) Chrysopa columbiana Banks is a junior subjective synonym of Ceraeochrysa lineaticornis (Fitch); (iii) Chrysopa rochina (Navas) is a junior subjective synonym of Ceraeochrysa cincta (Schneider). 2. Generic assignments: (a) Visual evidence is provided for the placement of Ceraeochrysa laufferi (Navas) in Ungla. Therefore, Ungla laufferi (Navas) is reinstated as the valid name [Reinstated combination]. (b) We question Freitas et al.'s rationale for including Cer. placita (Banks) and Cer. intacta (Navas) (as Cer. chiricahuae Freitas and Penny) in the genus Ceraeochrysa; female and larval features of the two species differ markedly from those used to characterize Ceraeochrysa species. As an alternative that recognizes the uncertainty surrounding the generic placement of these species and that avoids additional, unnecessary name changes, we propose including the caveat "genus incertae sedis" with the names, as follows: Ceraeochrysa placita (Banks), genus incertae sedis, and Ceraeochrysa intacta (Navas), genus incertae sedis. 3. Type designations: (a) Errors concerning the Chrysopa furculata Navas type in the Museum national d'Histoire naturelle, Paris (MNHN), are corrected, and doubts raised by Freitas et al. (2009) concerning the identification of this specimen as the holotype are removed. (b) The earlier designation of the Chrysopa rochina (Navas) type in the MNHN as the lectotype (not holotype) is verified. C1 [Tauber, Catherine A.] Cornell Univ, Dept Entomol, Ithaca, NY 14853 USA. [Tauber, Catherine A.] Univ Calif Davis, Dept Entomol, Davis, CA 95616 USA. [Flint, Oliver S., Jr.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. RP Tauber, CA (reprint author), Cornell Univ, Dept Entomol, Comstock Hall, Ithaca, NY 14853 USA. EM cat6@cornell.edu; flinto@si.edu FU National Science Foundation [DEB 0542373]; USDA/NRI [9802447]; Cornell University FX Special thanks go to Maurice J. Tauber (MJT) for his careful reading of the manuscript and constructive suggestions, to Gilberto Albuquerque for his comments on the manuscript and for sharing his notes on the C. cornuta type, and to Jean Legrand (MNHN) for providing the image of the C. cornuta lectotype. We thank S. P. Cover & P. Perkins (MCZ), D. Goodger (BMNH), J. Legrand (MNHN), V. Monserrat (Universidad Complutense, Madrid, MZB specimens), O. Lonsdale (CNC), C. Darling (ROM), B. Hubley (ROM), M. Wall (SDMNH), and Cheryl Barr (University of California, Berkeley, UCB) for providing access to types and specimens in their care. We thank J. Allan Garland (McGill University, Macdonald Campus, Quebec), John D. Oswald (Texas A & M University, College Station) and Atilano Contreras-Ramos (Universidad Nacional Autonoma de Mexico) for their constructive reviews of the manuscript. CAT thanks the Department of Entomology, University of California, Davis, for hospitality during the study. CAT's work was supported, in part, by National Science Foundation Grant DEB 0542373 (MJT, CAT), USDA/NRI Competitive Grant 9802447 (MJT, CAT), and Cornell University (MJT, CAT). NR 41 TC 8 Z9 8 U1 0 U2 1 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD AUG 12 PY 2010 IS 2565 BP 55 EP 67 PG 13 WC Zoology SC Zoology GA 637NP UT WOS:000280825300004 ER PT J AU Shankar, F Weinberg, DH Shen, Y AF Shankar, Francesco Weinberg, David H. Shen, Yue TI Constraints on black hole duty cycles and the black hole-halo relation from SDSS quasar clustering SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; galaxies: evolution; quasars: general; cosmology: theory ID DIGITAL-SKY-SURVEY; ACTIVE GALACTIC NUCLEI; DARK-MATTER HALOES; 5TH DATA RELEASE; HIGH-REDSHIFT; LUMINOSITY FUNCTION; SCALING RELATIONS; COSMIC EVOLUTION; GALAXY FORMATION; MASS FUNCTION AB We use Shen et al.'s (2009) measurements of luminosity-dependent clustering in the Sloan Digital Sky Survey Data Release 5 quasar catalogue, at redshifts 0.4 <= z <= 2.5, to constrain the relation between quasar luminosity and host halo mass and to infer the duty cycle f (opt), the fraction of black holes that shine as optically luminous quasars at a given time. We assume a monotonic mean relation between quasar luminosity and host halo mass, with lognormal scatter Sigma. For specified f (opt) and Sigma, matching the observed quasar space density determines the normalization of the luminosity-halo mass relation, from which we predict the clustering bias. The data show no change of bias between the faint and bright halves of the quasar sample but a modest increase in bias for the brightest 10 per cent. At the mean redshift z = 1.45 of the sample, the data can be well described either by models with small intrinsic scatter (Sigma = 0.1 dex) and a duty cycle f (opt) = 6 x 10(-4) or by models with much larger duty cycles and larger values of the scatter. 'Continuity equation' models of the black hole mass population imply f (opt) >= 2 x 10(-3) in this range of masses and redshifts, and the combination of this constraint with the clustering measurements implies scatter Sigma = 0.4 dex. These findings contrast with those inferred from the much stronger clustering of high-luminosity quasars at z approximate to 4, which require minimal scatter between luminosity and halo mass and duty cycles close to one. C1 [Shankar, Francesco] Max Planck Inst Astrophys, D-85748 Garching, Germany. [Weinberg, David H.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Weinberg, David H.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Weinberg, David H.] Inst Adv Study, Princeton, NJ 08540 USA. [Shen, Yue] Princeton Univ Observ, Princeton, NJ 08544 USA. [Shen, Yue] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Shankar, F (reprint author), Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85748 Garching, Germany. EM shankar@mpa-garching.mpg.de FU Alexander von Humboldt Foundation; NASA [NNG05GH77G] FX FS acknowledges the Alexander von Humboldt Foundation for support. FS and DW also acknowledge support from NASA Grant NNG05GH77G, and DW acknowledges support of an AMIAS membership at the Institute for Advanced Study. We thank Raul Angulo, Luca Graziani, Jeremy Tinker, Jaiyul Yoo and Zheng Zheng for interesting and helpful discussions. We thank the anonymous referee for comments that led to significant improvements of the paper. NR 80 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 AUG 11 PY 2010 VL 406 IS 3 BP 1959 EP 1966 DI 10.1111/j.1365-2966.2010.16801.x PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 635PT UT WOS:000280669200039 ER PT J AU Guainazzi, M Bianchi, S Matt, G Dadina, M Kaastra, J Malzac, J Risaliti, G AF Guainazzi, M. Bianchi, S. Matt, G. Dadina, M. Kaastra, J. Malzac, J. Risaliti, G. TI Final verdict from XMM-Newton: the X-ray obscured Seyfert galaxy NGC 5506 has a broad Fe K-alpha line SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; galaxies: Seyfert; X-rays: galaxies; X-rays: individual: NGC 5506 ID ACTIVE GALACTIC NUCLEI; PHOTON IMAGING CAMERA; BLACK-HOLE MASSES; IRON LINE; COMPTON-THIN; TIME VARIABILITY; ACCRETION DISK; STRONG GRAVITY; NGC-5506; REFLECTION AB We present the first unambiguous evidence of a broad (Gaussian width similar to 330 eV) component of the iron K-alpha fluorescent emission line in the X-ray obscured narrow-line Seyfert 1 galaxy, NGC 5506. This is the main result of a spectroscopic monitoring campaign on this source, performed with the XMM-Newton observatory between 2001 February and 2009 January. The broad line lacks extreme redward skewness. If modelled with a relativistic component, the profile of the line is consistent with a flat emissivity radial dependence (alpha similar or equal to 1.9). The disc inclination (similar or equal to 40 degrees) is nominally larger than typically observed in unobscured active galactic nuclei (AGNs), in agreement with most measurements of broadened iron lines in Seyfert 2 galaxies. The quality of the data allows us to decompose the full iron emission-line complex, and to study its long-term (time-scales of weeks to yr) variability pattern. The intensity of the neutral and narrow iron K-alpha core remains constant during the monitoring campaign. This indicates that the optically thick gas responsible for the non-relativistic reprocessing of the primary AGN continuum in NGC 5506 is probably located in the torus rather than in the optical broad-line region. C1 [Guainazzi, M.] European Space Agcy, European Space Astron Ctr, E-28691 Madrid, Spain. [Bianchi, S.; Matt, G.] Univ Roma Tre, Dipartimento Fis, I-00046 Rome, Italy. [Dadina, M.] INAF IASF Bo, I-40129 Bologna, Italy. [Kaastra, J.] SRON Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. [Malzac, J.] Univ Toulouse, Ctr Etud Spatiale Rayonnements, CNRS, F-31028 Toulouse 4, France. [Risaliti, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Risaliti, G.] INAF Osservatorio Arcetri, I-50125 Florence, Italy. RP Guainazzi, M (reprint author), European Space Agcy, European Space Astron Ctr, POB 78, E-28691 Madrid, Spain. EM Matteo.Guainazzi@sciops.esa.int RI Bianchi, Stefano/B-4804-2010; OI Bianchi, Stefano/0000-0002-4622-4240; Risaliti, Guido/0000-0002-3556-977X; Dadina, Mauro/0000-0002-7858-7564 FU ESA member states; National Aeronautics and Space Administration (NASA) FX This work is based on observations obtained with XMM-Newton, a European Space Agency (ESA) science mission, with instruments and contributions directly funded by ESA member states and the National Aeronautics and Space Administration (NASA). Useful discussions with Michal Dovciak and Giovanni Miniutti are gratefully acknowledged. A careful reading of the manuscript by an anonymous referee significantly improved the presentation of the results. NR 72 TC 24 Z9 24 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 AUG 11 PY 2010 VL 406 IS 3 BP 2013 EP 2022 DI 10.1111/j.1365-2966.2010.16805.x PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 635PT UT WOS:000280669200043 ER PT J AU Hughes, A Wong, T Ott, J Muller, E Pineda, JL Mizuno, Y Bernard, JP Paradis, D Maddison, S Reach, WT Staveley-Smith, L Kawamura, A Meixner, M Kim, S Onishi, T Mizuno, N Fukui, Y AF Hughes, A. Wong, T. Ott, J. Muller, E. Pineda, J. L. Mizuno, Y. Bernard, J. -P. Paradis, D. Maddison, S. Reach, W. T. Staveley-Smith, L. Kawamura, A. Meixner, M. Kim, S. Onishi, T. Mizuno, N. Fukui, Y. TI Physical properties of giant molecular clouds in the Large Magellanic Cloud SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE ISM: clouds; ISM: molecules; galaxies: ISM; Magellanic Clouds ID SEST KEY PROGRAM; REGULATED STAR-FORMATION; GALAXY EVOLUTION SAGE; ALL-SKY SURVEY; SPITZER SURVEY; GRAVITATIONAL-INSTABILITY; INTERSTELLAR CLOUDS; IRREGULAR GALAXIES; APERTURE SYNTHESIS; LINEAR-REGRESSION AB The Magellanic Mopra Assessment (MAGMA) is a high angular resolution 12CO (J = 1 -> 0) mapping survey of giant molecular clouds (GMCs) in the Large Magellanic Cloud (LMC) and Small Magellanic Cloud using the Mopra Telescope. Here we report on the basic physical properties of 125 GMCs in the LMC that have been surveyed to date. The observed clouds exhibit scaling relations that are similar to those determined for Galactic GMCs, although LMC clouds have narrower linewidths and lower CO luminosities than Galactic clouds of a similar size. The average mass surface density of the LMC clouds is 50 M(circle dot) pc-2, approximately half that of GMCs in the inner Milky Way. We compare the properties of GMCs with and without signs of massive star formation, finding that non-star-forming GMCs have lower peak CO brightness than star-forming GMCs. We compare the properties of GMCs with estimates for local interstellar conditions: specifically, we investigate the H i column density, radiation field, stellar mass surface density and the external pressure. Very few cloud properties demonstrate a clear dependence on the environment; the exceptions are significant positive correlations between (i) the H i column density and the GMC velocity dispersion, (ii) the stellar mass surface density and the average peak CO brightness and (iii) the stellar mass surface density and the CO surface brightness. The molecular mass surface density of GMCs without signs of massive star formation shows no dependence on the local radiation field, which is inconsistent with the photoionization-regulated star formation theory proposed by McKee. We find some evidence that the mass surface density of the MAGMA clouds increases with the interstellar pressure, as proposed by Elmegreen, but the detailed predictions of this model are not fulfilled once estimates for the local radiation field, metallicity and GMC envelope mass are taken into account. C1 [Hughes, A.; Maddison, S.] Swinburne Univ Technol, Ctr Supercomp & Astrophys, Hawthorn, Vic 3122, Australia. [Hughes, A.] CSIRO Australia Telescope Natl Facil, Epping, NSW 1710, Australia. [Wong, T.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Ott, J.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Muller, E.; Mizuno, Y.; Kawamura, A.; Onishi, T.; Mizuno, N.; Fukui, Y.] Nagoya Univ, Dept Astrophys, Chikusa Ku, Nagoya, Aichi 4648602, Japan. [Pineda, J. L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bernard, J. -P.] Univ Toulouse 3, Ctr Etud Spatiale Rayonnements, F-31028 Toulouse 4, France. [Paradis, D.; Reach, W. T.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Reach, W. T.] Univ Space Res Assoc, Stratospher Observ Infrared Astron, Moffett Field, CA 94035 USA. [Staveley-Smith, L.] Univ Western Australia, Int Ctr Radio Astron Res, Crawley, WA 6009, Australia. [Meixner, M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Meixner, M.] Harvard Smithsonian Astrophys, Radio & Geoastron Div, Cambridge, MA 02138 USA. [Kim, S.] Sejong Univ, Dept Astron & Space Sci, Seoul 143747, South Korea. [Onishi, T.] Osaka Prefecture Univ, Dept Phys Sci, Osaka 5998531, Japan. [Mizuno, N.] Natl Inst Nat Sci, Natl Astron Observ Japan, ALMA J Project Off, Mitaka, Tokyo 1818588, Japan. RP Hughes, A (reprint author), Swinburne Univ Technol, Ctr Supercomp & Astrophys, Hawthorn, Vic 3122, Australia. EM ahughes@astro.swin.edu.au RI Staveley-Smith, Lister/A-1683-2011 OI Reach, William/0000-0001-8362-4094; Staveley-Smith, Lister/0000-0002-8057-0294 FU NSF [08-07323]; University of Illinois; National Science Foundation; NASA; Australian Research Council; Korean government (MEST) [2009-0062866] FX We thank Christian Henkel, Jonathan Seale and Min Wang for their assistance with MAGMA observations. We also thank the staff at the ATNF for observing support and Robert Gruendl for providing the stellar mass surface density image. We acknowledge extensive use of NASA's Astrophysics Data System Bibliographic Services. TW is supported by NSF grant 08-07323 and the University of Illinois. JO is supported by the National Radio Astronomy Observatory (NRAO) which is operated by Associated Universities, Inc., under cooperative agreement with the National Science Foundation. JLP is supported by an appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory, California Institute of Technology, administered by Oak Ridge Associated Universities through a contract with NASA. AH, J-PB and DP are grateful to the Australian Research Council for financial assistance during this project via the Linkage International scheme (Australia-France Co-operation Fund in Astronomy). SK is supported in part by the National Research Foundation of Korea (NRF) grant funded by the Korean government (MEST) 2009-0062866. AH thanks Erik Rosolowsky, Adam Leroy, Alberto Bolatto, Kaye Marion and Michael Murphy for helpful discussions. We thank the referee for constructive criticism that improved the analysis in this paper. NR 93 TC 51 Z9 51 U1 0 U2 4 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD AUG 11 PY 2010 VL 406 IS 3 BP 2065 EP 2086 DI 10.1111/j.1365-2966.2010.16829.x PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 635PT UT WOS:000280669200048 ER PT J AU Strafella, F Elia, D Campeggio, L Giannini, T Lorenzetti, D Marengo, M Smith, HA Fazio, G De Luca, M Massi, F AF Strafella, F. Elia, D. Campeggio, L. Giannini, T. Lorenzetti, D. Marengo, M. Smith, H. A. Fazio, G. De Luca, M. Massi, F. TI THE SPITZER-IRAC POINT-SOURCE CATALOG OF THE VELA-D CLOUD SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared: stars; ISM: clouds; ISM: individual objects (Vela Molecular Ridge); stars: formation; stars: pre-main sequence; surveys ID YOUNG STELLAR OBJECTS; ARRAY CAMERA IRAC; CLASS-I SOURCES; STAR-FORMATION; MOLECULAR CLOUDS; C2D SURVEY; INTERSTELLAR CLOUDS; SPACE-TELESCOPE; OPHIUCHI CLOUD; RIDGE AB This paper presents the observations of Cloud D in the Vela Molecular Ridge, obtained with the Infrared Array Camera (IRAC) camera on board the Spitzer Space Telescope at the wavelengths lambda = 3.6, 4.5, 5.8, and 8.0 mu m. A photometric catalog of point sources, covering a field of approximately 1.2 deg(2), has been extracted and complemented with additional available observational data in the millimeter region. Previous observations of the same region, obtained with the Spitzer MIPS camera in the photometric bands at 24 mu m and 70 mu m, have also been reconsidered to allow an estimate of the spectral slope of the sources in a wider spectral range. A total of 170,299 point sources, detected at the 5 sigma sensitivity level in at least one of the IRAC bands, have been reported in the catalog. There were 8796 sources for which good quality photometry was obtained in all four IRAC bands. For this sample, a preliminary characterization of the young stellar population based on the determination of spectral slope is discussed; combining this with diagnostics in the color-magnitude and color-color diagrams, the relative population of young stellar objects (YSOs) in different evolutionary classes has been estimated and a total of 637 candidate YSOs have been selected. The main differences in their relative abundances have been highlighted and a brief account for their spatial distribution is given. The star formation rate has also been estimated and compared with the values derived for other star-forming regions. Finally, an analysis of the spatial distribution of the sources by means of the two-point correlation function shows that the younger population, constituted by the Class I and flat-spectrum sources, is significantly more clustered than the Class II and III sources. C1 [Strafella, F.; Elia, D.; Campeggio, L.] Univ Salento, Dipartimento Fis, I-73100 Lecce, Italy. [Elia, D.] Univ Lisbon, Fac Ciencias, Ctr Astron & Astrofis, Observ Astron Lisboa, P-1349018 Lisbon, Portugal. [Giannini, T.; Lorenzetti, D.; De Luca, M.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy. [Marengo, M.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Smith, H. A.; Fazio, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [De Luca, M.] Observ Paris, CNRS, UMR 8112, LERMA LRA, F-75231 Paris, France. [De Luca, M.] Ecole Normale Super, F-75231 Paris, France. [Massi, F.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. RP Strafella, F (reprint author), Univ Salento, Dipartimento Fis, CP 193, I-73100 Lecce, Italy. EM francesco.strafella@le.infn.it; eliad@oal.ul.pt; loretta.campeggio@le.infn.it; giannini@oa-roma.inaf.it; dloren@oa-roma.inaf.it; mmarengo@cfa.harvard.edu; hsmith@cfa.harvard.edu; massimo.de.luca@lra.ens.fr; fmassi@arcetri.astro.it OI Lorenzetti, Dario/0000-0001-6415-4162; Massi, Fabrizio/0000-0001-6407-8032; Elia, Davide/0000-0002-9120-5890; Giannini, Teresa/0000-0002-0224-096X FU European Commission [MRTN-CT-2006-035890]; Italian Space Agency (ASI); NASA; NASA through JPL/Caltech FX We thank Joao Lin Yun, Luca Olmi, and Berlinda Maiolo for many helpful discussions. D. E. has been partly supported by the European Commission FP6 Marie Curie Research Training Network CONSTELLATION (MRTN-CT-2006-035890). F. S. acknowledges partial support by the Italian Space Agency (ASI). This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. NR 44 TC 6 Z9 6 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 AUG 10 PY 2010 VL 719 IS 1 BP 9 EP 27 DI 10.1088/0004-637X/719/1/9 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 635KD UT WOS:000280653100002 ER PT J AU Kapyla, PJ Brandenburg, A Korpi, MJ Snellman, JE Narayan, R AF Kapyla, Petri J. Brandenburg, Axel Korpi, Maarit J. Snellman, Jan E. Narayan, Ramesh TI ANGULAR MOMENTUM TRANSPORT IN CONVECTIVELY UNSTABLE SHEAR FLOWS SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; convection; stars: rotation; Sun: rotation; turbulence ID TURBULENT CONVECTION; NUMERICAL SIMULATIONS; DIFFERENTIAL ROTATION; REYNOLDS STRESS; DIFFUSION; DISKS; INSTABILITY AB Angular momentum transport due to hydrodynamic turbulent convection is studied using local three-dimensional numerical simulations employing the shearing box approximation. We determine the turbulent viscosity from non-rotating runs over a range of values of the shear parameter and use a simple analytical model in order to extract the non-diffusive contribution (Lambda-effect) to the stress in runs where rotation is included. Our results suggest that the turbulent viscosity is on the order of the mixing length estimate and weakly affected by rotation. The Lambda-effect is non-zero and a factor of 2-4 smaller than the turbulent viscosity in the slow rotation regime. We demonstrate that for Keplerian shear, the angular momentum transport can change sign and be outward when the rotation period is greater than the turnover time, i.e., when the Coriolis number is below unity. This result seems to be relatively independent of the value of the Rayleigh number. C1 [Kapyla, Petri J.; Korpi, Maarit J.; Snellman, Jan E.] Univ Helsinki, Div Geophys & Astron, Dept Phys, FI-00014 Helsinki, Finland. [Kapyla, Petri J.; Brandenburg, Axel] AlbaNova Univ Ctr, NORDITA, SE-10691 Stockholm, Sweden. [Brandenburg, Axel] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden. [Narayan, Ramesh] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kapyla, PJ (reprint author), Univ Helsinki, Div Geophys & Astron, Dept Phys, FI-00014 Helsinki, Finland. RI Kapyla, Maarit/E-9126-2013; Brandenburg, Axel/I-6668-2013; OI Kapyla, Maarit/0000-0002-9614-2200; Brandenburg, Axel/0000-0002-7304-021X; Narayan, Ramesh/0000-0002-1919-2730 FU Academy of Finland [121431, 112020]; Finnish Cultural Foundation; Swedish Research Council [621-2007-4064]; European Research Council [227952]; NSF [AST-0805832] FX The authors acknowledge the detailed comments of an anonymous referee. The computations were performed on the facilities hosted by CSC-IT Center for Science Ltd. in Espoo, Finland, which are administered by the Finnish Ministry of Education. We wish to acknowledge the DECI-DEISA network for granting computational resources to the project CONVDYN. Financial support from the Academy of Finland grants no. 121431 (PJK) and 112020 (MJK), the financial support of the Finnish Cultural Foundation (JES), as well as the Swedish Research Council grant 621-2007-4064 and the European Research Council AstroDyn Research Project 227952 (AB) are acknowledged. The authors acknowledge the hospitality of NORDITA during their visits. R.N. acknowledges the financial support from NSF grant AST-0805832. NR 37 TC 7 Z9 7 U1 1 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2010 VL 719 IS 1 BP 67 EP 76 DI 10.1088/0004-637X/719/1/67 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 635KD UT WOS:000280653100006 ER PT J AU Perets, HB Gualandris, A AF Perets, Hagai B. Gualandris, Alessia TI DYNAMICAL CONSTRAINTS ON THE ORIGIN OF THE YOUNG B-STARS IN THE GALACTIC CENTER SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; black hole physics; galaxies: nuclei; Galaxy: center; stars: kinematics and dynamics; stars: massive ID MASSIVE BLACK-HOLES; GRAVITATIONAL-WAVE SOURCES; SAGITTARIUS-A-ASTERISK; N-BODY SIMULATIONS; CENTER S-STARS; STELLAR ORBITS; HYPERVELOCITY STARS; ACCRETION DISK; CLUSTER; EVOLUTION AB Regular star formation is thought to be inhibited close to the massive black hole (MBH) in the Galactic center. Nevertheless, tens of young main-sequence B-stars have been observed in an isotropic distribution close to it. These stars are observed to have an apparently continuous distribution from very close to the MBH (<0.01 pc) and up to at least similar to 0.5 pc, suggesting a common origin. Various models have been suggested for the formation of the B-stars closest to the MBH (<0.05 pc; the S-stars), typically involving the migration of these stars from their original birthplace to their currently observed position. Here, we explore the orbital phase space distribution of the B-stars throughout the central parsec expected from the various suggested models for the origin of the B-stars. We find that most of these models have difficulties in explaining, by themselves, both the population of the S-stars (<0.05 pc) and the population of the young B-stars further away (up to 0.5 pc). Most models grossly overpredict the number of B-stars up to 0.5 pc, given the observed number of S-stars. Such models include the intermediate-mass black hole assisted cluster inspiral scenario, Kozai-like perturbations by two disks, spiral density waves migration in a gaseous disk, and some of the eccentric disk instability models. We focus on one of the other models, the massive perturbers induced binary disruption, which is consistent with both the S-stars and the extended population of B-stars further away. For this model, we use analytical arguments and N-body simulations to provide further observational predictions. These could be compared with future observations to further support this model, constrain it, or refute it. These predictions include the radial distribution of the young B-stars, their eccentricity distribution, and its dependence on distance from the MBH (higher eccentricities at larger distances from the MBH), as well as less specific expectations regarding their mass function. C1 [Perets, Hagai B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gualandris, Alessia] Max Planck Inst Astrophys, D-85741 Garching, Germany. RP Perets, HB (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM hperets@cfa.harvard.edu RI Gualandris, Alessia/A-9421-2011; Perets, Hagai/K-9605-2015 OI Perets, Hagai/0000-0002-5004-199X FU Israeli Science Foundation; Bi-national Fulbright program; Israeli industrial and commercial club; NASA [NNX07AH15G] FX We thank Tal Alexander for helpful discussions as well as Hendrik Bartko and Michiko Fujii for providing us with data from their observations and simulations, respectively. We also thank David Merritt for the use of the GRAPE cluster at the Rochester Institute of Technology. H. B. P. thanks the Israeli Science Foundation, the Bi-national Fulbright program and the Israeli industrial and commercial club for their support through the BIKURA (FIRST) and Ilan Ramon-Fulbright fellowships. A. G. is supported by grant NNX07AH15G from NASA. NR 65 TC 28 Z9 28 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2010 VL 719 IS 1 BP 220 EP 228 DI 10.1088/0004-637X/719/1/220 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 635KD UT WOS:000280653100019 ER PT J AU Cohen, O Drake, JJ Kashyap, VL Korhonen, H Elstner, D Gombosi, TI AF Cohen, O. Drake, J. J. Kashyap, V. L. Korhonen, H. Elstner, D. Gombosi, T. I. TI MAGNETIC STRUCTURE OF RAPIDLY ROTATING FK COMAE-TYPE CORONAE SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: activity; stars: coronae; stars: magnetic field ID FLIP-FLOP PHENOMENON; SOLAR-WIND; ACTIVE LONGITUDES; POLYTROPIC INDEX; SPOT EVOLUTION; COOL STARS; BERENICES; SURFACE; FIELDS; SUN AB We present a three-dimensional simulation of the corona of an FK Com-type rapidly rotating G giant using a magnetohydrodynamic model that was originally developed for the solar corona in order to capture the more realistic, non-potential coronal structure. We drive the simulation with surface maps for the radial magnetic field obtained from a stellar dynamo model of the FK Com system. This enables us to obtain the coronal structure for different field topologies representing different periods of time. We find that the corona of such an FK Com-like star, including the large-scale coronal loops, is dominated by a strong toroidal component of the magnetic field. This is a result of part of the field being dragged by the radial outflow, while the other part remains attached to the rapidly rotating stellar surface. This tangling of the magnetic field, in addition to a reduction in the radial flow component, leads to a flattening of the gas density profile with distance in the inner part of the corona. The three-dimensional simulation provides a global view of the coronal structure. Some aspects of the results, such as the toroidal wrapping of the magnetic field, should also be applicable to coronae on fast rotators in general, which our study shows can be considerably different from the well-studied and well-observed solar corona. Studying the global structure of such coronae should also lead to a better understanding of their related stellar processes, such as flares and coronal mass ejections, and in particular should lead to an improved understanding of mass and angular momentum loss from such systems. C1 [Cohen, O.; Drake, J. J.; Kashyap, V. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Korhonen, H.] European So Observ, D-85748 Garching, Germany. [Elstner, D.] Astrophys Inst Potsdam, D-14482 Potsdam, Germany. [Gombosi, T. I.] Univ Michigan, Ctr Space Environm Modeling, Ann Arbor, MI 48109 USA. RP Cohen, O (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Gombosi, Tamas/G-4238-2011; Korhonen, Heidi/E-3065-2016; OI Gombosi, Tamas/0000-0001-9360-4951; Korhonen, Heidi/0000-0003-0529-1161; Cohen, Ofer/0000-0003-3721-0215 FU SHINE through NSF [ATM-0823592 grant]; NASA [NNG05GM44G, NAS8-39073]; NASA ESS; NASA ESTO-CT; NSF KDI; DoD MURI FX O.C. is supported by SHINE through NSF ATM-0823592 grant, and by NASA-LWSTRT grant NNG05GM44G. J.J.D. and V. L. K. were funded by NASA contract NAS8-39073 to the Chandra X-ray Center. Simulation results were obtained using the Space Weather Modeling Framework, developed by the Center for Space Environment Modeling, at the University of Michigan with funding support from NASA ESS, NASA ESTO-CT, NSF KDI, and DoD MURI. NR 49 TC 9 Z9 9 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2010 VL 719 IS 1 BP 299 EP 306 DI 10.1088/0004-637X/719/1/299 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 635KD UT WOS:000280653100025 ER PT J AU Fadda, D Yan, L Lagache, G Sajina, A Lutz, D Wuyts, S Frayer, DT Marcillac, D Le Floc'h, E Caputi, K Spoon, HWW Veilleux, S Blain, A Helou, G AF Fadda, Dario Yan, Lin Lagache, Guilaine Sajina, Anna Lutz, Dieter Wuyts, Stijn Frayer, David T. Marcillac, Delphine Le Floc'h, Emeric Caputi, Karina Spoon, Henrik W. W. Veilleux, Sylvain Blain, Andrew Helou, George TI ULTRA-DEEP MID-INFRARED SPECTROSCOPY OF LUMINOUS INFRARED GALAXIES AT z similar to 1 AND z similar to 2 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: high-redshift; galaxies: starburst; infrared: galaxies ID SPITZER-SPACE-TELESCOPE; STAR-FORMING GALAXIES; POLYCYCLIC AROMATIC-HYDROCARBON; ACTIVE GALACTIC NUCLEI; S-SELECTED GALAXIES; FIELD-SOUTH SURVEY; SUBMILLIMETER GALAXIES; HIGH-REDSHIFT; RED GALAXIES; STARBURST GALAXIES AB We present ultra-deep mid-infrared spectra of 48 infrared-luminous galaxies in the GOODS-south field obtained with the Infrared Spectrograph on the Spitzer Space Telescope. These galaxies are selected among faint infrared sources (0.14-0.5 mJy at 24 mu m) in two redshift bins (0.76-1.05 and 1.75-2.4) to sample the major contributors to the cosmic infrared background at the most active epochs. We estimate redshifts for 92% of the sample using polycyclic aromatic (PAH) and Si absorption features obtaining, in particular, eight new redshifts difficult to measure from ground-based observations. Only a few of these galaxies (5% at z similar to 1 and 12% at z similar to 2) have their total infrared luminosity dominated by emission from active galactic nuclei (AGNs). The averaged mid-IR spectrum of the z similar to 1 luminous infrared galaxies (LIRGs) is a very good match to the averaged spectrum of local starbursts. The averaged spectrum of the z similar to 2 ultra-luminous infrared galaxies (ULIRGs), because of a deeper Si absorption, is better fitted by the averaged spectrum of H II-like local ULIRGs. Combining this sample with other published data, we find that 6.2 mu m PAH equivalent widths (EW) reach a plateau of similar to 1 mu m for L-24 mu m less than or similar to 10(11) L-circle dot. At higher luminosities, EW6.2 mu m anti-correlates with L-24 mu m. Intriguingly, high-z ULIRGs and sub-millimeter galaxies (SMGs) lie above the local EW6.2 mu m-L-24 mu m relationship suggesting that, at a given luminosity, high-z ULIRGs have AGN contributions to their dust emission lower than those of local counterparts. A quantitative analysis of their morphology shows that most of the luminous IR galaxies have morphologies similar to those of IR-quiet galaxies at the same redshift. All z similar to 2 ULIRGs of our sample are IR-excess BzK galaxies and most of them have L-FIR/L-1600 angstrom ratios higher than those of starburst galaxies at a given UV slope. The "IR excess" is mostly due to strong 7.7 mu m PAH emission and underestimation of UV dust extinction. On the basis of the AGN-powered L-6 mu m continuum measured directly from the mid-IR spectra, we estimate an average intrinsic X-ray AGN luminosity of L2-10 (keV) = (0.1 +/- 0.6) x 1043 erg s(-1), a value substantially lower than the prediction by Daddi et al. C1 [Fadda, Dario; Yan, Lin; Frayer, David T.; Helou, George] CALTECH, IPAC, Pasadena, CA 91125 USA. [Lagache, Guilaine; Marcillac, Delphine] Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France. [Lagache, Guilaine; Marcillac, Delphine] CNRS, UMR 8617, F-91405 Orsay, France. [Sajina, Anna] Haverford Coll, Haverford, PA 19041 USA. [Lutz, Dieter] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Wuyts, Stijn] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Le Floc'h, Emeric] CEA Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France. [Caputi, Karina] Univ Edinburgh, Royal Observ, SUPA Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Spoon, Henrik W. W.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Veilleux, Sylvain] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Blain, Andrew] CALTECH, Dept Astron, Pasadena, CA 91125 USA. RP Fadda, D (reprint author), CALTECH, IPAC, Pasadena, CA 91125 USA. EM fadda@ipac.caltech.edu; lyan@ipac.caltech.edu FU NASA FX This research made use of Tiny Tim/Spitzer, developed by John Krist for the Spitzer Science Center. The Center is managed by the California Institute of Technology under a contract with NASA. We are grateful to Haojing Yan for providing us the reduced NICMOS H-band stamp images for some of our sources. We thank P. Capak for helpful discussions. We are grateful to the anonymous referee for the detailed reading of the paper and for many ideas and suggestions to improve the quality of the paper. Support for this work was provided by NASA through an award issued by JPL/Caltech. S. Wuyts acknowledges support from the W.M. Keck Foundation. NR 99 TC 41 Z9 41 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 AUG 10 PY 2010 VL 719 IS 1 BP 425 EP 450 DI 10.1088/0004-637X/719/1/425 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 635KD UT WOS:000280653100037 ER PT J AU Di Stefano, R AF Di Stefano, R. TI THE PROGENITORS OF TYPE Ia SUPERNOVAE. II. ARE THEY DOUBLE-DEGENERATE BINARIES? THE SYMBIOTIC CHANNEL SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: symbiotic; distance scale; supernovae: general; white dwarfs; X-rays: general ID X-RAY SOURCES; ACCRETING WHITE-DWARFS; FINAL MASS RELATION; QUASI-SOFT; BLACK-HOLE; EXTERNAL GALAXIES; SUPERSOFT SOURCES; GALACTIC-CENTER; SHELL FLASHES; XMM-NEWTON AB In order for a white dwarf (WD) to achieve the Chandrasekhar mass, M-C, and explode as a Type Ia supernova (SNIa), it must interact with another star, either accreting matter from or merging with it. The failure to identify the class or classes of binaries which produce SNeIa is the long-standing "progenitor problem." Its solution is required if we are to utilize the full potential of SNeIa to elucidate basic cosmological and physical principles. In single-degenerate models, a WD accretes and burns matter at high rates. Nuclear-burning white dwarfs (NBWDs) with mass close to MC are hot and luminous, potentially detectable as supersoft X-ray sources (SSSs). In previous work, we showed that >90%-99% of the required number of progenitors do not appear as SSSs during most of the crucial phase of mass increase. The obvious implication might be that double-degenerate binaries form the main class of progenitors. We show in this paper, however, that many binaries that later become double degenerates must pass through a long-lived NBWD phase during which they are potentially detectable as SSSs. The paucity of SSSs is therefore not a strong argument in favor of double-degenerate models. Those NBWDs that are the progenitors of double-degenerate binaries are likely to appear as symbiotic binaries for intervals >10(6) years. In fact, symbiotic pre-double-degenerates should be common, whether or not the WDs eventually produce SNeIa. The key to solving the Type Ia progenitor problem lies in understanding the appearance of NBWDs. Most of them do not appear as SSSs most of the time. We therefore consider the evolution of NBWDs to address the question of what their appearance may be and how we can hope to detect them. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Di Stefano, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU NASA; Smithsonian Institution FX It is a pleasure to acknowledge helpful conversations, most recently with Scott Kenyon and Jeno Sokoloski, and also with participants (especially Ed van den Heuvel, Lev Yungelson, and Jim Liebert), of the KITP conference and workshop on Accretion and Explosion held at UC Santa Barbara in 2007. I also thank the anonymous referee for useful comments. This work was supported in part by an LTSA grant from NASA and by funding from the Smithsonian Institution. NR 60 TC 43 Z9 43 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 AUG 10 PY 2010 VL 719 IS 1 BP 474 EP 482 DI 10.1088/0004-637X/719/1/474 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 635KD UT WOS:000280653100041 ER PT J AU Luketic, S Proga, D Kallman, TR Raymond, JC Miller, JM AF Luketic, S. Proga, D. Kallman, T. R. Raymond, J. C. Miller, J. M. TI ON THE PROPERTIES OF THERMAL DISK WINDS IN X-RAY TRANSIENT SOURCES: A CASE STUDY OF GRO J1655-40 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; hydrodynamics; methods: numerical ID COMPTON-HEATED WINDS; ACCRETION DISKS; RADIATION; CORONAE; LINE; SPECTROSCOPY; EMISSION; DYNAMICS; OUTFLOW; FLOWS AB We present the results of hydrodynamical simulations of the disk photosphere irradiated by strong X-rays produced in the innermost part of the disk of an accreting black hole. As expected, the irradiation heats the photosphere and drives a thermal wind. To apply our results to the well-studied X-ray transient source GRO J1655-40, we adopted the observed mass of its black hole and the observed properties of its X-ray radiation. To compare the results with the observations, we also computed transmitted X-ray spectra based on the wind solution. Our main finding is that the density of the fast-moving part of the wind is more than 1 order of magnitude lower than that inferred from the observations. Consequently, the model fails to predict spectra with line absorption as strong and as blueshifted as those observed. However, despite the thermal wind being weak and Compton thin, the ratio between the mass-loss rate and the mass-accretion rate is about seven. This high ratio is insensitive to the accretion luminosity, in the limit of lower luminosities. Most of the mass is lost from the disk between 0.07 and 0.2 of the Compton radius. We discovered that beyond this range the wind solution is self-similar. In particular, soon after it leaves the disk, the wind flows at a constant angle with respect to the disk. Overall, the thermal winds generated in our comprehensive simulations do not match the wind spectra observed in GRO J1655-40. This supports the conclusion of Miller et al. and Kallman et al. that the wind in GRO J1655-40, and possibly in other X-ray transients, may be driven by magnetic processes. This in turn implies that the disk wind carries even more material than our simulations predict and as such has a very significant impact on the accretion disk structure and dynamics. C1 [Luketic, S.; Proga, D.] Univ Nevada, Dept Phys, Las Vegas, NV 89154 USA. [Kallman, T. R.] NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. [Raymond, J. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Miller, J. M.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. RP Luketic, S (reprint author), Univ Nevada, Dept Phys, Las Vegas, NV 89154 USA. EM stefan@physics.unlv.edu; dproga@physics.unlv.edu FU NASA [NAS 8-39073] FX We thank Tim Waters for his comments on the manuscript. We acknowledge support provided by the Chandra awards TM8-9004X and TM0-11010X issued by the Chandra X-Ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS 8-39073. NR 26 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 AUG 10 PY 2010 VL 719 IS 1 BP 515 EP 522 DI 10.1088/0004-637X/719/1/515 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 635KD UT WOS:000280653100045 ER PT J AU Forbrich, J Posselt, B Covey, KR Lada, CJ AF Forbrich, Jan Posselt, Bettina Covey, Kevin R. Lada, Charles J. TI NOTHING TO HIDE: AN X-RAY SURVEY FOR YOUNG STELLAR OBJECTS IN THE PIPE NEBULA SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: pre-main sequence; X-rays: stars ID SPITZER C2D SURVEY; T-TAURI STARS; ROSAT PSPC CATALOG; ALL-SKY SURVEY; MASS FUNCTION; ORION NEBULA; DENSE CORES; REGION; EXTINCTION AB We have previously analyzed sensitive mid-infrared observations to establish that the Pipe Nebula (PiN) has a very low star formation efficiency. That study focused on young stellar objects (YSOs) with excess infrared emission (i.e., protostars and pre-main-sequence stars with disks), however, and could have missed a population of more evolved pre-main-sequence stars or Class III objects (i.e., young stars with dissipated disks that no longer show excess infrared emission). Evolved pre-main-sequence stars are X-ray bright, so we have used ROSAT All-Sky Survey data to search for diskless pre-main-sequence stars throughout the PiN. We have also analyzed archival XMM-Newton observations of three prominent areas within the Pipe: Barnard 59 (B 59), containing a known cluster of YSOs; Barnard 68, a dense core that has yet to form stars; and the Pipe molecular ring, a high-extinction region in the bowl of the Pipe. We also characterize the X-ray properties of YSOs in B 59. The ROSAT and XMM-Newton data provide no indication of a significant population of more evolved pre-main-sequence stars within the Pipe, reinforcing our previous measurement of the Pipe's very low star formation efficiency. C1 [Forbrich, Jan; Posselt, Bettina; Covey, Kevin R.; Lada, Charles J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Forbrich, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Posselt, Bettina/0000-0003-2317-9747; Covey, Kevin/0000-0001-6914-7797 NR 27 TC 10 Z9 10 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2010 VL 719 IS 1 BP 691 EP 699 DI 10.1088/0004-637X/719/1/691 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 635KD UT WOS:000280653100061 ER PT J AU Vieira, JD Crawford, TM Switzer, ER Ade, PAR Aird, KA Ashby, MLN Benson, BA Bleem, LE Brodwin, M Carlstrom, JE Chang, CL Cho, HM Crites, AT de Haan, T Dobbs, MA Everett, W George, EM Gladders, M Hall, NR Halverson, NW High, FW Holder, GP Holzapfel, WL Hrubes, JD Joy, M Keisler, R Knox, L Lee, AT Leitch, EM Lueker, M Marrone, DP McIntyre, V McMahon, JJ Mehl, J Meyer, SS Mohr, JJ Montroy, TE Padin, S Plagge, T Pryke, C Reichardt, CL Ruhl, JE Schaffer, KK Shaw, L Shirokoff, E Spieler, HG Stalder, B Staniszewski, Z Stark, AA Vanderlinde, K Walsh, W Williamson, R Yang, Y Zahn, O Zenteno, A AF Vieira, J. D. Crawford, T. M. Switzer, E. R. Ade, P. A. R. Aird, K. A. Ashby, M. L. N. Benson, B. A. Bleem, L. E. Brodwin, M. Carlstrom, J. E. Chang, C. L. Cho, H. -M. Crites, A. T. de Haan, T. Dobbs, M. A. Everett, W. George, E. M. Gladders, M. Hall, N. R. Halverson, N. W. High, F. W. Holder, G. P. Holzapfel, W. L. Hrubes, J. D. Joy, M. Keisler, R. Knox, L. Lee, A. T. Leitch, E. M. Lueker, M. Marrone, D. P. McIntyre, V. McMahon, J. J. Mehl, J. Meyer, S. S. Mohr, J. J. Montroy, T. E. Padin, S. Plagge, T. Pryke, C. Reichardt, C. L. Ruhl, J. E. Schaffer, K. K. Shaw, L. Shirokoff, E. Spieler, H. G. Stalder, B. Staniszewski, Z. Stark, A. A. Vanderlinde, K. Walsh, W. Williamson, R. Yang, Y. Zahn, O. Zenteno, A. TI EXTRAGALACTIC MILLIMETER-WAVE SOURCES IN SOUTH POLE TELESCOPE SURVEY DATA: SOURCE COUNTS, CATALOG, AND STATISTICS FOR AN 87 SQUARE-DEGREE FIELD SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: high-redshift; submillimeter: galaxies; surveys ID SPECTRUM RADIO-SOURCES; STAR-FORMING GALAXIES; SCUBA SUPER-MAP; GOODS-N FIELD; SUBMILLIMETER-SELECTED GALAXIES; COMPACT STEEP-SPECTRUM; 1200-MU-M MAMBO SURVEY; ALL-SKY SURVEY; 1.1 MM SURVEY; NUMBER COUNTS AB We report the results of an 87 deg(2) point-source survey centered at R. A. 5(h)30(m), decl. -55 degrees taken with the South Pole Telescope at 1.4 and 2.0 mm wavelengths with arcminute resolution and milli-Jansky depth. Based on the ratio of flux in the two bands, we separate the detected sources into two populations, one consistent with synchrotron emission from active galactic nuclei and the other consistent with thermal emission from dust. We present source counts for each population from 11 to 640 mJy at 1.4 mm and from 4.4 to 800mJy at 2.0 mm. The 2.0 mm counts are dominated by synchrotron-dominated sources across our reported flux range; the 1.4 mm counts are dominated by synchrotron-dominated sources above similar to 15 mJy and by dust-dominated sources below that flux level. We detect 141 synchrotron-dominated sources and 47 dust-dominated sources at signal-to-noise ratio S/N > 4.5 in at least one band. All of the most significantly detected members of the synchrotron-dominated population are associated with sources in previously published radio catalogs. Some of the dust-dominated sources are associated with nearby (z << 1) galaxies whose dust emission is also detected by the Infrared Astronomy Satellite. However, most of the bright, dust-dominated sources have no counterparts in any existing catalogs. We argue that these sources represent the rarest and brightestmembers of the population commonly referred to as submillimeter galaxies (SMGs). Because these sources are selected at longer wavelengths than in typical SMG surveys, they are expected to have a higher mean redshift distribution and may provide a new window on galaxy formation in the early universe. C1 [Vieira, J. D.; Crawford, T. M.; Switzer, E. R.; Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Crites, A. T.; Gladders, M.; Keisler, R.; Marrone, D. P.; McMahon, J. J.; Mehl, J.; Meyer, S. S.; Padin, S.; Plagge, T.; Pryke, C.; Schaffer, K. K.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Vieira, J. D.; Bleem, L. E.; Carlstrom, J. E.; Keisler, R.; Meyer, S. S.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. [Vieira, J. D.; Carlstrom, J. E.; Chang, C. L.; Keisler, R.; McMahon, J. J.; Meyer, S. S.; Pryke, C.; Schaffer, K. K.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Crawford, T. M.; Carlstrom, J. E.; Crites, A. T.; Gladders, M.; Meyer, S. S.; Padin, S.] Univ Chicago, Ctr Astron & Astrophys, Chicago, IL 60637 USA. [Ade, P. A. R.] Cardiff Univ, Dept Phys & Astron, Cardiff CF24 3YB, S Glam, Wales. [Ashby, M. L. N.; Brodwin, M.; Stalder, B.; Stark, A. A.; Walsh, W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Cho, H. -M.; George, E. M.; Holzapfel, W. L.; Lee, A. T.; Lueker, M.; Plagge, T.; Reichardt, C. L.; Shirokoff, E.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [de Haan, T.; Dobbs, M. A.; Holder, G. P.; Shaw, L.; Vanderlinde, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Hall, N. R.; Knox, L.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Halverson, N. W.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Halverson, N. W.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA. [High, F. W.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Joy, M.] NASA, George C Marshall Space Flight Ctr, Dept Space Sci, VP62, Huntsville, AL 35812 USA. [Lee, A. T.; Leitch, E. M.; Spieler, H. G.] Univ Calif Berkeley, Lawrence Berkeley Lab, Div Phys, Berkeley, CA 94720 USA. [McIntyre, V.] CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. [McMahon, J. J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Mohr, J. J.] Univ Munich, Dept Phys, D-81679 Munich, Germany. [Mohr, J. J.] Excellence Cluster Universe, D-85748 Garching, Germany. [Mohr, J. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Montroy, T. E.; Ruhl, J. E.; Staniszewski, Z.] Case Western Reserve Univ, Dept Phys, Cleveland, OH 44106 USA. [Montroy, T. E.; Ruhl, J. E.; Staniszewski, Z.] Case Western Reserve Univ, Ctr Educ & Res Cosmol & Astrophys, Cleveland, OH 44106 USA. [Shaw, L.] Yale Univ, Dept Phys, New Haven, CT 06520 USA. [Yang, Y.; Zenteno, A.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Yang, Y.; Zenteno, A.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA. [Zahn, O.] Univ Calif Berkeley, Berkeley Ctr Cosmol Phys, Dept Phys, Berkeley, CA 94720 USA. [Marrone, D. P.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. RP Vieira, JD (reprint author), Univ Chicago, Kavli Inst Cosmol Phys, 5640 S Ellis Ave, Chicago, IL 60637 USA. EM vieira@caltech.edu RI Williamson, Ross/H-1734-2015; Holzapfel, William/I-4836-2015; OI Williamson, Ross/0000-0002-6945-2975; Marrone, Daniel/0000-0002-2367-1080; Aird, Kenneth/0000-0003-1441-9518; Reichardt, Christian/0000-0003-2226-9169; Stark, Antony/0000-0002-2718-9996 FU Canadian Astronomy Data Centre; National Research Council of Canada; Canadian Space Agency; Commonwealth of Australia; CSIRO; Legacy Archive for Microwave Background Data Analysis (LAMBDA); NASA Office of Space Science FX This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France, 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, and the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research used the facilities of the Canadian Astronomy Data Centre operated by the National Research Council of Canada with the support of the Canadian Space Agency. The ATCA is part of the Australia Telescope, which is funded by the Commonwealth of Australia for operation as a national facility managed by the CSIRO. Some of the results in this paper have been derived using the HEALPix (G ' orski et al. 2005) package. We acknowledge the use of the Legacy Archive for Microwave Background Data Analysis (LAMBDA). Support for LAMBDA is provided by the NASA Office of Space Science. NR 107 TC 157 Z9 157 U1 1 U2 11 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2010 VL 719 IS 1 BP 763 EP 783 DI 10.1088/0004-637X/719/1/763 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 635KD UT WOS:000280653100068 ER PT J AU Dufour, P Kilic, M Fontaine, G Bergeron, P Lachapelle, FR Kleinman, SJ Leggett, SK AF Dufour, P. Kilic, M. Fontaine, G. Bergeron, P. Lachapelle, F-R. Kleinman, S. J. Leggett, S. K. TI THE DISCOVERY OF THE MOST METAL-RICH WHITE DWARF: COMPOSITION OF A TIDALLY DISRUPTED EXTRASOLAR DWARF PLANET SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: abundances; stars: atmospheres; stars: evolution; white dwarfs ID ABUNDANCE PATTERNS; DUSTY DISK; ELEMENT ABUNDANCES; DEBRIS DISKS; MINOR PLANET; DZ STARS; GD 40; COOL; ACCRETION; GD-362 AB Cool white dwarf stars are usually found to have an outer atmosphere that is practically pure in hydrogen or helium. However, a small fraction have traces of heavy elements that must originate from the accretion of extrinsic material, most probably circumstellar matter. Upon examining thousands of Sloan Digital Sky Survey (SDSS) spectra, we discovered that the helium-atmosphere white dwarf SDSS J073842.56+ 183509.6 shows the most severe metal pollution ever seen in the outermost layers of such stars. We present here a quantitative analysis of this exciting star by combining high signal-to-noise ratio follow-up spectroscopic and photometric observations with model atmospheres and evolutionary models. We determine the global structural properties of our target star, as well as the abundances of the most significant pollutants in its atmosphere, i. e., H, O, Na, Mg, Si, Ca, and Fe. The relative abundances of these elements imply that the source of the accreted material has a composition similar to that of Bulk Earth. We also report the signature of a circumstellar disk revealed through a large infrared excess in JHK photometry. Combined with our inferred estimate of the mass of the accreted material, this strongly suggests that we are witnessing the remains of a tidally disrupted extrasolar body that was as large as Ceres. C1 [Dufour, P.; Fontaine, G.; Bergeron, P.; Lachapelle, F-R.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. [Kilic, M.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Kleinman, S. J.; Leggett, S. K.] No Operat Ctr, Gemini Observ, Hilo, HI 96720 USA. RP Dufour, P (reprint author), Univ Montreal, Dept Phys, CP 6128, Montreal, PQ H3C 3J7, Canada. EM dufourpa@astro.umontreal.ca OI Lachapelle, Francois-Rene/0000-0003-4997-0449; Leggett, Sandy/0000-0002-3681-2989 NR 43 TC 53 Z9 53 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2010 VL 719 IS 1 BP 803 EP 809 DI 10.1088/0004-637X/719/1/803 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 635KD UT WOS:000280653100071 ER PT J AU Kashyap, VL van Dyk, DA Connors, A Freeman, PE Siemiginowska, A Xu, J Zezas, A AF Kashyap, Vinay L. van Dyk, David A. Connors, Alanna Freeman, Peter E. Siemiginowska, Aneta Xu, Jin Zezas, Andreas TI ON COMPUTING UPPER LIMITS TO SOURCE INTENSITIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods: data analysis; methods: statistical ID FLUX UPPER LIMITS; X-RAY-EMISSION; RADIO-EMISSION; COUNTS; SPECTRA; RATIO AB A common problem in astrophysics is determining how bright a source could be and still not be detected in an observation. Despite the simplicity with which the problem can be stated, the solution involves complicated statistical issues that require careful analysis. In contrast to the more familiar confidence bound, this concept has never been formally analyzed, leading to a great variety of often ad hoc solutions. Here we formulate and describe the problem in a self-consistent manner. Detection significance is usually defined by the acceptable proportion of false positives (background fluctuations that are claimed as detections, or Type I error), and we invoke the complementary concept of false negatives (real sources that go undetected, or Type II error), based on the statistical power of a test, to compute an upper limit to the detectable source intensity. To determine the minimum intensity that a source must have for it to be detected, we first define a detection threshold and then compute the probabilities of detecting sources of various intensities at the given threshold. The intensity that corresponds to the specified Type II error probability defines that minimum intensity and is identified as the upper limit. Thus, an upper limit is a characteristic of the detection procedure rather than the strength of any particular source. It should not be confused with confidence intervals or other estimates of source intensity. This is particularly important given the large number of catalogs that are being generated from increasingly sensitive surveys. We discuss, with examples, the differences between these upper limits and confidence bounds. Both measures are useful quantities that should be reported in order to extract the most science from catalogs, though they answer different statistical questions: an upper bound describes an inference range on the source intensity, while an upper limit calibrates the detection process. We provide a recipe for computing upper limits that applies to all detection algorithms. C1 [Kashyap, Vinay L.; Siemiginowska, Aneta] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [van Dyk, David A.; Xu, Jin] Univ Calif Irvine, Dept Stat, Irvine, CA 92697 USA. [Connors, Alanna] Eureka Sci, Oakland, CA 94602 USA. [Freeman, Peter E.] Carnegie Mellon Univ, Dept Stat, Pittsburgh, PA 15213 USA. [Zezas, Andreas] Univ Crete, Dept Phys, GR-71003 Iraklion, Crete, Greece. RP Kashyap, VL (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM vkashyap@cfa.harvard.edu; dvd@ics.uci.edu; aconnors@eurekabayes.com; pfreeman@cmu.edu; asiemiginowska@cfa.harvard.edu; jinx@ics.uci.edu; azezas@cfa.harvard.edu RI Zezas, Andreas/C-7543-2011; OI Zezas, Andreas/0000-0001-8952-676X; Freeman, Peter/0000-0001-9627-0053; Van Dyk, David/0000-0002-0816-331X FU NASA-AISRP [NNG06G F17G]; CXC NASA [NAS8-39073]; NSF [DMS 04-06085, DMS 09-07522] FX This work was supported by NASA-AISRP grant NNG06G F17G (A. C.), CXC NASA contract NAS8-39073 (V. L. K., A. S.), NSF grants DMS 04-06085, and DMS 09-07522 (D. A. v. D.). We acknowledge useful discussions with Rick Harnden, Frank Primini, Jeff Scargle, Tom Loredo, Tom Aldcroft, Paul Green, Jeremy Drake, and participants and organizers of the SAMSI/SaFeDe Program on Astrostatistcs. NR 37 TC 30 Z9 30 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2010 VL 719 IS 1 BP 900 EP 914 DI 10.1088/0004-637X/719/1/900 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 635KD UT WOS:000280653100080 ER PT J AU Acciari, VA Aliu, E Arlen, T Aune, T Bautista, M Beilicke, M Benbow, W Boltuch, D Bradbury, SM Buckley, JH Bugaev, V Butt, Y Byrum, K Cesarini, A Ciupik, L Cui, W Dickherber, R Duke, C Finley, JP Finnegan, G Fortson, L Furniss, A Galante, N Gall, D Gillanders, GH Godambe, S Gotthelf, EV Grube, J Guenette, R Gyuk, G Hanna, D Holder, J Hui, CM Humensky, TB Imran, A Kaaret, P Karlsson, N Kertzman, M Kieda, D Konopelko, A Krawczynski, H Krennrich, F Lang, MJ LeBohec, S Maier, G McArthur, S McCann, A McCutcheon, M Moriarty, P Muhkerjee, R Ong, RA Otte, AN Pandel, D Perkins, JS Pohl, M Quinn, J Ragan, K Reyes, LC Reynolds, PT Roache, E Rose, HJ Schroedter, M Sembroski, GH Senturk, GD Slane, P Smith, AW Steele, D Swordy, SP Tesic, G Theiling, M Thibadeau, S Vassiliev, VV Vincent, S Wakely, SP Ward, JE Weekes, TC Weinstein, A Weisgarber, T Williams, DA Wissel, S Wood, M Zitzer, B AF Acciari, V. A. Aliu, E. Arlen, T. Aune, T. Bautista, M. Beilicke, M. Benbow, W. Boltuch, D. Bradbury, S. M. Buckley, J. H. Bugaev, V. Butt, Y. Byrum, K. Cesarini, A. Ciupik, L. Cui, W. Dickherber, R. Duke, C. Finley, J. P. Finnegan, G. Fortson, L. Furniss, A. Galante, N. Gall, D. Gillanders, G. H. Godambe, S. Gotthelf, E. V. Grube, J. Guenette, R. Gyuk, G. Hanna, D. Holder, J. Hui, C. M. Humensky, T. B. Imran, A. Kaaret, P. Karlsson, N. Kertzman, M. Kieda, D. Konopelko, A. Krawczynski, H. Krennrich, F. Lang, M. J. LeBohec, S. Maier, G. McArthur, S. McCann, A. McCutcheon, M. Moriarty, P. Muhkerjee, R. Ong, R. A. Otte, A. N. Pandel, D. Perkins, J. S. Pohl, M. Quinn, J. Ragan, K. Reyes, L. C. Reynolds, P. T. Roache, E. Rose, H. J. Schroedter, M. Sembroski, G. H. Senturk, G. Demet Slane, P. Smith, A. W. Steele, D. Swordy, S. P. Tesic, G. Theiling, M. Thibadeau, S. Vassiliev, V. V. Vincent, S. Wakely, S. P. Ward, J. E. Weekes, T. C. Weinstein, A. Weisgarber, T. Williams, D. A. Wissel, S. Wood, M. Zitzer, B. TI DISCOVERY OF VERY HIGH ENERGY gamma-RAY EMISSION FROM THE SNR G54.1+0.3 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE gamma rays: general; ISM: supernova remnants; pulsars: individual (J1930+1852, J1928+1746) ID PULSAR WIND NEBULAE; SUPERNOVA REMNANT G54.1+0.3; CRAB-NEBULA; VERITAS; TELESCOPE; ASTRONOMY; G0.9+0.1; CATALOG; SEARCH AB We report the discovery of very high energy (VHE) gamma-ray emission from the direction of the SNR G54.1+ 0.3 using the VERITAS ground-based gamma-ray observatory. The TeV signal has an overall significance of 6.8s and appears pointlike given the resolution of the instrument. The integral flux above 1 TeV is 2.5% of the Crab Nebula flux and significant emission is measured between 250 GeV and 4 TeV, well described by a power-law energy spectrum dN/dE similar to E(-Gamma) with a photon index Gamma = 2.39 +/- 0.23(stat) +/- 0.30sys. We find no evidence of time variability among observations spanning almost two years. Based on the location, the morphology, the measured spectrum, the lack of variability, and a comparison with similar systems previously detected in the TeV band, the most likely counterpart of this new VHE gamma-ray source is the pulsar wind nebula (PWN) in the SNR G54.1+0.3. The measured X-ray to VHE gamma-ray luminosity ratio is the lowest among all the nebulae supposedly driven by young rotation-powered pulsars, which could indicate a particle-dominated PWN. C1 [Acciari, V. A.; Benbow, W.; Galante, N.; Perkins, J. S.; Roache, E.; Theiling, M.; Weekes, T. C.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Aliu, E.; Boltuch, D.; Holder, J.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Aliu, E.; Boltuch, D.; Holder, J.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Arlen, T.; Ong, R. A.; Vassiliev, V. V.; Weinstein, A.; Wood, M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Aune, T.; Furniss, A.; Otte, A. N.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Aune, T.; Furniss, A.; Otte, A. N.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Bautista, M.; Guenette, R.; Hanna, D.; Maier, G.; McCann, A.; McCutcheon, M.; Ragan, K.; Tesic, G.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Beilicke, M.; Buckley, J. H.; Bugaev, V.; Dickherber, R.; Krawczynski, H.; McArthur, S.; Thibadeau, S.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Bradbury, S. M.; Rose, H. J.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Butt, Y.; Slane, P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Byrum, K.; Smith, A. W.] Argonne Natl Lab, Argonne, IL 60439 USA. [Cesarini, A.; Gillanders, G. H.; Lang, M. J.] Natl Univ Ireland Galway, Sch Phys, Galway, Ireland. [Ciupik, L.; Fortson, L.; Grube, J.; Gyuk, G.; Karlsson, N.; Steele, D.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA. [Cui, W.; Finley, J. P.; Gall, D.; Sembroski, G. H.; Zitzer, B.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Duke, C.] Grinnell Coll, Dept Phys, Grinnell, IA 50112 USA. [Finnegan, G.; Godambe, S.; Hui, C. M.; Kieda, D.; LeBohec, S.; Vincent, S.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Gotthelf, E. V.; Senturk, G. Demet] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Grube, J.; Quinn, J.; Ward, J. E.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Humensky, T. B.; Swordy, S. P.; Wakely, S. P.; Weisgarber, T.; Wissel, S.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Imran, A.; Krennrich, F.; Pohl, M.; Schroedter, M.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Kaaret, P.; Pandel, D.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. [Konopelko, A.] Pittsburg State Univ, Dept Phys, Pittsburg, KS 66762 USA. [Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland. [Muhkerjee, R.] Columbia Univ, Dept Phys & Astron, Barnard Coll, New York, NY 10027 USA. [Reyes, L. C.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland. RP Acciari, VA (reprint author), Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. EM ealiu@astro.columbia.edu; wakely@uchicago.edu OI Cui, Wei/0000-0002-6324-5772; Cesarini, Andrea/0000-0002-8611-8610; Ward, John E/0000-0003-1973-0794 FU U.S. Department of Energy; U.S. National Science Foundation; Smithsonian Institution; NSERC in Canada; Science Foundation Ireland; STFC in the UK FX This research is supported by grants from the U.S. Department of Energy, the U.S. National Science Foundation, and the Smithsonian Institution, by NSERC in Canada, by Science Foundation Ireland, and by STFC in the UK. NR 37 TC 14 Z9 15 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD AUG 10 PY 2010 VL 719 IS 1 BP L69 EP L73 DI 10.1088/2041-8205/719/1/L69 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 637YB UT WOS:000280853500016 ER PT J AU Aravena, M Younger, JD Fazio, GG Gurwell, M Espada, D Bertoldi, F Capak, P Wilner, D AF Aravena, M. Younger, J. D. Fazio, G. G. Gurwell, M. Espada, D. Bertoldi, F. Capak, P. Wilner, D. TI IDENTIFICATION OF TWO BRIGHT z > 3 SUBMILLIMETER GALAXY CANDIDATES IN THE COSMOS FIELD SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: evolution; galaxies: high-redshift; galaxies: starburst ID STAR-FORMING GALAXIES; HIGH-REDSHIFT; PHOTOMETRIC REDSHIFTS; IMAGING SURVEY; GOODS 850-5; RADIO; POPULATION; EMISSION; SOFTWARE; CATALOG AB We present high-resolution interferometric Submillimeter Array imaging at 890 mu m (similar to 2" resolution) of two millimeter selected galaxies-MMJ100015+ 021549 and MMJ100047+ 021021-discovered with the Max-Planck Millimeter Bolometer (MAMBO) on the IRAM 30 m telescope and also detected with Bolocam on the CSO, in the COSMOS field. The first source is significantly detected at the similar to 11 sigma level, while the second source is tentatively detected at the -4 sigma level, leading to a positional accuracy of similar to 0 ''.2-0.'' 3. MM100015+021549 is identified with a faint radio and K-band source. MMJ100047+021021 shows no radio emission and is tentatively identified with a very faint K-band peak which lies at similar to 1 ''.2 from a clumpy optical source. The submillimeterto- radio flux ratio for MM100015+021549 yields a redshift of similar to 4.8, consistent with the redshift implied by the UV-to-submillimeter photometry, z similar to 3.0-5.0. We find evidence for warm dust in this source with an infrared luminosity in the range similar to(0.9-2.5) x 10(13) L circle dot , supporting the increasing evidence for a population of luminous submillimeter galaxies at z > 3. Finally, the lack of photometric data for MMJ100047+021021 does not allow us to investigate its properties in detail; however, its submillimeter-to-radio flux ratio implies z > 3.5. C1 [Aravena, M.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Younger, J. D.] Inst Adv Study, Princeton, NJ 08544 USA. [Fazio, G. G.; Gurwell, M.; Espada, D.; Wilner, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Espada, D.] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. [Bertoldi, F.] Argelander Inst Astron, D-53121 Bonn, Germany. [Capak, P.] CALTECH, Pasadena, CA 91125 USA. RP Aravena, M (reprint author), Natl Radio Astron Observ, 520 Edgemont Rd, Charlottesville, VA 22903 USA. EM maravena@nrao.edu RI Aravena, Manuel/O-2361-2014 FU NASA [HF-51266.01, NAS 5-26555]; Space Telescope Science Institute; Marie Curie International Fellowship [MOIF-CT-2006-40298] FX J.D.Y. acknowledges support from NASA through Hubble Fellowship grant HF-51266.01 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. D. E. was supported by a Marie Curie International Fellowship within the 6th European Community Framework Programme (MOIF-CT-2006-40298). NR 41 TC 17 Z9 17 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD AUG 10 PY 2010 VL 719 IS 1 BP L15 EP L19 DI 10.1088/2041-8205/719/1/L15 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 637YB UT WOS:000280853500004 ER PT J AU Brown, WR Anderson, J Gnedin, OY Bond, HE Geller, MJ Kenyon, SJ Livio, M AF Brown, Warren R. Anderson, Jay Gnedin, Oleg Y. Bond, Howard E. Geller, Margaret J. Kenyon, Scott J. Livio, Mario TI A GALACTIC ORIGIN FOR HE 0437-5439, THE HYPERVELOCITY STAR NEAR THE LARGE MAGELLANIC CLOUD SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE Galaxy: center; Galaxy: kinematics and dynamics; Galaxy: stellar content; Magellanic Clouds; stars: individual (HE 0437-5439) ID SUPERMASSIVE BLACK-HOLE; MAIN-SEQUENCE; HORIZONTAL-BRANCH; BLUE STRAGGLERS; STELLAR ORBITS; HOT STARS; HALO; HE-0437-5439; CLUSTERS; RUNAWAY AB We use Hubble Space Telescope imaging to measure the absolute proper motion of the hypervelocity star (HVS) HE 0437-5439, a short-lived B star located in the direction of the Large Magellanic Cloud (LMC). We observe (mu(alpha), mu(delta)) = (+0.53 +/- 0.25(stat) +/- 0.33(sys), + 0.09 +/- 0.21(stat) +/- 0.48(sys)) mas yr(-1). The velocity vector points directly away from the center of the Milky Way; an origin from the center of the LMC is ruled out at the 3 sigma level. The flight time of the HVS from the Milky Way exceeds its main-sequence lifetime, thus its stellar nature requires it to be a blue straggler. The large space velocity rules out a Galactic-disk ejection. Combining the HVS's observed trajectory, stellar nature, and required initial velocity, we conclude that HE 0437-5439 was most likely a compact binary ejected by the Milky Way's central black hole. C1 [Brown, Warren R.; Geller, Margaret J.; Kenyon, Scott J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Anderson, Jay; Bond, Howard E.; Livio, Mario] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Gnedin, Oleg Y.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. RP Brown, WR (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM wbrown@cfa.harvard.edu; jayander@stsci.edu; ognedin@umich.edu; bond@stsci.edu; mgeller@cfa.harvard.edu; skenyon@cfa.harvard.edu; mlivio@stsci.edu OI Kenyon, Scott/0000-0003-0214-609X; Gnedin, Oleg/0000-0001-9852-9954 FU NASA through Space Telescope Science Institute [GO-10824, GO-11782, NAS5-26555] FX We thank Andy Gould, Hagai Perets, and the anonymous referee for helpful comments. Support for this research was provided by NASA through grants GO-10824 and GO-11782 from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. This research makes use of NASA's Astrophysics Data System Bibliographic Services. NR 49 TC 25 Z9 26 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD AUG 10 PY 2010 VL 719 IS 1 BP L23 EP L27 DI 10.1088/2041-8205/719/1/L23 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 637YB UT WOS:000280853500006 ER PT J AU Keshet, U Markevitch, M Birnboim, Y Loeb, A AF Keshet, Uri Markevitch, Maxim Birnboim, Yuval Loeb, Abraham TI DYNAMICS AND MAGNETIZATION IN GALAXY CLUSTER CORES TRACED BY X-RAY COLD FRONTS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: clusters: general; galaxies: clusters: intracluster medium; hydrodynamics; intergalactic medium; magnetic fields; X-rays: galaxies: clusters ID PERSEUS CLUSTER; CHANDRA OBSERVATION; COOLING FLOWS; XMM-NEWTON; BUBBLES; GAS; TEMPERATURE; SHOCKS; A3667; M87 AB Cold fronts (CFs)-density and temperature plasma discontinuities-are ubiquitous in cool cores of galaxy clusters, where they appear as X-ray brightness edges in the intracluster medium, nearly concentric with the cluster center. We analyze the thermodynamic profiles deprojected across core CFs found in the literature. While the pressure appears continuous across these CFs, we find that all of them require significant centripetal acceleration beneath the front. This is naturally explained by a tangential, nearly sonic bulk flow just below the CF, and a tangential shear flow involving a fair fraction of the plasma beneath the front. Such shear should generate near-equipartition magnetic fields on scales less than or similar to 50 pc from the front and could magnetize the entire core. Such fields would explain the apparent stability of cool core CFs and the recently reported CF-radio minihalo association. C1 [Keshet, Uri; Markevitch, Maxim; Birnboim, Yuval; Loeb, Abraham] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Keshet, U (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Birnboim, Yuval/0000-0002-6547-8545 FU NASA through Einstein Post-doctoral Fellowship [PF8-90059]; NASA [NAS8-39073]; Harvard College Observatory; NSF [AST-0907890] FX We thank W. Forman and O. Cohen for useful discussions. U. K. acknowledges support from NASA through Einstein Post-doctoral Fellowship grant number PF8-90059. This work was supported in part by NASA contract NAS8-39073 (M.M.), by an ITC fellowship from the Harvard College Observatory (Y.B.), and by NSF grant AST-0907890 (A.L.). NR 26 TC 26 Z9 26 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD AUG 10 PY 2010 VL 719 IS 1 BP L74 EP L78 DI 10.1088/2041-8205/719/1/L74 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 637YB UT WOS:000280853500017 ER PT J AU Liu, JF McClintock, JE Narayan, R Davis, SW Orosz, JA AF Liu, Jifeng McClintock, Jeffrey E. Narayan, Ramesh Davis, Shane W. Orosz, Jerome A. TI PRECISE MEASUREMENT OF THE SPIN PARAMETER OF THE STELLAR-MASS BLACK HOLE M33 X-7 (vol 679, L37, 2008) SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Correction C1 [Liu, Jifeng; McClintock, Jeffrey E.; Narayan, Ramesh] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Davis, Shane W.] Inst Adv Study, Princeton, NJ 08540 USA. [Orosz, Jerome A.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. RP Liu, JF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 3 TC 19 Z9 19 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD AUG 10 PY 2010 VL 719 IS 1 BP L109 EP L109 DI 10.1088/2041-8205/719/1/L109 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 637YB UT WOS:000280853500024 ER PT J AU Tscherbul, TV Pavlovic, Z Sadeghpour, HR Cote, R Dalgarno, A AF Tscherbul, T. V. Pavlovic, Z. Sadeghpour, H. R. Cote, R. Dalgarno, A. TI Collisions of trapped molecules with slow beams SO PHYSICAL REVIEW A LA English DT Article AB We present a theoretical study of molecular-trap loss induced by collisions with slow atomic beams based on an explicit analysis of collision kinematics in the laboratory frame and a rigorous quantum description of atom-molecule scattering in external fields. The theory is applied to elucidate the effects of nonuniform magnetic and optical trapping fields on low-temperature collisions of OH (J = 3/2, M-J = 3/2, f) molecules with He-4 atoms. Our calculations quantify the extent to which both elastic and inelastic cross sections are suppressed by external trapping fields, clarify the role of small-angle scattering in trap loss, and may benefit future experiments on collisional cooling of molecules in electromagnetic traps. The calculated cross sections for trap loss in He-4 + OH collisions are consistent with recent experimental observations at low beam energies [B. C. Sawyer et al., Phys. Rev. Lett. 101, 203203 (2008)], demonstrating the importance of including the effects of nonuniform trapping fields in theoretical simulations of cold collision experiments with trapped molecules and slow atomic beams. C1 [Tscherbul, T. V.; Dalgarno, A.] Harvard MIT Ctr Ultracold Atoms, Cambridge, MA 02138 USA. [Tscherbul, T. V.; Pavlovic, Z.; Sadeghpour, H. R.; Dalgarno, A.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys, Cambridge, MA 02138 USA. [Pavlovic, Z.; Cote, R.] Univ Connecticut, Dept Phys, Storrs, CT 06269 USA. RP Tscherbul, TV (reprint author), Harvard MIT Ctr Ultracold Atoms, Cambridge, MA 02138 USA. EM tshcherb@cfa.harvard.edu RI Tscherbul, Timur/K-3286-2014 OI Tscherbul, Timur/0000-0001-5689-040X FU Chemical Science, Geoscience, and Bioscience Division of the Office of Basic Energy Science, Office of Science, US Department of Energy; NSF FX We thank Colin Connolly, Vasili Kharchenko, Bas van de Meerakker, and Kirk Madison for valuable discussions and helpful comments on the manuscript. This work was supported by the Chemical Science, Geoscience, and Bioscience Division of the Office of Basic Energy Science, Office of Science, US Department of Energy, and NSF grants to the Harvard-MIT Center for Ultracold Atoms and the Institute for Theoretical Atomic, Molecular, and Optical Physics at Harvard University and Smithsonian Astrophysical Observatory. NR 37 TC 13 Z9 13 U1 1 U2 9 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD AUG 10 PY 2010 VL 82 IS 2 AR 022704 DI 10.1103/PhysRevA.82.022704 PG 10 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA V25JB UT WOS:000208473200001 ER PT J AU Green, WA AF Green, W. A. TI The function of the aerenchyma in arborescent lycopsids: evidence of an unfamiliar metabolic strategy SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Review DE aerenchyma; aquatic CAM; arborescent lycopsids; metabolic pathways; parichnos ID CRASSULACEAN ACID METABOLISM; UNIFLORA L ASCHERS; AQUATIC CAM PLANT; DEVELOPMENTAL MORPHOLOGY; PHANEROZOIC TIME; PHOTOSYNTHETIC APPARATUS; PHRAGMITES-AUSTRALIS; TEMPERATURE REGIMES; PORTULACA-OLERACEA; C-4 PHOTOSYNTHESIS AB Most species of the modern family Isoetaceae (Quillworts) some other modern hydrophytes, use a metabolic pathway for carbon fixation that involves uptake of sedimentary carbon and enrichment of CO(2) in internal gas spaces as a carbon-concentrating mechanism. This metabolism, which is related to 'aquatic CAM', is characterized by morphological, physiological and biochemical adaptations for decreasing photorespirative loss, aerating roots and maintaining high growth rates in anoxic, oligotrophic, stressed environments. Some of the closest relatives of the Isoetaceae were the 'arborescent lycopsids', which were among the dominant taxa in the coal swamps found in lowland ecosystems during the Carboniferous and Permian periods (approx. 300 Ma). Morphological, ecological and geochemical evidence supports the hypothesis that the arborescent lycopsids had an unusual metabolism similar to that of modern Isoetaceae and processed a biogeochemically significant proportion of organically fixed carbon over a period of about 100 million years in the late Palaeozoic. The temporal coincidence between the dominance of plants with this metabolism and an anomalous global atmosphere ( high O(2); low CO(2)) supports the idea that biosphere feedbacks are important in regulating global climatic homeostasis. The potential influence of this metabolism on the global carbon cycle and its specific adaptive function suggest that it should perhaps be considered a fourth major photosynthetic pathway. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. RP Green, WA (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. EM wagreen@bricol.net NR 96 TC 17 Z9 17 U1 3 U2 19 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 J9 P ROY SOC B-BIOL SCI JI Proc. R. Soc. B-Biol. Sci. PD AUG 7 PY 2010 VL 277 IS 1692 BP 2257 EP 2267 DI 10.1098/rspb.2010.0224 PG 11 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 616WX UT WOS:000279243300001 PM 20356894 ER PT J AU Robinson, H Bunwong, S Chantaranothai, P AF Robinson, Harold Bunwong, Sukhonthip Chantaranothai, Pranom TI A new genus, Kurziella from Thailand (Vernonieae: Asteraceae) SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article ID GYMNANTHEMINAE VERNONIEAE; INDIA; RESTORATION; CHINA; ASIA AB A new genus, Kurziella, is named to accommodate the Southeast Asian species Vernonia gymnoclada Coll. & Hemsl., a species often determined in herbaria as Vernonia juncea Kurz in Hook.f., nom. nud. C1 [Robinson, Harold] Natl Museum Nat Hist, Dept Bot, Smithsonian Inst, Washington, DC 20013 USA. [Bunwong, Sukhonthip; Chantaranothai, Pranom] Khon Kaen Univ, Fac Sci, Dept Biol, Appl Taxon Res Ctr, Khon Kaen 40002, Thailand. RP Robinson, H (reprint author), Natl Museum Nat Hist, Dept Bot, Smithsonian Inst, MRC 166,POB 37012, Washington, DC 20013 USA. EM robinsoh@si.edu; sukhonthipb37@gmail.com; pranom@kku.ac.th FU TRF/BIOTEC Special Program for Biodiversity Research and Training [BRT_T151007]; Ministry of Education; Institute for the Promotion of Teaching Science and Technology (IPST), Thailand FX The Royal Botanic Garden at Kew is thanked for access to the type specimen of Vernonia gymnoclada. The TRF/BIOTEC Special Program for Biodiversity Research and Training Grant BRT_T151007 and Ministry of Education and the Institute for the Promotion of Teaching Science and Technology (IPST), Thailand support this work. We would like to thank the curators of the herbaria cited above for the use of their facilities. NR 12 TC 1 Z9 1 U1 0 U2 1 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD AUG 6 PY 2010 VL 123 IS 2 BP 174 EP 178 PG 5 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 636YP UT WOS:000280781700008 ER PT J AU Prockter, LM Ernst, CM Denevi, BW Chapman, CR Head, JW Fassett, CI Merline, WJ Solomon, SC Watters, TR Strom, RG Cremonese, G Marchi, S Massironi, M AF Prockter, Louise M. Ernst, Carolyn M. Denevi, Brett W. Chapman, Clark R. Head, James W., III Fassett, Caleb I. Merline, William J. Solomon, Sean C. Watters, Thomas R. Strom, Robert G. Cremonese, Gabriele Marchi, Simone Massironi, Matteo TI Evidence for Young Volcanism on Mercury from the Third MESSENGER Flyby SO SCIENCE LA English DT Article ID CRATERING RECORD; SMOOTH PLAINS; IMPACT BASINS; CALORIS BASIN; EVOLUTION; MISSION; GEOLOGY; VIEW AB During its first two flybys of Mercury, the MESSENGER spacecraft acquired images confirming that pervasive volcanism occurred early in the planet's history. MESSENGER's third Mercury flyby revealed a 290-kilometer-diameter peak-ring impact basin, among the youngest basins yet seen, having an inner floor filled with spectrally distinct smooth plains. These plains are sparsely cratered, postdate the formation of the basin, apparently formed from material that once flowed across the surface, and are therefore interpreted to be volcanic in origin. An irregular depression surrounded by a halo of bright deposits northeast of the basin marks a candidate explosive volcanic vent larger than any previously identified on Mercury. Volcanism on the planet thus spanned a considerable duration, perhaps extending well into the second half of solar system history. C1 [Prockter, Louise M.; Ernst, Carolyn M.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Denevi, Brett W.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85251 USA. [Chapman, Clark R.; Merline, William J.] SW Res Inst, Boulder, CO 80302 USA. [Head, James W., III; Fassett, Caleb I.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. [Solomon, Sean C.] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA. [Watters, Thomas R.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. [Strom, Robert G.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Cremonese, Gabriele] Astron Observ Padova, Inst Nazl Astrofis, I-35122 Padua, Italy. [Marchi, Simone] Univ Padua, Dept Astron, I-35137 Padua, Italy. [Massironi, Matteo] Univ Padua, Dept Geosci, I-35137 Padua, Italy. RP Prockter, LM (reprint author), Johns Hopkins Univ, Appl Phys Lab, Johns Hopkins Rd, Laurel, MD 20723 USA. EM Louise.Prockter@jhuapl.edu RI Massironi, Matteo/F-8860-2012; Ernst, Carolyn/I-4902-2012; Denevi, Brett/I-6502-2012; OI Denevi, Brett/0000-0001-7837-6663; Cremonese, Gabriele/0000-0001-9021-1140; Fassett, Caleb/0000-0001-9155-3804; Massironi, Matteo/0000-0002-7757-8818 FU NASA [NASW-00002, NAS5-97271] FX We are grateful to N. Chabot, N. Laslo, and H. Kang, who designed the imaging sequences that made this contribution possible, and to the tireless efforts of the engineers and technical support personnel on the MESSENGER team. The MESSENGER project is supported by the NASA Discovery Program under contracts NASW-00002 to the Carnegie Institution of Washington and NAS5-97271 to the Johns Hopkins University Applied Physics Laboratory. NR 25 TC 48 Z9 48 U1 2 U2 13 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD AUG 6 PY 2010 VL 329 IS 5992 BP 668 EP 671 DI 10.1126/science.1188186 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 634RV UT WOS:000280602700035 PM 20647421 ER PT J AU McFadden, RR Siddoway, CS Teyssier, C Fanning, CM AF McFadden, R. R. Siddoway, C. S. Teyssier, C. Fanning, C. M. TI Cretaceous oblique extensional deformation and magma accumulation in the Fosdick Mountains migmatite-cored gneiss dome, West Antarctica SO TECTONICS LA English DT Article ID MARIE-BYRD-LAND; U-PB GEOCHRONOLOGY; HIGH-GRADE METAMORPHISM; KARAKORAM SHEAR ZONE; ROSS SEA RIFT; NEW-ZEALAND; ZIRCON GEOCHRONOLOGY; MELT SEGREGATION; PACIFIC MARGIN; GRANITE MAGMA AB The Fosdick Mountains, West Antarctica, expose a 15 x 80 km migmatite-cored gneiss dome consisting of migmatitic gneisses, diatexite migmatite, and sub-horizontal leucogranite sheets. The Fosdick dome was emplaced and exhumed in the mid-Cretaceous due to oblique extension associated with the West Antarctic Rift system along the West Antarctic-New Zealand segment of East Gondwana. The dome is bounded to the south by a dextral oblique detachment structure and to the north by an inferred dextral strike-slip fault. Within the Fosdick dome and in the detachment zone, granite occupies leucosomes, dikes, sills, and dilatant and shear structures. The pattern of kilometer-scale domains of migmatite and granite suggest that lithologic variations and heterogeneous deformation (boudinage) resulted in pressure gradients that enhanced melt flow and magma accumulation in the Fosdick dome. Steep foliations are overprinted, folded, and transposed by subhorizontal fabrics. The crosscutting relationship is interpreted as a transition from wrench deformation to oblique divergence. Steep structures in the dome host concordant, subvertical leucosome and granite sheets yielding SHRIMP U-Pb zircon ages between ca. 117 and 114 Ma. Prevalent subhorizontal domains host large volumes of subhorizontal diatexite migmatite and granite sheets that yield U-Pb zircon ages between ca. 109 and 102 Ma. These ages indicate a timescale for melt influx of approximately 15 Ma and that the transition from wrench to oblique divergence may have occurred in as little as 5 Ma. Granites with crystallization ages between ca. 109 and 102 Ma were also emplaced in the South Fosdick Detachment zone, indicating that the detachment was active during oblique divergence. SHRIMP U-Pb titanite ages between ca. 102 and 97 Ma for late-to post-tectonic diorite dikes are interpreted as emplacement ages and give a minimum age for gneissic foliation development during detachment faulting. The Fosdick Mountains preserve a record of the middle to lower crustal response to a transition from wrench to oblique extensional deformation. Overprinting structural relationships show that a change in the angle of oblique extension can induce accumulation of sub-horizontal magma sheets and lead to initiation of a detachment zone. Citation: McFadden, R. R., C. S. Siddoway, C. Teyssier, and C. M. Fanning (2010), Cretaceous oblique extensional deformation and magma accumulation in the Fosdick Mountains migmatite-cored gneiss dome, West Antarctica, Tectonics, 29, TC4022, doi:10.1029/2009TC002492. C1 [Fanning, C. M.] Australian Natl Univ, Res Sch Earth Sci, Canberra, ACT 0200, Australia. [Siddoway, C. S.] Colorado Coll, Dept Geol, Colorado Springs, CO 80903 USA. [McFadden, R. R.; Teyssier, C.] Univ Minnesota, Dept Geol & Geophys, Minneapolis, MN 55455 USA. RP McFadden, RR (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama. RI Fanning, C. Mark/I-6449-2016; OI Fanning, C. Mark/0000-0003-3331-3145; Siddoway, Christine Smith/0000-0003-0478-6138 FU National Science Foundation Office of Polar [NSF-OPP 0338279, NSF-OPP 0337488] FX This manuscript has been improved by extensive and insightful reviews of an earlier version by R. Weinberg, A. Tulloch, and Associate Editor R. Miller. We thank D. L. Whitney for significant contributions to ideas presented in this work and comments on earlier drafts of this paper. Companion studies by Fawna Korhonen, Tetsu Saito, and Mike Brown aided the formulation of hypotheses presented here. We thank Seth Kruckenberg and Jenny Haywood for fieldwork collaboration; Sylvie Fadrhonc, Chuck Magee, Sam Mertens, and Brenda Armstrong for contributions to the SHRIMP research; and Mike Roberts, Allen O'Bannon, and Forrest McCarthy for field coordination and safety. For logistical support, we thank employees of Raytheon Polar Services (Berg Field Center and USAP Cargo, in particular), ANG 109th, and Kenn Borek Air crews. Research was funded by the National Science Foundation Office of Polar Programs grants NSF-OPP 0338279 to C. S. Siddoway and NSF-OPP 0337488 to C. Teyssier, but the authors are fully responsible for the scientific content. NR 96 TC 21 Z9 21 U1 0 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0278-7407 J9 TECTONICS JI Tectonics PD AUG 6 PY 2010 VL 29 AR TC4022 DI 10.1029/2009TC002492 PG 27 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 636HO UT WOS:000280722600001 ER PT J AU Mangan, SA Schnitzer, SA Herre, EA Mack, KML Valencia, MC Sanchez, EI Bever, JD AF Mangan, Scott A. Schnitzer, Stefan A. Herre, Edward A. Mack, Keenan M. L. Valencia, Mariana C. Sanchez, Evelyn I. Bever, James D. TI Negative plant-soil feedback predicts tree-species relative abundance in a tropical forest SO NATURE LA English DT Article ID LOCAL NEIGHBORHOOD; DENSITY-DEPENDENCE; SEEDLING MORTALITY; MAINTAIN DIVERSITY; SPATIAL-PATTERNS; COMMUNITY; PATHOGENS; GROWTH; RECRUITMENT; COEXISTENCE AB The accumulation of species-specific enemies around adults is hypothesized to maintain plant diversity by limiting the recruitment of conspecific seedlings relative to heterospecific seedlings(1-6). Although previous studies in forested ecosystems have documented patterns consistent with the process of negative feedback(7-16), these studies are unable to address which classes of enemies (for example, pathogens, invertebrates, mammals) exhibit species-specific effects strong enough to generate negative feedback(17), and whether negative feedback at the level of the individual tree is sufficient to influence community-wide forest composition. Here we use fully reciprocal shade-house and field experiments to test whether the performance of conspecific tree seedlings (relative to heterospecific seedlings) is reduced when grown in the presence of enemies associated with adult trees. Both experiments provide strong evidence for negative plant-soil feedback mediated by soil biota. In contrast, above-ground enemies (mammals, foliar herbivores and foliar pathogens) contributed little to negative feedback observed in the field. In both experiments, we found that tree species that showed stronger negative feedback were less common as adults in the forest community, indicating that susceptibility to soil biota may determine species relative abundance in these tropical forests. Finally, our simulation models confirm that the strength of local negative feedback that we measured is sufficient to produce the observed community-wide patterns in tree-species relative abundance. Our findings indicate that plant-soil feedback is an important mechanism that can maintain species diversity and explain patterns of tree-species relative abundance in tropical forests. C1 [Mangan, Scott A.; Schnitzer, Stefan A.] Univ Wisconsin, Dept Biol Sci, Milwaukee, WI 53201 USA. [Mangan, Scott A.; Schnitzer, Stefan A.; Herre, Edward A.; Sanchez, Evelyn I.] Smithsonian Trop Res Inst, MRC 0580 06, Dpo, AA 34002 USA. [Mack, Keenan M. L.; Bever, James D.] Indiana Univ, Dept Biol, Bloomington, IN 47405 USA. [Valencia, Mariana C.] Univ Illinois, Dept Biol Sci, Chicago, IL 60607 USA. RP Mangan, SA (reprint author), Univ Wisconsin, Dept Biol Sci, POB 413, Milwaukee, WI 53201 USA. EM smangan37@gmail.com OI Schnitzer, Stefan/0000-0002-2715-9455 FU Smithsonian Tropical Research Institute (STRI); University of Wisconsin-Milwaukee (UWM) Research Growth Initiative; UWM Research Foundation; National Science Foundation; STRI Soil Initiative FX We thank G. Adler, M. Kaspari, E. Leigh, T. Lambert, I. Rubinoff, E. Tanner, M. Tobin, B. Turner, S. Van Bael and N. Wurzburger for providing discussions and comments on the manuscript. R. Kolodziej, K. Meyer, K. McElligott and T. Shirshac provided greenhouse and field assistance. Logistical support was provided by the Smithsonian Tropical Research Institute. The Center of Tropical Forest Science provided BCI tree abundance data published online at https://ctfs.arnarb.harvard.edu/webatlas/datasets/bci/abundance. This study was supported by a Smithsonian Tropical Research Institute (STRI) postdoctoral fellowship to S. A. M., a University of Wisconsin-Milwaukee (UWM) Research Growth Initiative grant to S. A. S., a fellowship from the UWM Research Foundation, and a grant from the National Science Foundation to J.D.B. We thank I. Rubinoff for his support of the STRI Soil Initiative. NR 30 TC 284 Z9 290 U1 37 U2 326 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD AUG 5 PY 2010 VL 466 IS 7307 BP 752 EP U10 DI 10.1038/nature09273 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 634EN UT WOS:000280562500038 PM 20581819 ER PT J AU Guglielmino, M Penna, V Capogrosso-Sansone, B AF Guglielmino, M. Penna, V. Capogrosso-Sansone, B. TI Mott-insulator-to-superfluid transition in Bose-Bose mixtures in a two-dimensional lattice SO PHYSICAL REVIEW A LA English DT Article ID QUANTUM MONTE-CARLO; OPTICAL LATTICES; POLARON; PHYSICS; GASES; ATOMS AB We perform a numeric study (worm algorithm Monte Carlo simulations) of ultracold two-component bosons in two-dimensional optical lattices. We study how the Mott-insulator-to-superfluid transition is affected by the presence of a second superfluid bosonic species. We find that, at fixed interspecies interaction, the upper and lower boundaries of the Mott lobe are differently modified. The lower boundary is strongly renormalized even for relatively low filling factor of the second component and moderate (interspecies) interaction. The upper boundary, instead, is affected only for large enough filling of the second component. Whereas boundaries are renormalized we find evidence of polaron-like excitations. Our results are of interest for current experimental setups. C1 [Guglielmino, M.; Penna, V.] Politecn Torino, Dipartimento Fis, I-10129 Turin, Italy. [Penna, V.] Politecn Torino, CNISM Unita Ric, I-10129 Turin, Italy. [Capogrosso-Sansone, B.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys, Cambridge, MA 02138 USA. RP Guglielmino, M (reprint author), Politecn Torino, Dipartimento Fis, Corso Duca Abruzzi 24, I-10129 Turin, Italy. FU Institute for Atomic, Molecular and Optical Physics (ITAMP) FX B. Capogrosso-Sansone thanks D. Schneble, D. Pertot, B. Gadway, N. Prokof'ev, and L. Pollet for interesting discussion. V. Penna thanks F. Minardi for useful comments on the realization of bosonic mixtures. The work of B. Capogrosso-Sansone was supported by the Institute for Atomic, Molecular and Optical Physics (ITAMP). NR 34 TC 18 Z9 18 U1 1 U2 7 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD AUG 4 PY 2010 VL 82 IS 2 AR 021601 DI 10.1103/PhysRevA.82.021601 PG 4 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 634IW UT WOS:000280575300001 ER PT J AU Vigneron, JP Simonis, P Aiello, A Bay, A Windsor, DM Colomer, JF Rassart, M AF Vigneron, Jean Pol Simonis, Priscilla Aiello, Annette Bay, Annick Windsor, Donald M. Colomer, Jean-Francois Rassart, Marie TI Reverse color sequence in the diffraction of white light by the wing of the male butterfly Pierella luna (Nymphalidae: Satyrinae) SO PHYSICAL REVIEW E LA English DT Article AB The butterfly Pierella luna (Nymphalidae) shows an intriguing rainbow iridescence effect: the forewings of the male, when illuminated along the axis from the body to the wing tip, decompose a white light beam as a diffraction grating would do. Violet light, however, emerges along a grazing angle, near the wing surface, while the other colors, from blue to red, exit respectively at angles progressively closer to the direction perpendicular to the wing plane. This sequence is the reverse of the usual decomposition of light by a grating with a periodicity parallel to the wing surface. It is shown that this effect is produced by a macroscopic deformation of the entire scale, which curls in such a way that it forms a "vertical" grating, perpendicular to the wing surface, and functions in transmission instead of reflection. C1 [Vigneron, Jean Pol; Simonis, Priscilla; Bay, Annick; Colomer, Jean-Francois; Rassart, Marie] Univ Namur FUNDP, Res Ctr Phys Matter & Radiat PMR, B-5000 Namur, Belgium. [Aiello, Annette; Windsor, Donald M.] Smithsonian Trop Res Inst, Balboa 084303092, Ancon Panama, Panama. RP Vigneron, JP (reprint author), Univ Namur FUNDP, Res Ctr Phys Matter & Radiat PMR, 61 Rue Bruxelles, B-5000 Namur, Belgium. EM jean-pol.vigneron@fundp.ac.be FU Belgian National Fund for Scientific Research (F.R.S.-FNRS) FX The authors thank Steve Collins for the permission to reproduce the picture in Fig. 1. Namur Interuniversity Scientific Computing Facility (Namur-ISCF) was used for computations. M. R. and J.-F.C. were supported by the Belgian National Fund for Scientific Research (F.R.S.-FNRS). J.P.V. and M. R. acknowledge the hospitality of the Smithsonian Tropical Research Institute (STRI), in the Republic of Panama, during the earliest stages of this work. NR 9 TC 9 Z9 10 U1 0 U2 7 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1539-3755 J9 PHYS REV E JI Phys. Rev. E PD AUG 4 PY 2010 VL 82 IS 2 AR 021903 DI 10.1103/PhysRevE.82.021903 PN 1 PG 8 WC Physics, Fluids & Plasmas; Physics, Mathematical SC Physics GA 634JM UT WOS:000280577100003 PM 20866833 ER PT J AU Jha, S Dick, CW AF Jha, Shalene Dick, Christopher W. TI Native bees mediate long-distance pollen dispersal in a shade coffee landscape mosaic SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE agriculture; pollination; tropical ecology; gene flow; fragmentation ID TROPICAL AGROFORESTRY SYSTEMS; CROP POLLINATION SERVICES; HABITAT FRAGMENTATION; RAIN-FOREST; REPRODUCTIVE SUSCEPTIBILITY; GENETIC CONSEQUENCES; PLANT-POPULATIONS; MATING SYSTEMS; LAND-USE; TREES AB Coffee farms are often embedded within a mosaic of agriculture and forest fragments in the world's most biologically diverse tropical regions. Although shade coffee farms can potentially support native pollinator communities, the degree to which these pollinators facilitate gene flow for native trees is unknown. We examined the role of native bees as vectors of gene flow for a reproductively specialized native tree, Miconia affinis, in a shade coffee and remnant forest landscape mosaic. We demonstrate extensive cross-habitat gene flow by native bees, with pollination events spanning more than 1,800 m. Pollen was carried twice as far within shade coffee habitat as in nearby forest, and trees growing within shade coffee farms received pollen from a far greater number of sires than trees within remnant forest. The study shows that shade coffee habitats support specialized native pollinators that enhance the fecundity and genetic diversity of remnant native trees. C1 [Jha, Shalene] Univ Calif Berkeley, Dept Environm Sci Policy & Management, Berkeley, CA 94720 USA. [Jha, Shalene; Dick, Christopher W.] Univ Michigan, Dept Ecol & Evolutionary Biol, Ann Arbor, MI 48109 USA. [Dick, Christopher W.] Univ Michigan Herbarium, Ann Arbor, MI 48108 USA. [Dick, Christopher W.] Smithsonian Trop Res Inst, Balboa Ancon, Panama. RP Jha, S (reprint author), Univ Calif Berkeley, Dept Environm Sci Policy & Management, Berkeley, CA 94720 USA. EM s.jha@berkeley.edu RI Dick, Christopher/A-8744-2008; Jha, Shalene/B-4271-2012 FU University of Michigan; National Science Foundation [DEB 0908661, DEB 043665] FX We thank J. Vandermeer, I. Perfecto, B. Rathcke, B. Ferguson, and S. Pereira for help in the development of this project; G. Dominguez-Martinez for his help in scouting trees; and the farmers of Nueva Alemania for permission to conduct this study on their land. All experiments were in compliance with current laws governing biodiversity protection in Mexico. This project was supported by the Helen Olson Brower Fellowship at the University of Michigan and National Science Foundation Awards DEB 0908661 and DEB 043665. NR 57 TC 31 Z9 31 U1 3 U2 44 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD AUG 3 PY 2010 VL 107 IS 31 BP 13760 EP 13764 DI 10.1073/pnas.1002490107 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 634SP UT WOS:000280605900039 PM 20660738 ER PT J AU Gowaty, PA Kim, YK Rawlings, J Anderson, WW AF Gowaty, Patricia Adair Kim, Yong-Kyu Rawlings, Jessica Anderson, W. W. TI Polyandry increases offspring viability and mother productivity but does not decrease mother survival in Drosophila pseudoobscura SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE fitness; mating system; monogamy; multiple mating ID SEXUAL SELECTION; MULTIPLE INSEMINATION; REPRODUCTIVE SUCCESS; NATURAL-POPULATIONS; MATE PREFERENCES; FEMALE FITNESS; EVOLUTION; MELANOGASTER; BENEFITS; PATTERNS AB Polyandrous mating is common, but the benefits for females of polyandry remain controversial. To test whether mating with multiple males affects female fitness, we compared lifetime components of fitness of three experimental sets of Drosophila pseudoobscura females: monogamous females allowed to copulate one time (M(OC)); monogamous females held with a male over her entire life and experiencing many copulations (M(MC)); and polyandrous females with a different male over each day of their lives and also experiencing many copulations (P(MC)). Consistent with previous studies in this species, females in treatments in which multiple copulations occurred, M(MC) and P(MC), had offspring with significantly higher egg-to-adult survival (i.e., offspring viability) and higher numbers of adult offspring (i.e., productivity) than M(OC) females, showing that multiple inseminations enhance offspring and mother fitness. In addition, although M(MC) females laid significantly more eggs than polyandrous (P(MC)) females, percent egg-to-adult survival and number of adult offspring were higher for P(MC) than M(MC) females, showing that polyandrous mating enhances the fitness of females more than multiply mating with only one male. Inconsistent with the cost of reproduction, lifespan was not significantly longer for M(OC) females than for M(MC) or P(MC) females. To our knowledge, this is the first study to examine simultaneously in outbred WT Drosophila pseudoobscura the lifetime costs and benefits to females of polyandry, monogamy with a single copulation, and monogamy with repeat copulations. 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, Los Angeles, CA 90095 USA. [Gowaty, Patricia Adair] Smithsonian Trop Res Inst, Balboa, Panama. [Kim, Yong-Kyu; Rawlings, Jessica; Anderson, W. W.] Univ Georgia, Dept Genet, Athens, GA 30602 USA. RP Gowaty, PA (reprint author), Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA. EM gowaty@eeb.ucla.edu; wyatt@uga.edu FU National Science Foundation FX We thank Margaret Anderson and Stephen P. Hubbell for statistical advice and discussion about these data; we thank Malin Ah-King, J. P. Drury, Brant Faircloth, David Hoskens, Therese Markow, and Judy Stamps for comments on a previous version. This work was partially supported by a National Science Foundation grant (to P. A. G. and W.W.A.). NR 33 TC 36 Z9 36 U1 0 U2 16 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD AUG 3 PY 2010 VL 107 IS 31 BP 13771 EP 13776 DI 10.1073/pnas.1006174107 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 634SP UT WOS:000280605900041 PM 20643932 ER PT J AU Crawford, AJ Lips, KR Bermingham, E AF Crawford, Andrew J. Lips, Karen R. Bermingham, Eldredge TI Epidemic disease decimates amphibian abundance, species diversity, and evolutionary history in the highlands of central Panama SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE amphibian decline; biodiversity; chytridiomycosis; DNA barcoding; phylogenetic diversity ID POPULATION DECLINES; BATRACHOCHYTRIUM-DENDROBATIDIS; CENTRAL-AMERICA; EXTINCTION; CHYTRIDIOMYCOSIS; FROG; PATTERNS; BIODIVERSITY; COMMUNITY; CLIMATE AB Amphibian populations around the world are experiencing unprecedented declines attributed to a chytrid fungal pathogen, Batrachochytrium dendrobatidis. Despite the severity of the crisis, quantitative analyses of the effects of the epidemic on amphibian abundance and diversity have been unavailable as a result of the lack of equivalent data collected before and following disease outbreak. We present a community-level assessment combining long-term field surveys and DNA barcode data describing changes in abundance and evolutionary diversity within the amphibian community of El Cope, Panama, following a disease epidemic and mass-mortality event. The epidemic reduced taxonomic, lineage, and phylogenetic diversity similarly. We discovered that 30 species were lost, including five undescribed species, representing 41% of total amphibian lineage diversity in El Cope. These extirpations represented 33% of the evolutionary history of amphibians within the community, and variation in the degree of population loss and decline among species was random with respect to the community phylogeny. Our approach provides a fast, economical, and informative analysis of loss in a community whether measured by species or phylogenetic diversity. C1 [Crawford, Andrew J.; Lips, Karen R.; Bermingham, Eldredge] Smithsonian Trop Res Inst, Panama City, Panama. [Crawford, Andrew J.] Univ Los Andes, Dept Biol Sci, Bogota 4976, Colombia. [Crawford, Andrew J.] Circulo Herpetol Panama, Panama City, Panama. [Lips, Karen R.] Univ Maryland, Dept Biol, College Pk, MD 20742 USA. RP Crawford, AJ (reprint author), Smithsonian Trop Res Inst, Panama City, Panama. EM andrew@dna.ac OI Lips, Karen/0000-0002-2719-1551 FU National Science Foundation [DEB 0213851, 0234386, 0130273, 9996355]; Bay and Paul Foundation FX The Panamanian National Environmental Authority granted collecting and export permits. A. Driskell, A. Ormos and L. Weigt (Smithsonian Institution's Laboratory of Analytical Biology) contributed most of the raw DNA barcode data. Field assistance was provided by J. Ray, J. Robertson, F. Brem, R. Brenes, M. Ryan, and L. Witters. Circulo Herpetologico de Panama contributed additional samples. R. Ibanez provided valuable insights. M. Ruiz, S. Galeano and S. Flechas provided assistance. Comments from D. Wake, S. Castroviejo-Fisher and two anonymous reviewers substantially improved this document. Field work was funded by National Science Foundation Grants DEB 0213851, 0234386, 0130273, and 9996355 and a Bay and Paul Foundation grant (to K. R. L.). NR 69 TC 157 Z9 169 U1 12 U2 76 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD AUG 3 PY 2010 VL 107 IS 31 BP 13777 EP 13782 DI 10.1073/pnas.0914115107 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 634SP UT WOS:000280605900042 PM 20643927 ER PT J AU Miloslavich, P Diaz, JM Klein, E Jose Alvarado, J Diaz, C Gobin, J Escobar-Briones, E Cruz-Motta, JJ Weil, E Cortes, J Bastidas, AC Robertson, R Zapata, F Martin, A Castillo, J Kazandjian, A Ortiz, M AF Miloslavich, Patricia Manuel Diaz, Juan Klein, Eduardo Jose Alvarado, Juan Diaz, Cristina Gobin, Judith Escobar-Briones, Elva Jose Cruz-Motta, Juan Weil, Ernesto Cortes, Jorge Carolina Bastidas, Ana Robertson, Ross Zapata, Fernando Martin, Alberto Castillo, Julio Kazandjian, Aniuska Ortiz, Manuel TI Marine Biodiversity in the Caribbean: Regional Estimates and Distribution Patterns SO PLOS ONE LA English DT Review ID CORAL-ALGAL SYMBIOSIS; PUERTO-RICO TRENCH; VENEZUELA BASIN; CLIMATE-CHANGE; SHALLOW-WATER; ECHINODERMS ECHINODERMATA; COMMUNITY STRUCTURE; CAYOS-COCHINOS; ROCKY SHORES; PHASE-SHIFTS AB This paper provides an analysis of the distribution patterns of marine biodiversity and summarizes the major activities of the Census of Marine Life program in the Caribbean region. The coastal Caribbean region is a large marine ecosystem (LME) characterized by coral reefs, mangroves, and seagrasses, but including other environments, such as sandy beaches and rocky shores. These tropical ecosystems incorporate a high diversity of associated flora and fauna, and the nations that border the Caribbean collectively encompass a major global marine biodiversity hot spot. We analyze the state of knowledge of marine biodiversity based on the geographic distribution of georeferenced species records and regional taxonomic lists. A total of 12,046 marine species are reported in this paper for the Caribbean region. These include representatives from 31 animal phyla, two plant phyla, one group of Chromista, and three groups of Protoctista. Sampling effort has been greatest in shallow, nearshore waters, where there is relatively good coverage of species records; offshore and deep environments have been less studied. Additionally, we found that the currently accepted classification of marine ecoregions of the Caribbean did not apply for the benthic distributions of five relatively well known taxonomic groups. Coastal species richness tends to concentrate along the Antillean arc (Cuba to the southernmost Antilles) and the northern coast of South America (Venezuela -Colombia), while no pattern can be observed in the deep sea with the available data. Several factors make it impossible to determine the extent to which these distribution patterns accurately reflect the true situation for marine biodiversity in general: (1) highly localized concentrations of collecting effort and a lack of collecting in many areas and ecosystems, (2) high variability among collecting methods, (3) limited taxonomic expertise for many groups, and (4) differing levels of activity in the study of different taxa. C1 [Miloslavich, Patricia; Klein, Eduardo; Jose Cruz-Motta, Juan; Martin, Alberto] Univ Simon Bolivar, Dept Estudios Ambientales, Caracas, Venezuela. [Miloslavich, Patricia; Klein, Eduardo; Jose Cruz-Motta, Juan; Martin, Alberto; Castillo, Julio; Kazandjian, Aniuska] Univ Simon Bolivar, Ctr Biodiversidad Marina, Caracas, Venezuela. [Manuel Diaz, Juan; Castillo, Julio] Univ Nacl Colombia, Bogota, Colombia. [Jose Alvarado, Juan; Cortes, Jorge] Univ Costa Rica, Ctr Invest Ciencias Mar & Limnol CIMAR, San Jose, Costa Rica. [Diaz, Cristina] Museo Mar, Margarita, Venezuela. [Gobin, Judith] Univ W Indies, Dept Life Sci, St Augustine, Trinid & Tobago. [Escobar-Briones, Elva] Univ Nacl Autonoma Mexico, Inst Ciencias Mar & Limnol, Mexico City 04510, DF, Mexico. [Weil, Ernesto] Univ Puerto Rico, Dept Marine Sci, Lajas, PR USA. [Carolina Bastidas, Ana; Kazandjian, Aniuska] Univ Simon Bolivar, Dept Biol Organismos, Caracas, Venezuela. [Robertson, Ross] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Zapata, Fernando] Univ Valle, Dept Biol, Cali, Colombia. [Ortiz, Manuel] Univ La Habana, Ctr Invest Marinas, Havana, Cuba. RP Miloslavich, P (reprint author), Univ Simon Bolivar, Dept Estudios Ambientales, Caracas, Venezuela. EM pmilos@usb.ve RI Alvarado, Juan /A-4002-2012; OI Klein, Eduardo/0000-0003-2935-7065 FU Alfred P. Sloan Foundation; Centro de Biodiversidad Marina CBM; Decanato de Investigacion y Desarrollo of the Universidad Simon Bolivar; Smithsonian Marine Sciences Network FX The Alfred P. Sloan Foundation, the Centro de Biodiversidad Marina CBM and the Decanato de Investigacion y Desarrollo of the Universidad Simon Bolivar provided funds for this work. The Smithsonian Marine Sciences Network provided financial support of the fish work. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 311 TC 71 Z9 88 U1 9 U2 107 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 AUG 2 PY 2010 VL 5 IS 8 AR e11916 DI 10.1371/journal.pone.0011916 PG 25 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 633RA UT WOS:000280520400012 PM 20689856 ER PT J AU Cameron, DD Bolin, JF AF Cameron, Duncan D. Bolin, Jay F. TI ISOTOPIC EVIDENCE OF PARTIAL MYCOHETEROTROPHY IN THE GENTIANACEAE: BARTONIA VIRGINICA AND OBOLARIA VIRGINICA AS CASE STUDIES SO AMERICAN JOURNAL OF BOTANY LA English DT Article DE Bartonia virginica; C-13; carbon; Gentianaceae; mass spectrometry; mycorrhiza; mycoheterotrophy; N-15; Obolaria virginica; stable isotope ID CARBON; PLANTS; MIXOTROPHY; ERICACEAE; NITROGEN; ORCHIDS; FUNGI; PHOTOSYNTHESIS; GENTIANEAE; DELTA-N-15 AB Premise of the study : An estimated 10% of plant species have evolved to steal C from their symbiotic fungal partners (mycoheterotrophy), and while physiological evidence for full and partial mycoheterotrophy is well developed in the Orchidaceae and Ericaceae, it is lacking for the majority of other mycoheterotrophic taxa. The family Gentianaceae not only contains several lineages of achlorophyllous mycoheterotrophs, but also contains species that are putative partially mycoheterotrophic. The North American genera Bartonia and Obolaria (Gentianaceae) are green but have leaves reduced to scales or foliose bracts and so have ambiguous mycoheterotrophic status. Methods : We investigated the natural abundance C-13 and N-15 profiles of both genera along with total N and chlorophyll content and investigated mycorrhizal infection using light microscopy. Key results : The shoots of B. virginica were significantly more enriched in N-15 than the surrounding vegetation but not in C-13. In contrast, the shoots of O. virginica are not enriched in N-15 compared to the surrounding vegetation but were significantly enriched in C-13. Total N concentrations were significantly higher than the surrounding vegetation in B. virginica, while the collaroid roots of both species were infected by arbuscular mycorrhizal fungi. Conclusions : This microscopic evidence coupled with the natural abundance stable isotope profiles strongly suggests that both species are partially mycoheterotrophic. However, differences in the root-shoot stable isotopic patterns relative to surrounding vegetation between B. virginica and O. virginica are suggestive of the utilization of different physiological pathways or extent of commitment to mycoheterotrophic C gain. C1 [Cameron, Duncan D.] Univ Sheffield, Dept Anim & Plant Sci, Sheffield S10 2TN, S Yorkshire, England. [Bolin, Jay F.] Smithsonian Inst, Dept Bot, Washington, DC 20013 USA. RP Cameron, DD (reprint author), Univ Sheffield, Dept Anim & Plant Sci, Western Bank, Sheffield S10 2TN, S Yorkshire, England. EM d.cameron@sheffield.ac.uk OI Cameron, Duncan/0000-0002-5439-6544 FU Natural Environment Research Council UK [NE/E014070/1]; Mary Payne Hogan Botany Endowment at Old Dominion University FX The authors thank the Natural Environment Research Council UK (award number: NE/E014070/1 to D. D. C.) and the Mary Payne Hogan Botany Endowment at Old Dominion University for financial support. They also thank Dr. J. R. Leake and Prof. Sir David Read FRS for invaluable discussions, I. Johnson (University of Sheffield) for technical support, Prof. L. Musselman for field assistance (Old Dominion University) and H. Walker (University of Sheffield) for analyzing the samples for 13C and 15N. NR 29 TC 7 Z9 7 U1 0 U2 22 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 AUG PY 2010 VL 97 IS 8 BP 1272 EP 1277 DI 10.3732/ajb.0900292 PG 6 WC Plant Sciences SC Plant Sciences GA 633EH UT WOS:000280481800003 PM 21616879 ER PT J AU Nie, ZL Sun, H Chen, DA Meng, Y Manchester, SR Wen, J AF Nie, Ze-Long Sun, Hang Chen, Duan Meng, Ying Manchester, Steven R. Wen, Jun TI MOLECULAR PHYLOGENY AND BIOGEOGRAPHIC DIVERSIFICATION OF PARTHENOCISSUS (VITACEAE) DISJUNCT BETWEEN ASIA AND NORTH AMERICA SO AMERICAN JOURNAL OF BOTANY LA English DT Article DE Asia; boreotropical element; disjunction; North America; Parthenocissus; Vitaceae ID NUCLEAR RIBOSOMAL DNA; HEMISPHERE; EVOLUTION; SEQUENCES; MAGNOLIACEAE; DIVERGENCE; CONFIDENCE; INFERENCE; SELECTION; PATTERNS AB Premise of the study : Parthenocissus is a genus of the grape family Vitaceae and has a disjunct distribution in Asia and North America with members in both tropical and temperate regions. The monophyly of Parthenocissus has not yet been tested, and the species relationships and the evolution of its intercontinental disjunction have not been investigated with extensive sampling and molecular phylogenetic methods. Methods : Plastid (trnL-F, rps16, and atpB-rbcL) and nuclear GAI1 sequences of 56 accessions representing all 12 Parthenocissus species were analyzed with parsimony, likelihood, and Bayesian inference. Divergence times of disjunct lineages were estimated with relaxed Bayesian dating. Evolution of the leaflet number was assessed by tracing this character onto Bayesian trees using the Trace Character Over Trees option in the program Mesquite. Key results : Parthenocissus is monophyletic and sister to the newly described segregate genus Yua. Two major clades within Parthenocissus are recognizable corresponding to their distribution in Asia and North America. The disjunction between the two continents is estimated to be at 21.64 (95% higher posterior densities 10.23-34.89) million years ago. Conclusions : Parthenocissus is likely to have derived from the Eocene boreotropical element. Its current Asian-North American disjunction is dated to the early Miocene, congruent with fossil and paleoclimatic evidence. The tropical species is nested within the temperate clade and is inferred to have dispersed from the adjacent temperate regions. Parthenocissus and Yua are best treated as distinct genera. Leaflet number in this genus has a complex history and cannot be used as a character for infrageneric classification. C1 [Nie, Ze-Long; Sun, Hang; Meng, Ying; Wen, Jun] Chinese Acad Sci, Kunming Inst Bot, Key Lab Biodivers & Biogeog, Kunming 650204, Yunnan, Peoples R China. [Nie, Ze-Long] Chinese Acad Sci, Grad Sch, Beijing 100039, Peoples R China. [Chen, Duan; Wen, Jun] Chinese Acad Sci, Key Lab Systemat & Evolutionary Bot, Inst Bot, Beijing 100093, Peoples R China. [Manchester, Steven R.] Univ Florida, Dept Bot, Gainesville, FL 32611 USA. [Wen, Jun] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, MRC 166, Washington, DC 20013 USA. RP Wen, J (reprint author), Chinese Acad Sci, Kunming Inst Bot, Key Lab Biodivers & Biogeog, Kunming 650204, Yunnan, Peoples R China. EM wenj@si.edu RI Nie, Ze-Long/N-8471-2015 OI Nie, Ze-Long/0000-0001-8065-3981 FU National Basic Research Program of China (973 Program) [2007CB411601]; National Science Foundation [DEB 0743474]; Natural Science Foundation of China [NSFC 30625004, 40771073]; John D. and Catherine T. MacArthur Foundation; Laboratory of Analytical Biology of the National Museum of Natural History, Smithsonian Institution FX The authors thank Li-Min Lu for critically reading earlier versions of the manuscript. This study was supported by grants from the National Basic Research Program of China (973 Program, grant 2007CB411601), the National Science Foundation (grant DEB 0743474 to S. R. M. and J.W.), the Natural Science Foundation of China (grant NSFC 30625004 and 40771073 to H. S.), and the John D. and Catherine T. MacArthur Foundation to J.W., R. Ree, and G. Mueller. Laboratory work was done at and partially supported by the Laboratory of Analytical Biology of the National Museum of Natural History, Smithsonian Institution. Fieldwork in North America was supported by the Small Grants Program of the National Museum of Natural History, the Smithsonian Institution. NR 72 TC 28 Z9 31 U1 0 U2 19 PU BOTANICAL SOC AMER INC PI ST LOUIS PA PO BOX 299, ST LOUIS, MO 63166-0299 USA SN 0002-9122 J9 AM J BOT JI Am. J. Bot. PD AUG PY 2010 VL 97 IS 8 BP 1342 EP 1353 DI 10.3732/ajb.1000085 PG 12 WC Plant Sciences SC Plant Sciences GA 633EH UT WOS:000280481800011 PM 21616887 ER PT J AU Power, ML Ross, CN Tardif, SD AF Power, M. L. Ross, C. N. Tardif, S. D. TI THE DEVELOPMENT OF OBESITY BEGINS AT AN EARLY AGE IN CAPTIVE COMMON MARMOSETS (CALLITHRIX JACCHUS) SO AMERICAN JOURNAL OF PRIMATOLOGY LA English DT Meeting Abstract CT 33rd Annual Meeting of the American-Society-of-Primatologists CY JUN 16-19, 2010 CL Louisville, KY SP Amer Soc Primatologists, Louisville Zoo, Centre Coll, Bellarmine Univ C1 [Power, M. L.] Smithsonian Natl Zool Pk, Conservat Ecol Ctr, Nutr Lab, Washington, DC 20008 USA. [Ross, C. N.; Tardif, S. D.] Univ Texas Hlth Sci Ctr San Antonio, San Antonio, TX 78229 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0275-2565 J9 AM J PRIMATOL JI Am. J. Primatol. PD AUG PY 2010 VL 72 SU 1 MA 16 BP 30 EP 31 PG 2 WC Zoology SC Zoology GA 636GS UT WOS:000280720400017 ER PT J AU Bentley-Condit, VK Power, M AF Bentley-Condit, V. K. Power, M. TI AN EXAMINATION OF PROTEIN-FIBER RATIOS IN TANA RIVER PRIMATE NATIONAL RESERVE, KENYA, YELLOW BABOON (PAPIO CYNOCEPHALUS) FOODS: IS THERE A BABOON NORM? SO AMERICAN JOURNAL OF PRIMATOLOGY LA English DT Meeting Abstract CT 33rd Annual Meeting of the American-Society-of-Primatologists CY JUN 16-19, 2010 CL Louisville, KY SP Amer Soc Primatologists, Louisville Zoo, Centre Coll, Bellarmine Univ C1 [Bentley-Condit, V. K.] Grinnell Coll, Dept Anthropol, Grinnell, IA 50112 USA. [Power, M.] Smithsonian Inst, Nutr Lab, Conservat Ecol Ctr, Natl Zool Pk, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 1 U2 1 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0275-2565 J9 AM J PRIMATOL JI Am. J. Primatol. PD AUG PY 2010 VL 72 SU 1 MA 39 BP 37 EP 38 PG 2 WC Zoology SC Zoology GA 636GS UT WOS:000280720400040 ER PT J AU Foerster, S Cords, M Monfort, SL AF Foerster, S. Cords, M. Monfort, S. L. TI METABOLIC BUT NOT PSYCHOLOGICAL STRESSORS MODULATE TEMPORAL AND INTER-INDIVIDUAL VARIATION IN FECAL GLUCOCORTICOID LEVELS AMONG WILD FEMALE CERCOPITHECUS MITIS IN TWO KENYAN POPULATIONS SO AMERICAN JOURNAL OF PRIMATOLOGY LA English DT Meeting Abstract CT 33rd Annual Meeting of the American-Society-of-Primatologists CY JUN 16-19, 2010 CL Louisville, KY SP Amer Soc Primatologists, Louisville Zoo, Centre Coll, Bellarmine Univ C1 [Foerster, S.; Cords, M.] Columbia Univ, Dept Ecol Evolut & Environm Biol, New York, NY USA. [Foerster, S.] Natl Museums Kenya, Inst Primate Res, Nairobi, Kenya. [Monfort, S. L.] Smithsonian Conservat Biol Inst, Front Royal, VA USA. NR 0 TC 0 Z9 0 U1 0 U2 2 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0275-2565 J9 AM J PRIMATOL JI Am. J. Primatol. PD AUG PY 2010 VL 72 SU 1 MA 149 BP 73 EP 73 PG 1 WC Zoology SC Zoology GA 636GS UT WOS:000280720400150 ER PT J AU Stubbs, JE Post, JE Elbert, DC Heaney, PJ Veblen, DR AF Stubbs, Joanne E. Post, Jeffrey E. Elbert, David C. Heaney, Peter J. Veblen, David R. TI Uranyl phosphate sheet reconstruction during dehydration of metatorbernite [Cu(UO2)(2)(PO4)(2)center dot 8H(2)O] SO AMERICAN MINERALOGIST LA English DT Article DE Uranium; autunite; torbernite; metatorbernite; meta-autunite; Rietveld; synchrotron X-ray powder diffraction ID CONTAMINATED HANFORD SEDIMENTS; RAY-POWDER DIFFRACTION; X-RAY; CRYSTAL-STRUCTURES; META-AUTUNITE; VADOSE ZONE; MICROPROBE ANALYSIS; URANIUM SPECIATION; MINERALS; SITE AB The metatorbernite [Cu(UO2)(2)(PO4)(2)center dot 8H(2)O] structure comprises autunite-type sheets of corner-sharing uranyl square bipyramids and phosphate tetrahedra, with the interlayer region occupied by Cu2+ ions and molecular water. Previous studies have shown that heating induces stepwise dehydration and reduction in basal spacing. Structures of the lower hydrates have not been determined previously because suitable single crystals of these phases have yet to be prepared. We have used synchrotron X-ray diffraction data collected during in situ, continuous heating of powdered metatorbernite to elucidate structures of its lower hydrates. Using Rietveld analysis, we have determined that autunite-type sheets remain intact through the first dehydration event above room temperature (onset 102 degrees C). We have discovered that the second dehydration event (onset 138 C) triggers a major reconstruction to uranophane-type sheets, composed of chains of edge-sharing uranyl pentagonal bipyramids linked to one another by sharing edges and vertices with phosphate tetrahedra. This reconstruction enables the structure to overcome steric constraints on the minimum possible basal spacing, while maintaining Cu within the interlayer. Four distinct phases have been identified with increasing temperature: Cu(UO2)(2)(PO4)(2)center dot 8H(2)O, space group P4/n, a = 6.96519(23), c = 17.3102(8) angstrom; Cu(UO2)(2)(PO4)(2)center dot 6.1H(2)O, space group P4/n, a = 6.95510(29), c = 16.6604(9) angstrom; Cu(UO2)(2)(PO4)(2)center dot 3H(2)O, space group P2(1), a = 14.4979(23), b = 7.0159(9), c = 6.6312(10) angstrom, beta = 107.585(14)degrees; and a lower hydrate with monoclinic or triclinic symmetry, a approximate to 6.7, b approximate to 7, c approximate to 11 angstrom, beta approximate to 100 degrees. As shown here, in situ heating experiments and the Rietveld method provide fundamental insights into the crystal chemistry and structural behaviors of the important meta-autunite mineral group. C1 [Stubbs, Joanne E.; Elbert, David C.; Veblen, David R.] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA. [Post, Jeffrey E.] Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. [Heaney, Peter J.] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. RP Stubbs, JE (reprint author), Stanford Synchrotron Radiat Lightsource, Menlo Pk, CA 94025 USA. EM jstubbs1@jhu.edu RI Stubbs, Joanne/F-9710-2013 OI Stubbs, Joanne/0000-0002-8509-2009 FU U.S. Department of Energy, Basic Energy Sciences [DEFG02-89ER14074]; NSF [EAR07-45374, CHE04-31328]; Center for Environmental Kinetics Analysis (CEKA); DOE; U.S. Department of Energy, Office of Science, Office of Basic Energy Sciences [DEAC02-98CH10886] FX This research was supported by U.S. Department of Energy, Basic Energy Sciences Grant no. DEFG02-89ER14074 to D.R.V. and D.C.E., NSF Grant no. EAR07-45374 to P.J.H. and J.E.P., and the Center for Environmental Kinetics Analysis (CEKA), an NSF- and DOE-sponsored Environmental Molecular Science Insititute (NSF Grant no. CHE04-31328 to Pill.). Use of the National Synchrotron Light Source, Brookhaven National Laboratory, was supported by the U.S. Department of Energy, Office of Science, Office of Basic Energy Sciences, under Contract no. DEAC02-98CH10886. We thank Peter Burns for commenting on an earlier draft of the manuscript. We thank our AE, Aaron Celestian, and three anonymous reviewers for their helpful suggestions. NR 49 TC 8 Z9 8 U1 1 U2 15 PU MINERALOGICAL SOC AMER PI CHANTILLY PA 3635 CONCORDE PKWY STE 500, CHANTILLY, VA 20151-1125 USA SN 0003-004X J9 AM MINERAL JI Am. Miner. PD AUG-SEP PY 2010 VL 95 IS 8-9 BP 1132 EP 1140 DI 10.2138/am.2010.3439 PG 9 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA 642NE UT WOS:000281220900002 ER PT J AU Mccubbin, FM Steele, A Nekvasil, H Schnieders, A Rose, T Fries, M Carpenter, PK Jolliff, BL AF Mccubbin, Francis M. Steele, Andrew Nekvasil, Hanna Schnieders, Albert Rose, Timothy Fries, Marc Carpenter, Paul K. Jolliff, Bradley L. TI Detection of structurally bound hydroxyl in fluorapatite from Apollo Mare basalt 15058,128 using TOF-SIMS SO AMERICAN MINERALOGIST LA English DT Article DE Water on Moon; TOF-SIMS; apatite; mare basalt; lunar water; EPMA; Raman spectroscopy; Apollo sample ID RAMAN-SPECTROSCOPY; MASS-SPECTROMETRY; CRYSTAL-CHEMISTRY; PLANETARY MAGMAS; STARDUST AEROGEL; APATITE; MOON; SURFACE; WATER; OH AB Fluorapatite grains from Apollo 15 Mare basalt 15058,128 were analyzed by Raman spectroscopy, Raman spectral imaging, time-of-flight secondary ion mass spectrometry (TOF-SIMS), field emission scanning electron microscopy (FE-SEM), and electron probe microanalysis (EPMA) in an attempt to detect structurally bound OH(-) in the fluorapatite. Although OH(-) could not be definitively detected by Raman spectroscopy because of REE-induced photoluminescence, hydroxyl was detected in the fluorapatite by TOF-SIMS. The TOF-SIMS technique is qualitative but capable of detecting the presence of hydroxyl even at trace levels. Electron microprobe data indicate that on average, F and Cl (F+Cl) fill the monovalent anion site in these fluorapatite grains within the uncertainties of the analyses (about 0.07 +/- 0.01 atoms per formula unit). However, some individual spot analyses have F+Cl deficiencies greater than analytical uncertainties that could represent structural OH(-). On the basis of EPMA data, the fluorapatite grain with the largest F+Cl deficiency constrains the upper limit of the OH(-) content to be no more than 4600 +/- 2000 ppm by weight (the equivalent of similar to 2400 +/- 1100 ppm water). The TOF-SIMS detection of OH(-) in fluorapatite from Apollo sample 15058,128 represents the first direct confirmation of structurally bound hydroxyl in a lunar magmatic mineral. This result provides justification for attributing at least some of the missing structural component in the monovalent anion site of other lunar fluorapatite grains to the presence of OH(-). Moreover, this finding supports the presence of dissolved water in lunar magmas and the presence of at least some water within the lunar interior. C1 [Mccubbin, Francis M.; Steele, Andrew] Carnegie Inst Washington, Geophys Lab, Washington, DC 20015 USA. [Nekvasil, Hanna] SUNY Stony Brook, Dept Geosci, Stony Brook, NY 11794 USA. [Schnieders, Albert] ION TOF USA Inc, New York, NY 10977 USA. [Rose, Timothy] Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. [Fries, Marc] Jet Prop Lab, Pasadena, CA 91109 USA. [Carpenter, Paul K.; Jolliff, Bradley L.] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. [Carpenter, Paul K.; Jolliff, Bradley L.] Washington Univ, McDonnell Ctr Space Sci, St Louis, MO 63130 USA. RP Mccubbin, FM (reprint author), Carnegie Inst Washington, Geophys Lab, 5251 Broad Branch Rd NW, Washington, DC 20015 USA. EM fmccubbin@ciw.edu RI McCubbin, Francis/D-1698-2009 FU NASA [NNX08AZ04G]; LASER program; NASA SRLIDA; Mars Fundamental Research programs; NASA's Cosmochemistry program; Carnegie Institution of Washington; Geophysical Laboratory; NASA Astrobiology Institute FX We thank the Lunar Curatorial staff at the Lyndon B. Johnson Space Center in Houston, Texas, for allocation of the thin section of Apollo sample 15058,128. We are grateful for Daniel Harlov and Jennifer Thomson for the editorial handling of this manuscript. Insightful and constructive reviews were provided by John Hughes and Philip Piccoli. We also thank Alberto E. Patino Douce and Lutz Nasdala for helpful and insightful reviews of a previous version of the manuscript. Steven Symes and Bjorn Mysen are acknowledged for productive and fruitful discussions on this topic. Financial support for this work was provided by NASA grant NNX08AZ04G from the LASER program awarded to Hanna Nekvasil; Andrew Steele acknowledges support from the NASA SRLIDA and Mars Fundamental Research programs; and Brad Jolliff acknowledges support from NASA's Cosmochemistry program. Francis McCubbin acknowledges fellowship support from the Carnegie Institution of Washington, Geophysical Laboratory, and NASA Astrobiology Institute during this study. NR 53 TC 69 Z9 69 U1 2 U2 27 PU MINERALOGICAL SOC AMER PI CHANTILLY PA 3635 CONCORDE PKWY STE 500, CHANTILLY, VA 20151-1125 USA SN 0003-004X J9 AM MINERAL JI Am. Miner. PD AUG-SEP PY 2010 VL 95 IS 8-9 BP 1141 EP 1150 DI 10.2138/am.2010.3448 PG 10 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA 642NE UT WOS:000281220900003 ER PT J AU Estrada, C Gilbert, LE AF Estrada, Catalina Gilbert, Lawrence E. TI Host plants and immatures as mate-searching cues in Heliconius butterflies SO ANIMAL BEHAVIOUR LA English DT Article DE butterfly; Heliconius; host fidelity; host plant; male mate searching; pupal mating; plant volatile; sexual behaviour ID REPRODUCTIVE ISOLATION; SEX-PHEROMONE; PHYTOPHAGOUS INSECTS; LOCATING BEHAVIOR; SYMPATRIC RACES; CHEMICAL CUES; GENE FLOW; EVOLUTION; VOLATILES; LEPIDOPTERA AB The study of interactions between phytophagous insects and their host plants extends beyond understanding how insects deal with plant chemical defences. Sexual behaviour of these herbivores is integrated in several ways with host plants, as the latter influence timing and location of reproduction, and can provide clues for finding mates. Nevertheless, while numerous studies link butterfly evolution to host plant adaptations, the influence of plants on butterfly sexual behaviour has been little studied. We conducted experiments to determine the role of host plant cues in mate-searching behaviour of Heliconius charithonia butterflies. This species exhibits precopulatory mate guarding behaviour, wherein males find and perch on pupae, then copulate with eclosing females ('pupal mating'). We found that males (1) visited plants damaged by feeding larvae more often than they visited undamaged plants and (2) displayed searching behaviour around the plant and in front of larvae, suggesting that odours signal the location of potential partners (pupae). Although males were attracted to common plant odours released after tissue damage, plants damaged by heterospecific butterfly larvae were less attractive, indicating that species recognition can occur at early life stages. Overall, our results suggest that host plants influence mate-searching behaviour of Heliconius. This might also be true for other species of butterflies with more conventional mating strategies, potentially contributing to the diversification of this group of phytophagous insects. (C) 2010 The Association for the Study of Animal Behaviour. Published by Elsevier Ltd. All rights reserved. C1 [Estrada, Catalina; Gilbert, Lawrence E.] Univ Texas Austin, Austin, TX 78712 USA. RP Estrada, C (reprint author), Smithsonian Trop Res Inst, Apartado Postal 0843-03092, Balboa, Ancon, Panama. EM catalinaestra72@hotmail.com FU National Science Foundation (NSF); Office of International Science and Engineering [DDIG 0608167]; Texas Academy of Sciences; Southwestern Association of Naturalists; Private Lands Research Grants; Environmental Science Institute; Section of Integrative Biology; NSF; University of Texas, Austin FX We thank Barrett Klein for help with the caterpillar silicone models, Molly Cummins and Mike Ryan for assistance with spectrometer and UV analysis. We are grateful to Mary Owens, Angie Martinez, Jamtsho, Tony Alexander, John and Grace Crutchfield, Priscilla Martinez, Siona Marout, Ariani Wartenberg, Kathryn Busby and Colin Strickland for their help with data, rearing and maintenance of greenhouse facilities, to Samraat Pawar, Christian Salcedo, Mike Singer and two anonymous referees for comments on the manuscript. This work was supported by the National Science Foundation (NSF) and the Office of International Science and Engineering (DDIG 0608167), the Texas Academy of Sciences, the Southwestern Association of Naturalists, Private Lands Research Grants, the Environmental Science Institute and the Section of Integrative Biology. Greenhouse facilities in Austin were developed through grants from NSF support and the University of Texas, Austin, to L.E.G. NR 79 TC 11 Z9 11 U1 2 U2 26 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0003-3472 J9 ANIM BEHAV JI Anim. Behav. PD AUG PY 2010 VL 80 IS 2 BP 231 EP 239 DI 10.1016/j.anbehav.2010.04.023 PG 9 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA 627SY UT WOS:000280064400010 ER PT J AU Garg, A Cook, KH Nikolaev, S Huber, ME Rest, A Becker, AC Challis, P Clocchiatti, A Miknaitis, G Minniti, D Morelli, L Olsen, K Prieto, JL Suntzeff, NB Welch, DL Wood-Vasey, WM AF Garg, A. Cook, K. H. Nikolaev, S. Huber, M. E. Rest, A. Becker, A. C. Challis, P. Clocchiatti, A. Miknaitis, G. Minniti, D. Morelli, L. Olsen, K. Prieto, J. L. Suntzeff, N. B. Welch, D. L. Wood-Vasey, W. M. TI HIGH-AMPLITUDE delta-SCUTIS IN THE LARGE MAGELLANIC CLOUD SO ASTRONOMICAL JOURNAL LA English DT Article DE Magellanic Clouds; surveys ID ESSENCE SUPERNOVA SURVEY; RR LYRAE STARS; MACHO PROJECT; IMAGE SUBTRACTION; VARIABLE-STARS; PULSATION; PHOTOMETRY; CATALOG; GALAXY; SPACE AB We present 2323 high-amplitude delta-Scuti (HADS) candidates discovered in the Large Magellanic Cloud by the SuperMACHO survey (Rest et al.). Frequency analyses of these candidates reveal that several are multimode pulsators, including 119 whose largest amplitude of pulsation is in the fundamental (F) mode and 19 whose largest amplitude of pulsation is in the first overtone (FO) mode. Using Fourier decomposition of the HADS light curves, we find that the period-luminosity (PL) relation defined by the FO pulsators does not show a clear separation from the PL relation defined by the F pulsators. This differs from other instability strip pulsators such as type c RR Lyrae. We also present evidence for a larger amplitude, subluminous population of HADS similar to that observed in Fornax. C1 [Garg, A.; Cook, K. H.; Nikolaev, S.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94550 USA. [Huber, M. E.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Rest, A.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Rest, A.; Olsen, K.; Suntzeff, N. B.] Natl Opt Astron Observ, Cerro Tololo Inter Amer Observ, La Serena, Chile. [Becker, A. C.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Challis, P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Clocchiatti, A.; Minniti, D.] Pontificia Univ Catolica Chile, Dept Astron, Santiago 22, Chile. [Minniti, D.] Vatican Observ, V-00120 Vatican City, Vatican. [Miknaitis, G.] Ctr Neighborhood Technol, Chicago, IL 60647 USA. [Morelli, L.] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy. [Olsen, K.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Prieto, J. L.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Suntzeff, N. B.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA. [Suntzeff, N. B.] Texas A&M Univ, Mitchell Inst Fundamental Phys & Astron, College Stn, TX 77843 USA. [Welch, D. L.] McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1, Canada. [Wood-Vasey, W. M.] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. RP Garg, A (reprint author), Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, 7000 East Ave, Livermore, CA 94550 USA. FU NOAO; National Science Foundation; STScI [GO-10583]; U.S. Department of Energy [DE-AC52-07NA27344]; McDonnell Foundation; Harvard University; ICM-MIDEPLAN [P06-045-F]; FONDAP [15010003, 0609]; Padova University [CPDR061795/06]; Natural Sciences and Engineering Research Council of Canada (NSERC) FX We thank D. H. McNamara for his helpful insights into this data set. The SuperMACHO survey was undertaken under the auspices of the NOAO Survey Program. We are very grateful for the support provided to the Survey program from the NOAO and the National Science Foundation. We are particularly indebted to the scientists and staff at the Cerro Tololo Inter-American Observatory for their assistance in helping us carry out the survey. SuperMACHO is supported by the STScI grant GO-10583. We are grateful to the members of the ESSENCE supernova survey with whom we work closely. We thank the High Performance Technical Computing staff at Harvard. A.G.'s, K.H.C.'s, M.E.H.'s, and S.N.'s work was performed under the auspices of the U.S. Department of Energy by Lawrence Livermore National Laboratory under Contract DE-AC52-07NA27344. C. Stubbs thanks the McDonnell Foundation for its support through a Centennial Fellowship. A. G. and A. R. are also grateful for support from Harvard University. A. C. acknowledges the support of grant P06-045-F ICM-MIDEPLAN. D. M. and A. C. are supported by grants FONDAP CFA 15010003 and Basal CATA 0609. L. M. is supported by grant (CPDR061795/06) from Padova University. D. L. W. acknowledges financial support in the form of a Discovery Grant from the Natural Sciences and Engineering Research Council of Canada (NSERC). NR 36 TC 9 Z9 9 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD AUG PY 2010 VL 140 IS 2 BP 328 EP 338 DI 10.1088/0004-6256/140/2/328 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 626HW UT WOS:000279958000003 ER PT J AU Bonanos, AZ Lennon, DJ Kohlinger, F van Loon, JT Massa, DL Sewilo, M Evans, CJ Panagia, N Babler, BL Block, M Bracker, S Engelbracht, CW Gordon, KD Hora, JL Indebetouw, R Meade, MR Meixner, M Misselt, KA Robitaille, TP Shiao, B Whitney, BA AF Bonanos, A. Z. Lennon, D. J. Koehlinger, F. van Loon, J. Th. Massa, D. L. Sewilo, M. Evans, C. J. Panagia, N. Babler, B. L. Block, M. Bracker, S. Engelbracht, C. W. Gordon, K. D. Hora, J. L. Indebetouw, R. Meade, M. R. Meixner, M. Misselt, K. A. Robitaille, T. P. Shiao, B. Whitney, B. A. TI SPITZER SAGE-SMC INFRARED PHOTOMETRY OF MASSIVE STARS IN THE SMALL MAGELLANIC CLOUD SO ASTRONOMICAL JOURNAL LA English DT Article DE catalogs; galaxies: individual (SMC); infrared: stars; stars: early-type; stars: emission-line; Be; stars: massive ID GIANT BRANCH STARS; O-TYPE STARS; B-TYPE STARS; GRAVITATIONAL LENSING EXPERIMENT; BLANKETED MODEL ATMOSPHERES; EFFECTIVE TEMPERATURE SCALE; VLT-FLAMES SURVEY; WOLF-RAYET STARS; RED SUPERGIANTS; LOSS RATES AB We present a catalog of 5324 massive stars in the Small Magellanic Cloud (SMC), with accurate spectral types compiled from the literature, and a photometric catalog for a subset of 3654 of these stars, with the goal of exploring their infrared properties. The photometric catalog consists of stars with infrared counterparts in the Spitzer SAGE-SMC survey database, for which we present uniform photometry from 0.3 to 24 mu m in the UBVIJHK(s)+IRAC+MIPS24 bands. We compare the color-magnitude diagrams and color-color diagrams to those of stars in the Large Magellanic Cloud (LMC), finding that the brightest infrared sources in the SMC are also the red supergiants, supergiant B[e] (sgB[e]) stars, luminous blue variables, and Wolf-Rayet stars, with the latter exhibiting less infrared excess, the red supergiants being less dusty and the sgB[e] stars being on average less luminous. Among the objects detected at 24 mu m in the SMC are a few very luminous hypergiants, four B-type stars with peculiar, flat spectral energy distributions, and all three known luminous blue variables. We detect a distinct Be star sequence, displaced to the red, and suggest a novel method of confirming Be star candidates photometrically. We find a higher fraction of Oe and Be stars among O and early-B stars in our SMC catalog, respectively, when compared to the LMC catalog, and that the SMC Be stars occur at higher luminosities. We estimate mass-loss rates for the red supergiants, confirming the correlation with luminosity even at the metallicity of the SMC. Finally, we confirm the new class of stars displaying composite A & F type spectra, the sgB[e] nature of 2dFS1804 and find the F0 supergiant 2dFS3528 to be a candidate luminous blue variable with cold dust. C1 [Bonanos, A. Z.] Natl Observ Athens, Inst Astron & Astrophys, Athens 15236, Greece. [Lennon, D. J.; Massa, D. L.; Sewilo, M.; Panagia, N.; Gordon, K. D.; Meixner, M.; Shiao, B.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Lennon, D. J.] European Space Agcy, Res & Sci Support Dept, Baltimore, MD 21218 USA. [Koehlinger, F.] Univ Heidelberg, Dept Phys & Astron, D-69120 Heidelberg, Germany. [van Loon, J. Th.] Univ Keele, Lennard Jones Labs, Astrophys Grp, Keele ST5 5BG, Staffs, England. [Evans, C. J.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Panagia, N.] Osserv Astrofis Catania, INAF, I-95123 Catania, Italy. [Panagia, N.] Supernova Ltd, Virgin Gorda, British Virgin, England. [Babler, B. L.; Bracker, S.; Engelbracht, C. W.; Meade, M. R.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Block, M.; Misselt, K. A.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Hora, J. L.; Robitaille, T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Indebetouw, R.] Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. [Whitney, B. A.] Space Sci Inst, Boulder, CO 80301 USA. RP Bonanos, AZ (reprint author), Natl Observ Athens, Inst Astron & Astrophys, I Metaxa & Vas Pavlou St, Athens 15236, Greece. EM bonanos@astro.noa.gr; lennon@stsci.edu; koehlinger@stud.uni-heidelberg.de; jacco@astro.keele.ac.uk; massa@stsci.edu; sewilo@stsci.edu; chris.evans@stfc.ac.uk; panagia@stsci.edu; brian@sal.wisc.edu; mblock@as.arizona.edu; s_bracker@hotmail.com; cengelbracht@as.arizona.edu; kgordon@stsci.edu; jhora@cfa.harvard.edu; remy@virginia.edu; meade@astro.wisc.edu; meixner@stsci.edu; kmisselt@as.arizona.edu; trobitaille@cfa.harvard.edu; shiao@stsci.edu; bwhitney@spacescience.org RI Bonanos, Alceste/K-5392-2013; OI Bonanos, Alceste/0000-0003-2851-1905; Kohlinger, Fabian/0000-0001-6286-9797; Lennon, Daniel/0000-0003-3063-4867; Babler, Brian/0000-0002-6984-5752; Hora, Joseph/0000-0002-5599-4650; Robitaille, Thomas/0000-0002-8642-1329 FU Space Telescope Science Institute; NASA [NAG5-12595]; National Aeronautics and Space Administration; National Science Foundation FX A.Z.B. acknowledges support from the Riccardo Giacconi Fellowship award of the Space Telescope Science Institute and from the European Commission Framework Program Seven under a Marie Curie International Reintegration Grant. The Spitzer SAGE-SMC project was supported by NASA grant NAG5-12595. This work is based (in part) on archival data obtained with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by an award issued by JPL/Caltech. This publication makes use of data products from the 2MASS, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. NR 98 TC 71 Z9 71 U1 1 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD AUG PY 2010 VL 140 IS 2 BP 416 EP 429 DI 10.1088/0004-6256/140/2/416 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 626HW UT WOS:000279958000010 ER PT J AU Wolk, SJ Pillitteri, I Guinan, E Stencel, R AF Wolk, Scott J. Pillitteri, Ignazio Guinan, Edward Stencel, Robert TI XMM-NEWTON OBSERVATIONS OF THE ENIGMATIC LONG PERIOD ECLIPSING BINARY EPSILON AURIGAE: CONSTRAINING THE PHYSICAL MODELS SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries: eclipsing; stars: chemically peculiar; stars: individual (Epsilon Aurigae) ID GIANT BRANCH EVOLUTION; SECONDARY; STARS; DISK; SYSTEM; MASS; ACCRETION; COMPONENT; POLARIS; CLUSTER AB We report on an XMM-Newton observation of the unusual, long period (F0 supergiant + cool disk companion) eclipsing binary star epsilon Aurig observed in X-rays prior to the onset of the 2009-2011 eclipse phase. While it appears certain that a disk-like body is obscuring the star, it remains unclear what kind of object is at the center of the disk. The XMM-Newton observation had a duration of similar to 25 ks. The X-ray image does not show a source at the optical position of the star. We have determined a limiting X-ray flux of about 2.5x10(-15) erg cm(-2) s(-1). This flux is equivalent to a luminosity of about log L(X) similar to 29.3-29.7 erg s(-1) for an unabsorbed source at the assumed distance, estimated to be between 650 and 1300 pc. The direct emission from an otherwise unobscured primary is excluded at a level above L(X) similar to 4 x 10(29) erg s(-1). We explore the physical constraints that these limits put on the primary and several proposed models for the system secondary. For a black hole, we find that the direct absorption required by the disk is approximately N(H) >= 10(25) cm(-2). While not unreasonable for a protoplanetary disk, the lack of secondary X-rays makes this model unlikely. For high-mass models, in which the disk harbors pre-main-sequence stars, we find a minimum disk absorption of NH similar to 1023 cm(-2). Since this is not unlikely for a protoplanetary disk, this is not a significant constraint. For low-mass models, in which the disk harbors older stars, the known line-of-sight absorption is nearly enough to account for the non-detection. The data do not discriminate between these models. C1 [Wolk, Scott J.; Pillitteri, Ignazio] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Guinan, Edward] Villanova Univ, Dept Astron, Villanova, PA 19085 USA. [Stencel, Robert] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA. RP Wolk, SJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Pillitteri, Ignazio/L-1549-2016; OI Pillitteri, Ignazio/0000-0003-4948-6550; Wolk, Scott/0000-0002-0826-9261 FU NASA [NAS8-03060]; XMM guest investigator program [NNX10AE52G]; NSF/RUI [5-0507536, 5-0507542] FX S.J.W. was supported by NASA contract NAS8-03060. I. P. was supported by XMM guest investigator program through grant NNX10AE52G. E. F. G. was supported by NSF/RUI grants 5-0507536 and 5-0507542. We thank Nancy Adams and Nancy Evans for providing a critical review of the revised draft. NR 55 TC 6 Z9 6 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD AUG PY 2010 VL 140 IS 2 BP 595 EP 601 DI 10.1088/0004-6256/140/2/595 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 626HW UT WOS:000279958000025 ER PT J AU Hall, NR Keisler, R Knox, L Reichardt, CL Ade, PAR Aird, KA Benson, BA Bleem, LE Carlstrom, JE Chang, CL Cho, HM Crawford, TM Crites, AT De Haan, T Dobbs, MA George, EM Halverson, NW Holder, GP Holzapfel, WL Hrubes, JD Joy, M Lee, AT Leitch, EM Lueker, M McMahon, JJ Mehl, J Meyer, SS Mohr, JJ Montroy, TE Padin, S Plagge, T Pryke, C Ruhl, JE Schaffer, KK Shaw, L Shirokoff, E Spieler, HG Stalder, B Staniszewski, Z Stark, AA Switzer, ER Vanderlinde, K Vieira, JD Williamson, R Zahn, O AF Hall, N. R. Keisler, R. Knox, L. Reichardt, C. L. Ade, P. A. R. Aird, K. A. Benson, B. A. Bleem, L. E. Carlstrom, J. E. Chang, C. L. Cho, H. -M. Crawford, T. M. Crites, A. T. De Haan, T. Dobbs, M. A. George, E. M. Halverson, N. W. Holder, G. P. Holzapfel, W. L. Hrubes, J. D. Joy, M. Lee, A. T. Leitch, E. M. Lueker, M. McMahon, J. J. Mehl, J. Meyer, S. S. Mohr, J. J. Montroy, T. E. Padin, S. Plagge, T. Pryke, C. Ruhl, J. E. Schaffer, K. K. Shaw, L. Shirokoff, E. Spieler, H. G. Stalder, B. Staniszewski, Z. Stark, A. A. Switzer, E. R. Vanderlinde, K. Vieira, J. D. Williamson, R. Zahn, O. TI ANGULAR POWER SPECTRA OF THE MILLIMETER-WAVELENGTH BACKGROUND LIGHT FROM DUSTY STAR-FORMING GALAXIES WITH THE SOUTH POLE TELESCOPE SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic background radiation; galaxies: abundances; large-scale structure of universe; submillimeter: diffuse background; submillimeter: galaxies ID MULTIBAND IMAGING PHOTOMETER; DEEP-FIELD-SOUTH; SOURCE COUNTS; SUBMILLIMETER GALAXIES; EXTRAGALACTIC SOURCES; ENERGY-DISTRIBUTIONS; RADIO-SOURCES; SPITZER; ANISOTROPIES; EMISSION AB We use data from the first 100 deg(2) field observed by the South Pole Telescope (SPT) in 2008 to measure the angular power spectrum of temperature anisotropies contributed by the background of dusty star-forming galaxies (DSFGs) at millimeter wavelengths. From the auto- and cross-correlation of 150 and 220 GHz SPT maps, we significantly detect both Poisson distributed and, for the first time at millimeter wavelengths, clustered components of power from a background of DSFGs. The spectral indices of the Poisson and clustered components are found to be (alpha) over bar alpha(P)(150-220) = 3.86 +/- 0.23 and alpha(C)(150-220) = 3.8 +/- 1.3, implying a steep scaling of the dust emissivity index beta similar to 2. The Poisson and clustered power detected in SPT, BLAST (at 600, 860, and 1200 GHz), and Spitzer (1900 GHz) data can be understood in the context of a simple model in which all galaxies have the same graybody spectrum with dust emissivity index of beta = 2 and dust temperature T-d = 34 K. In this model, half of the 150 GHz background light comes from redshifts greater than 3.2. We also use the SPT data to place an upper limit on the amplitude of the kinetic Sunyaev-Zel'dovich power spectrum at l = 3000 of 13 mu K-2 at 95% confidence. C1 [Hall, N. R.; Knox, L.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Keisler, R.; Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Crawford, T. M.; Crites, A. T.; Leitch, E. M.; McMahon, J. J.; Meyer, S. S.; Padin, S.; Pryke, C.; Schaffer, K. K.; Switzer, E. R.; Vieira, J. D.; Williamson, R.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Keisler, R.; Bleem, L. E.; Carlstrom, J. E.; Meyer, S. S.; Vieira, J. D.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. [Ade, P. A. R.] Cardiff Univ, Dept Phys & Astron, Cardiff CF24 3YB, S Glam, Wales. [Benson, B. A.; Carlstrom, J. E.; Chang, C. L.; McMahon, J. J.; Meyer, S. S.; Pryke, C.; Schaffer, K. K.; Switzer, E. R.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Carlstrom, J. E.; Crawford, T. M.; Crites, A. T.; Leitch, E. M.; Meyer, S. S.; Padin, S.; Pryke, C.; Williamson, R.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [De Haan, T.; Dobbs, M. A.; Holder, G. P.; Shaw, L.; Vanderlinde, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Halverson, N. W.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Halverson, N. W.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA. [Joy, M.] NASA, Marshall Space Flight Ctr, Dept Space Sci, Huntsville, AL 35812 USA. [Lee, A. T.; Spieler, H. G.] Univ Calif Berkeley, Lawrence Berkeley Lab, Div Phys, Berkeley, CA 94720 USA. [Mohr, J. J.] Univ Munich, Dept Phys, D-81679 Munich, Germany. [Mohr, J. J.] Excellence Cluster Univ, D-85748 Garching, Germany. [Mohr, J. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Montroy, T. E.; Ruhl, J. E.; Staniszewski, Z.] Case Western Reserve Univ, Dept Phys, Ctr Educ & Res Cosmol & Astrophys, Cleveland, OH 44106 USA. [Stalder, B.; Stark, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Zahn, O.] Univ Calif Berkeley, Dept Phys, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA. RP Hall, NR (reprint author), Univ Calif Davis, Dept Phys, 1 Shields Ave, Davis, CA 95616 USA. EM nrhall@ucdavis.edu RI Williamson, Ross/H-1734-2015; Holzapfel, William/I-4836-2015; OI Williamson, Ross/0000-0002-6945-2975; Aird, Kenneth/0000-0003-1441-9518; Reichardt, Christian/0000-0003-2226-9169 FU National Science Foundation (NSF) [ANT-0638937, ANT-0130612, PHY-0114422]; United States Antarctic Program; Raytheon Polar Services Company; Kavli Foundation; Gordon and Betty Moore Foundation; Office of Science of the U.S. Department of Energy [DE-AC02-05CH11231]; National Sciences and Engineering Research Council of Canada; Quebec Fonds de recherche sur la nature et les technologies; Canadian Institute for Advanced Research; Fermi Fellowship; GAAN Fellowship; Miller Institute for Basic Research in Science, University of California Berkeley; Alfred P. Sloan Research Fellowship; KICP Fellowships FX We thank Marco Viero and Guilaine Lagache for comparison of calculations as well as Andrew Blain, Douglas Scott, Rashid Sunyaev, Simon White, and George Efstathiou for useful conversations. The SPT team gratefully acknowledges the contributions to the design and construction of the telescope by S. Busetti, E. Chauvin, T. Hughes, P. Huntley, and E. Nichols and his team of ironworkers. We also thank the National Science Foundation (NSF) Office of Polar Programs, the United States Antarctic Program, and the Raytheon Polar Services Company for their support of the project. We are grateful for professional support from the staff of the South Pole station. We thank T. Lanting, J. Leong, A. Loehr, W. Lu, M. Runyan, D. Schwan, M. Sharp, and C. Greer for their early contributions to the SPT project, and J. Joseph and C. Vu for their contributions to the electronics.; The South Pole Telescope is supported by the National Science Foundation through grants ANT-0638937 and ANT-0130612. Partial support is also provided by the NSF Physics Frontier Center grant PHY-0114422 to the Kavli Institute of Cosmological Physics at the University of Chicago, the Kavli Foundation, and the Gordon and Betty Moore Foundation. This research used resources of the National Energy Research Scientific Computing Center, which is supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. The McGill group acknowledges funding from the National Sciences and Engineering Research Council of Canada, the Quebec Fonds de recherche sur la nature et les technologies, and the Canadian Institute for Advanced Research. The following individuals acknowledge additional support: J.J.M. from a Fermi Fellowship, Z.S. from a GAAN Fellowship, A.T.L. from the Miller Institute for Basic Research in Science, University of California Berkeley, N.W.H. from an Alfred P. Sloan Research Fellowship, and K.S., B.A.B., and E.R.S. from KICP Fellowships. NR 67 TC 92 Z9 92 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2010 VL 718 IS 2 BP 632 EP 646 DI 10.1088/0004-637X/718/2/632 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 626OV UT WOS:000279976200005 ER PT J AU Braatz, JA Reid, MJ Humphreys, EML Henkel, C Condon, JJ Lo, KY AF Braatz, J. A. Reid, M. J. Humphreys, E. M. L. Henkel, C. Condon, J. J. Lo, K. Y. TI THE MEGAMASER COSMOLOGY PROJECT. II. THE ANGULAR-DIAMETER DISTANCE TO UGC 3789 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; cosmology: observations; galaxies: distances and redshifts; galaxies: individual (UGC 3789); galaxies: nuclei; masers ID HUBBLE-SPACE-TELESCOPE; ACTIVE GALAXY NGC-4258; WATER MASER EMISSION; GEOMETRIC DISTANCE; SPIRAL STRUCTURE; DARK ENERGY; CONSTANT; SFI++; DISK AB The Megamaser Cosmology Project (MCP) aims to determine H(0) by measuring angular-diameter distances to galaxies in the Hubble flow using observations of water vapor megamasers in the circumnuclear accretion disks of active galaxies. The technique is based only on geometry and determines H(0) in one step, independent of standard candles and the extragalactic distance ladder. In Paper I, we presented a very long baseline interferometry map of the maser emission from the Seyfert 2 galaxy UGC 3789. The map reveals an edge-on, sub-parsec disk in Keplerian rotation, analogous to the megamaser disk in NGC 4258. Here, we present 3.2 years of monthly Green Bank Telescope observations of the megamaser disk in UGC 3789. We use these observations to measure the centripetal accelerations of both the systemic and high-velocity maser components. The measured accelerations suggest that maser emission lines near the systemic velocity originate on the front side of the accretion disk, primarily from segments of two narrow rings. Adopting a two-ring model for the systemic features, we determine the angular-diameter distance to UGC 3789 to be 49.9 +/- 7.0 Mpc. This is the most accurate geometric distance to a galaxy in the Hubble flow yet obtained. Based on this distance, we determine H(0) = 69 +/- 11 km s(-1) Mpc(-1). We also measure the mass of the central black hole to be 1.09 x 10(7) M(circle dot) +/- 14%. With additional observations, the uncertainty in the distance to this galaxy can be reduced to under 10%. Observations of megamaser disks in other galaxies will further reduce the uncertainty in H(0) as measured by the MCP. C1 [Braatz, J. A.; Condon, J. J.; Lo, K. Y.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Reid, M. J.; Humphreys, E. M. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Henkel, C.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. RP Braatz, JA (reprint author), Natl Radio Astron Observ, 520 Edgemont Rd, Charlottesville, VA 22903 USA. EM jbraatz@nrao.edu FU National Science Foundation FX We thank the referee for helpful comments, and we are grateful to the NRAO staff in Green Bank for their many contributions to this research program. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. NR 15 TC 31 Z9 31 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2010 VL 718 IS 2 BP 657 EP 665 DI 10.1088/0004-637X/718/2/657 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 626OV UT WOS:000279976200007 ER PT J AU Friesen, RK Di Francesco, J Myers, PC Belloche, A Shirley, YL Bourke, TL Andre, P AF Friesen, R. K. Di Francesco, J. Myers, P. C. Belloche, A. Shirley, Y. L. Bourke, T. L. Andre, P. TI THE INITIAL CONDITIONS OF CLUSTERED STAR FORMATION. III. THE DEUTERIUM FRACTIONATION OF THE OPHIUCHUS B2 CORE SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: kinematics and dynamics; ISM: molecules; ISM: structure; radio lines: ISM; stars: formation ID PRE-STELLAR CORES; DENSE INTERSTELLAR CLOUDS; C2D LEGACY CLOUDS; MOLECULAR CLOUDS; RHO-OPHIUCHI; PROTOSTELLAR CORES; PRESTELLAR CORES; MAIN CLOUD; DARK CLOUD; HYPERFINE-STRUCTURE AB We present N2D+ 3-2 (IRAM), and H2D+ 1(11)-1(10) and N2H+ 4-3 (JCMT) maps of the small cluster-forming Ophiuchus B2 core in the nearby Ophiuchus molecular cloud. In conjunction with previously published N2H+ 1-0 observations, the N2D+ data reveal the deuterium fractionation in the high-density gas across Oph B2. The average deuterium fractionation R-D = N(N2D+)/N(N2H+) similar to 0.03 over Oph B2, with several small scale R-D peaks and a maximum R-D = 0.1. The mean RD is consistent with previous results in isolated starless and protostellar cores. The column density distributions of both H2D+ and N2D+ show no correlation with total H-2 column density. We find, however, an anticorrelation in deuterium fractionation with proximity to the embedded protostars in Oph B2 to distances greater than or similar to 0.04 pc. Destruction mechanisms for deuterated molecules require gas temperatures greater than those previously determined through NH3 observations of Oph B2 to proceed. We present temperatures calculated for the dense core gas through the equating of non-thermal line widths for molecules (i.e., N2D+ and H2D+) expected to trace the same core regions, but the observed complex line structures in B2 preclude finding a reasonable result in many locations. This method may, however, work well in isolated cores with less complicated velocity structures. Finally, we use RD and the H2D+ column density across Oph B2 to set a lower limit on the ionization fraction across the core, finding a mean x(e,lim) greater than or similar to few x 10(-8). Our results show that care must be taken when using deuterated species as a probe of the physical conditions of dense gas in star-forming regions. C1 [Friesen, R. K.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Friesen, R. K.; Di Francesco, J.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8W 3P6, Canada. [Friesen, R. K.; Di Francesco, J.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Myers, P. C.; Bourke, T. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Belloche, A.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Bourke, T. L.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Andre, P.] Univ Paris Diderot, IRFU,Serv Astrophys, CE Saclay, Lab AIM,CEA,DSM,CNRS, F-91191 Gif Sur Yvette, France. RP Friesen, RK (reprint author), Natl Radio Astron Observ, 520 Edgemont Rd, Charlottesville, VA 22903 USA. EM rfriesen@nrao.edu FU University of Victoria; National Research Council Canada; National Science and Engineering Research Council of Canada; National Science Foundation [0708158] FX We thank the anonymous referee and E. Feigelson for comments, which improved the paper. We also thank H. Kirk for providing SCUBA maps of the observed regions and H. Weisemeyer for help with the IRAM observations. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. The James Clerk Maxwell Telescope is operated by the Joint Astronomy Centre on behalf of the Particle Physics and Astronomy Research Council of the United Kingdom, the Netherlands Association for Scientific Research, and the National Research Council of Canada. R. K. F. acknowledges financial support from the University of Victoria and the National Research Council Canada Graduate Student Scholarship Supplement Program. We also acknowledge the support of the National Science and Engineering Research Council of Canada. This research is supported in part by the National Science Foundation under grant number 0708158 (T.L.B.). NR 68 TC 20 Z9 20 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 AUG 1 PY 2010 VL 718 IS 2 BP 666 EP 682 DI 10.1088/0004-637X/718/2/666 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 626OV UT WOS:000279976200008 ER PT J AU Oberg, KIR van Dishoeck, EF Linnartz, H Andersson, S AF Oeberg, Karin I. R. van Dishoeck, Ewine F. Linnartz, Harold Andersson, Stefan TI THE EFFECT OF H2O ON ICE PHOTOCHEMISTRY SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; circumstellar matter; ISM: molecules; methods: laboratory; molecular data molecular processes ID YOUNG STELLAR OBJECTS; SPITZER SPECTROSCOPIC SURVEY; INTERSTELLAR ICES; GRAIN MANTLES; WATER-ICE; CO; MOLECULES; CHEMISTRY; MIXTURES; DESORPTION AB UV irradiation of simple ices is proposed to efficiently produce complex organic species during star formation and planet formation. Through a series of laboratory experiments, we investigate the effects of the H2O concentration, the dominant ice constituent in space, on the photochemistry of more volatile species, especially CH4, in ice mixtures. In the experiments, thin (similar to 40 ML) ice mixtures, kept at 20-60 K, are irradiated under ultrahigh vacuum conditions with a broadband UV hydrogen discharge lamp. Photodestruction cross sections of volatile species (CH4 and NH3) and production efficiencies of new species (C2H6, C2H4, CO, H2CO, CH3OH, CH3CHO, and CH3CH2OH) in water-containing ice mixtures are determined using reflection-absorption infrared spectroscopy during irradiation and during a subsequent slow warm-up. The four major effects of increasing the H2O concentration are: (1) an increase of the destruction efficiency of the volatile mixture constituent by up to an order of magnitude due to a reduction of back reactions following photodissociation, (2) a shift to products rich in oxygen, e.g., CH3OH and H2CO, (3) trapping of up to a factor of 5 more of the formed radicals in the ice, and (4) a disproportional increase in the diffusion barrier for the OH radical compared with the CH3 and HCO radicals. The radical diffusion temperature dependencies are consistent with calculated H2O-radical bond strengths. All the listed effects are potentially important for the production of complex organics in H2O-rich icy grain mantles around protostars and should thus be taken into account when modeling ice chemistry. C1 [Oeberg, Karin I. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Oeberg, Karin I. R.; Linnartz, Harold] Leiden Univ, Leiden Observ, Sackler Lab Astrophys, NL-2300 RA Leiden, Netherlands. [Andersson, Stefan] SINTEF Mat & Chem, NO-7465 Trondheim, Norway. [van Dishoeck, Ewine F.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Andersson, Stefan] Univ Gothenburg, Dept Chem, SE-41296 Gothenburg, Sweden. [Andersson, Stefan] Leiden Univ, Leiden Inst Chem, Gorlaeus Labs, NL-2300 RA Leiden, Netherlands. RP Oberg, KIR (reprint author), Harvard Smithsonian Ctr Astrophys, MS 42,60 Garden St, Cambridge, MA 02138 USA. FU NASA; Netherlands Organization for Scientific Research (NWO); NOVA FX This work has benefitted from discussions with Herma Cuppen and Robin Garrod. Support for K.I.O. is provided by NASA through Hubble Fellowship grant awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA. Astrochemistry in Leiden is supported by a SPINOZA grant of the Netherlands Organization for Scientific Research (NWO) and NOVA. The work by S.A. was partly funded by an NWO-CW Top grant. Some of the electronic structure calculations were performed at C3SE (Chalmers Centre for Computational Science and Engineering) computing resources. NR 44 TC 23 Z9 23 U1 2 U2 20 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2010 VL 718 IS 2 BP 832 EP 840 DI 10.1088/0004-637X/718/2/832 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 626OV UT WOS:000279976200020 ER PT J AU Sharon, K Gal-Yam, A Maoz, D Filippenko, AV Foley, RJ Silverman, JM Ebeling, H Ma, CJ Ofek, EO Kneib, JP Donahue, M Ellis, RS Freedman, WL Kirshner, RP Mulchaey, JS Sarajedini, VL Voit, GM AF Sharon, Keren Gal-Yam, Avishay Maoz, Dan Filippenko, Alexei V. Foley, Ryan J. Silverman, Jeffrey M. Ebeling, Harald Ma, Cheng-Jiun Ofek, Eran O. Kneib, Jean-Paul Donahue, Megan Ellis, Richard S. Freedman, Wendy L. Kirshner, Robert P. Mulchaey, John S. Sarajedini, Vicki L. Voit, G. Mark TI THE TYPE Ia SUPERNOVA RATE IN REDSHIFT 0.5-0.9 GALAXY CLUSTERS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: general; supernovae: general ID HUBBLE-SPACE-TELESCOPE; DIGITAL SKY SURVEY; GAMMA-RAY BURST; STAR-FORMATION HISTORY; TO-LIGHT RATIOS; HYDRODYNAMICAL SIMULATIONS; CHEMICAL ENRICHMENT; INTRACLUSTER MEDIUM; MAGNITUDE RELATION; MASS FUNCTIONS AB Supernova (SN) rates are potentially powerful diagnostics of metal enrichment and SN physics, particularly in galaxy clusters with their deep, metal-retaining potentials and relatively simple star formation histories. We have carried out a survey for SNe in galaxy clusters, at a redshift range of 0.5 < z < 0.9, using the Advanced Camera for Surveys (ACS) on the Hubble Space Telescope. We reimaged a sample of 15 clusters that were previously imaged by ACS, thus obtaining two to three epochs per cluster in which we discovered five likely cluster SNe, six possible cluster Type Ia supernovae, two hostless SN candidates, and several background and foreground events. Keck spectra of the host galaxies were obtained to establish cluster membership. We conducted detailed efficiency simulations, and measured the stellar luminosities of the clusters using Subaru images. We derive a cluster SN rate of 0.35SNu(B-0.12)(+0.17) (statistical) +/- 0.13(classification) +/- 0.01(systematic) (where SNu(B) = SNe (100 yr 10(10) L(B,circle dot))(-1)) and 0.112SNu(M-0.039)(+0.055)(statistical) +/- 0.042(classification) +/- 0.005(systematic) (where SNu(M) = SNe (100 yr 10(10) M(circle dot))(-1)). As in previous measurements of cluster SN rates, the uncertainties are dominated by small-number statistics. The SN rate in this redshift bin is consistent with the SN rate in clusters at lower redshifts (to within the uncertainties), and shows that there is, at most, only a slight increase of cluster SN rate with increasing redshift. The low and fairly constant SN Ia rate out to z approximate to 1 implies that the bulk of the iron mass in clusters was already in place by z approximate to 1. The recently observed doubling of iron abundances in the intracluster medium between z = 1 and 0, if real, is likely to be the result of redistribution of existing iron, rather than new production of iron. C1 [Sharon, Keren] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Sharon, Keren; Maoz, Dan] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Gal-Yam, Avishay] Weizmann Inst Sci, Fac Phys, Benoziyo Ctr Astrophys, IL-76100 Rehovot, Israel. [Filippenko, Alexei V.; Foley, Ryan J.; Silverman, Jeffrey M.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Foley, Ryan J.; Kirshner, Robert P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 01238 USA. [Ebeling, Harald; Ma, Cheng-Jiun] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Ofek, Eran O.; Ellis, Richard S.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Kneib, Jean-Paul] Univ Aix Marseille, CNRS, Lab Astrophys Marseille, F-13388 Marseille 13, France. [Donahue, Megan; Mulchaey, John S.; Voit, G. Mark] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Freedman, Wendy L.] Carnegie Observ, Pasadena, CA 91101 USA. [Sarajedini, Vicki L.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. RP Sharon, K (reprint author), Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. RI Donahue, Megan/B-5361-2012; Kneib, Jean-Paul/A-7919-2015; OI Kneib, Jean-Paul/0000-0002-4616-4989; Voit, Gerard/0000-0002-3514-0383 FU Ministry of Science, Culture Sport, Israel [07AST-F9]; Ministry of Research, France; Israeli Science Foundation; EU; Benoziyo Center for Astrophysics; Peter and Patricia Gruber Awards; Israel Science Foundation; National Science Foundation [AST-0607485, AST-0908886]; NASA/HST; NASA [NAS 5-26555]; Department of Energy [DE-FG02-08ER41563] FX We thank the anonymous referee for very useful comments that greatly improved the paper. We thank D. Poznanski and M. Sullivan for useful discussions and help with the Keck observations. K.S. acknowledges support from the Kersten Visiting Fellowship Fund, and thanks the Department of Astronomy and Astrophysics at the University of Chicago for their hospitality during the time some of this research was conducted. A.G. and J.P.K. acknowledge support by the grant 07AST-F9 from the Ministry of Science, Culture & Sport, Israel, & the Ministry of Research, France. A.G. is also supported by the Israeli Science Foundation, an EU Seventh Framework Programme Marie Curie IRG fellowship, and the Benoziyo Center for Astrophysics, a research grant from the Peter and Patricia Gruber Awards, and the William Z. and Eda Bess Novick New Scientists Fund at the Weizmann Institute. D.M. acknowledges support by the Israel Science Foundation. This research was supported by National Science Foundation grants AST-0607485 and AST-0908886 to A.V.F., as well as by NASA/HST grant GO-10793 from the Space Telescope Science Institute (STScI), which is operated by AURA, Inc., under NASA contract NAS 5-26555. A.V.F. is also grateful for the Department of Energy grant DE-FG02-08ER41563. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea (where the Subaru and Keck data were obtained) has always had within the indigenous Hawaiian community; we are most fortunate to have the opportunity to conduct observations from this mountain. NR 117 TC 24 Z9 26 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2010 VL 718 IS 2 BP 876 EP 893 DI 10.1088/0004-637X/718/2/876 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 626OV UT WOS:000279976200023 ER PT J AU Li, HB Houde, M Lai, SP Sridharan, TK AF Li, Hua-Bai Houde, Martin Lai, Shih-Ping Sridharan, T. K. TI TRACING TURBULENT AMBIPOLAR DIFFUSION IN MOLECULAR CLOUDS SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: clouds; ISM: kinematics and dynamics; ISM: magnetic fields; turbulence ID MAGNETIC-FIELD; STAR-FORMATION; ION SPECTRA; EMISSION; REGIONS; DUST AB Though flux freezing is a good approximation frequently assumed for molecular clouds, ambipolar diffusion (AD) is inevitable at certain scales. The scale at which AD sets in can be a crucial parameter for turbulence and the star formation process. However, both observation and simulation of AD are very challenging and our knowledge of it is very limited. We recently proposed that the difference between ion and neutral velocity spectra is a signature of turbulent AD and can be used to estimate the AD scales and magnetic field strengths. Here, we present observational evidence showing that this difference between the velocity dispersions from coexistent ions and neutrals is indeed correlated with magnetic field strength. C1 [Li, Hua-Bai] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Houde, Martin] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [Lai, Shih-Ping] Natl Tsing Hua Univ, Inst Astron, Hsinchu 30013, Taiwan. [Lai, Shih-Ping] Natl Tsing Hua Univ, Dept Phys, Hsinchu 30013, Taiwan. [Sridharan, T. K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Li, HB (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. EM li@mpia-hd.mpg.de FU Max-Planck-Institut fur Astronomie; Harvard-Smithsonian Center for Astrophysics; NSERC; Canada Research Chair; Canada Fund programs for Innovation; Ontario Innovation Trust; Western's Academic Development Fund programs; NSF [AST-0540882]; Smithsonian Institution; Academia Sinica FX H.L. appreciates the encouragement and valuable comments from Roger H. Hildebrand, Philip C. Myers, Eric R. Keto, and Qizhou Zhang on LH08. We appreciate the help from the SMA staff on observations and from Alice Argon on data analysis. The research of H.L. is supported by the postdoctoral fellowships from Max-Planck-Institut fur Astronomie and from Harvard-Smithsonian Center for Astrophysics. The research of M.H. is funded through the NSERC Discovery Grant, Canada Research Chair, Canada Fund programs for Innovation, Ontario Innovation Trust, and Western's Academic Development Fund programs. The Caltech Submillimeter Observatory is funded through the NSF grant AST-0540882. The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. NR 31 TC 13 Z9 13 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2010 VL 718 IS 2 BP 905 EP 912 DI 10.1088/0004-637X/718/2/905 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 626OV UT WOS:000279976200026 ER PT J AU Umana, G Buemi, CS Trigilio, C Leto, P Hora, JL AF Umana, G. Buemi, C. S. Trigilio, C. Leto, P. Hora, J. L. TI SPITZER, VERY LARGE TELESCOPE, AND VERY LARGE ARRAY OBSERVATIONS OF THE GALACTIC LUMINOUS BLUE VARIABLE CANDIDATE HD 168625 SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; infrared: stars; stars: early-type; stars: individual (HD 168625); stars: winds, outflows ID SN 2008S; PROTOPLANETARY NEBULAE; INFRARED-EMISSION; SPACE-TELESCOPE; MASSIVE STARS; DUSTY NEBULA; LBV NEBULAE; HD-168625; DISCOVERY; SPECTRUM AB We present mid-IR and radio observations of the Galactic luminous blue variables (LBVs) candidate HD 168625 and its associated nebula. We obtained mid-IR spectroscopic observations using the Infrared Spectrograph on board the Spitzer Space Telescope, and performed mid-IR and radio imaging observations using VISIR on the Very Large Telescope and the Very Large Array with comparable angular resolution. Our spectroscopic observations detected spectral features attributable to polycyclic aromatic hydrocarbons (PAHs) and therefore indicate the presence of a photodissociation region (PDR) around the ionized nebula. This result increases the number of LBVs and LBV candidates where a PDR has been found, confirming the importance of such a component in the total mass-loss budget of the central object during this elusive phase of massive star evolution. We have analyzed and compared the mid-IR and radio maps, and derive several results concerning the associated nebula. There is evidence for grain distribution variations across the nebula, with a predominant contribution from bigger grains in the northern part of the nebula while PAH and smaller grains are more concentrated in the southern part. A compact radio component located where there is a lack of thermal dust grains corroborates the presence of a shock in the southern nebula, which could arise as a consequence of the interaction of a fast outflow with the slower, expanding dusty nebula. Such a shock would be a viable means for PAH production as well as for changes in the grain size distribution. Finally, from the detection of a central radio component probably associated with the wind from the central massive supergiant, we derive a current mass-loss rate of. M = (1.46 +/- 0.15) x 10(-6) M(circle dot)yr(-1). C1 [Umana, G.; Buemi, C. S.; Trigilio, C.; Leto, P.] INAF, Osservatorio Astrofis Catania, I-95123 Catania, Italy. [Hora, J. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Umana, G (reprint author), INAF, Osservatorio Astrofis Catania, Via S Sofia 78, I-95123 Catania, Italy. OI Buemi, Carla Simona/0000-0002-7288-4613; Leto, Paolo/0000-0003-4864-2806; Hora, Joseph/0000-0002-5599-4650 FU ASI [I/016/07/0]; PRIN-INAF; NASA [1256790]; NASA through the Jet Propulsion Laboratory and Ames Research Center FX We thank an anonymous referee for the extremely helpful suggestions that improved the paper. We acknowledge partial financial support from the ASI contract I/016/07/0 "COFIS" and from PRIN-INAF 2007. 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 NASA contract 1407. Support for this work was provided by NASA through contract number 1256790 issued by JPL/Caltech. The IRS was a collaborative venture between Cornell University and Ball Aerospace Corporation funded by NASA through the Jet Propulsion Laboratory and Ames Research Center. This work is based also on observations made with the VISIR instrument on the ESO VLT telescope (program ID. 079.D-0748A). The Very Large Array is a facility of the National Radio Astronomy Observatory, which is operated by Associated Universities, Inc., under cooperative agreement with the National Science Foundation. SMART was developed at Cornell University and is available through the Spitzer Science Center at Caltech. NR 52 TC 17 Z9 17 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2010 VL 718 IS 2 BP 1036 EP 1045 DI 10.1088/0004-637X/718/2/1036 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 626OV UT WOS:000279976200039 ER PT J AU Rujopakarn, W Eisenstein, DJ Rieke, GH Papovich, C Cool, RJ Moustakas, J Jannuzi, BT Kochanek, CS Rieke, MJ Dey, A Eisenhardt, P Murray, SS Brown, MJI Le Floc'h, E AF Rujopakarn, Wiphu Eisenstein, Daniel J. Rieke, George H. Papovich, Casey Cool, Richard J. Moustakas, John Jannuzi, Buell T. Kochanek, Christopher S. Rieke, Marcia J. Dey, Arjun Eisenhardt, Peter Murray, Steve S. Brown, Michael J. I. Le Floc'h, Emeric TI THE EVOLUTION OF THE STAR FORMATION RATE OF GALAXIES AT 0.0 <= z <= 1.2 SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; galaxies: evolution; galaxies: high-redshift; infrared: galaxies ID ACTIVE GALACTIC NUCLEI; INFRARED LUMINOSITY FUNCTIONS; SPECTRAL ENERGY-DISTRIBUTION; DEEP-FIELD-SOUTH; MULTIBAND IMAGING PHOTOMETER; X-RAY SOURCES; FORMATION HISTORY; FORMING GALAXIES; SOURCE COUNTS; REDSHIFT SURVEY AB We present the 24 mu m rest-frame luminosity function (LF) of star-forming galaxies in the redshift range 0.0 <= z <= 0.6 constructed from 4047 spectroscopic redshifts from the AGN and Galaxy Evolution Survey of 24 mu m selected sources in the Bootes field of the NOAO Deep Wide-Field Survey. This sample provides the best available combination of large area (9 deg(2)), depth, and statistically complete spectroscopic observations, allowing us to probe the evolution of the 24 mu m LF of galaxies at low and intermediate redshifts while minimizing the effects of cosmic variance. In order to use the observed 24 mu m luminosity as a tracer for star formation, active galactic nuclei (AGNs) that could contribute significantly at 24 mu m are identified and excluded from our star-forming galaxy sample based on their mid-IR spectral energy distributions or the detection of X-ray emission. Optical emission line diagnostics are considered for AGN identification, but we find that 24 mu m emission from optically selected AGNs is usually from star-forming activity and therefore should not be excluded. The evolution of the 24 mu m LF of star-forming galaxies for redshifts of z <= 0.65 is consistent with a pure luminosity evolution where the characteristic 24 mu m luminosity evolves as (1 + z)(3.8 +/- 0.3). We extend our evolutionary study to encompass 0.0 <= z <= 1.2 by combining our data with that of the Far-Infrared Deep Extragalactic Legacy Survey. Over this entire redshift range, the evolution of the characteristic 24 mu m luminosity is described by a slightly shallower power law of (1 + z)(3.4 +/- 0.2). We find a local star formation rate density of (1.09 +/- 0.21) x 10(-2) M(circle dot) yr(-1) Mpc(-3), and that it evolves as (1 + z)(3.5 +/- 0.2) over 0.0 <= z <= 1.2. These estimates are in good agreement with the rates using optical and UV fluxes corrected for the effects of intrinsic extinction in the observed sources. This agreement confirms that star formation at z <= 1.2 is robustly traced by 24 mu m observations and that it largely occurs in obscured regions of galaxies. C1 [Rujopakarn, Wiphu; Eisenstein, Daniel J.; Rieke, George H.; Rieke, Marcia J.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Papovich, Casey] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA. [Cool, Richard J.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Moustakas, John] Univ Calif San Diego, Ctr Astrophys & Space Sci, San Diego, CA 92093 USA. [Jannuzi, Buell T.; Dey, Arjun] Natl Opt Astron Observ, Tucson, AZ 85726 USA. [Kochanek, Christopher S.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Kochanek, Christopher S.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Eisenhardt, Peter] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Murray, Steve S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Brown, Michael J. I.] Monash Univ, Sch Phys, Clayton, Vic 3800, Australia. [Le Floc'h, Emeric] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. RP Rujopakarn, W (reprint author), Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. EM wiphu@as.arizona.edu RI Rujopakarn, Wiphu/E-7849-2012; Brown, Michael/B-1181-2015; OI Brown, Michael/0000-0002-1207-9137; Rujopakarn, Wiphu/0000-0002-0303-499X FU JPL/Caltech [1255094]; Spitzer archival [JPL-1278815]; NSF [AST-0607541]; Thai Government FX We thank Benjamin Weiner, Benjamin Magnelli, Christopher Willmer, and Pablo Perez-Gonzalez for invaluable discussions. W. R. thanks Andrew Hopkins for supplying his rho* compilation and Xinyu Dai for his inputs on the cosmic variance in the Bootes field. This work was supported by the contract 1255094 from JPL/Caltech to the University of Arizona. W. R. was supported by Spitzer archival grant JPL-1278815, NSF AST-0607541, and the Thai Government Scholarship. NR 107 TC 42 Z9 42 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2010 VL 718 IS 2 BP 1171 EP 1185 DI 10.1088/0004-637X/718/2/1171 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 626OV UT WOS:000279976200050 ER PT J AU Kunert-Bajraszewska, M Janiuk, A Gawronski, MP Siemiginowska, A AF Kunert-Bajraszewska, Magdalena Janiuk, Agnieszka Gawronski, Marcin P. Siemiginowska, Aneta TI ORIGIN OF THE COMPLEX RADIO STRUCTURE IN BAL QSO 1045+352 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; quasars: absorption lines; quasars: individual (1045+352) ID BROAD-ABSORPTION-LINE; COMPACT STEEP-SPECTRUM; ACTIVE GALACTIC NUCLEI; DIGITAL SKY SURVEY; ACCRETION DISK; PARSEC-SCALE; OBSERVATIONAL EVIDENCE; INTERMITTENT ACTIVITY; INTRINSIC FRACTION; JET ACTIVITY AB We present new, more sensitive, high-resolution radio observations of a compact broad absorption line (BAL) quasar, 1045+352, made with the EVN+MERLIN at 5 GHz. These observations allowed us to trace the connection between the arcsecond structure and the radio core of the quasar. The radio morphology of 1045+352 is dominated by a knotty jet showing several bends. We discuss possible scenarios that could explain such a complex morphology: galaxy merger, accretion disk instability, precession of the jet, and jet-cloud interactions. It is possible that we are witnessing an ongoing jet precession in this source due to internal instabilities within the jet flow; however, a dense environment detected in the submillimeter band and an outflowing material suggested by the X-ray absorption could strongly interact with the jet. It is difficult to establish the orientation between the jet axis and the observer in 1045+352 because of the complex structure. Nevertheless, taking into account the most recent inner radio structure, we conclude that the radio jet is oriented close to the line of sight, which can mean that the opening angle of the accretion disk wind can be large in this source. We also suggest that there is no direct correlation between the jet-observer orientation and the possibility of observing BALs. C1 [Kunert-Bajraszewska, Magdalena; Gawronski, Marcin P.] Nicholas Copernicus Univ, Torun Ctr Astron, PL-87100 Torun, Poland. [Janiuk, Agnieszka] Nicholas Copernicus Astron Ctr, PL-00716 Warsaw, Poland. [Siemiginowska, Aneta] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kunert-Bajraszewska, M (reprint author), Nicholas Copernicus Univ, Torun Ctr Astron, Gagarina 11, PL-87100 Torun, Poland. RI Kunert-Bajraszewska, Magdalena/F-9060-2014; Gawronski, Marcin/H-6744-2014 FU national research councils; Polish Ministry of Science and Higher Education [N N203 303635] FX We thank Zsolt Paragi and Bob Campbell for their help with EVN data reduction. The European VLBI Network is a joint facility of European, Chinese, South African, and other radio astronomy institutes funded by their national research councils.; This work was supported by the Polish Ministry of Science and Higher Education under grant N N203 303635. NR 54 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 J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2010 VL 718 IS 2 BP 1345 EP 1352 DI 10.1088/0004-637X/718/2/1345 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 626OV UT WOS:000279976200062 ER PT J AU Irwin, J Buchhave, L Berta, ZK Charbonneau, D Latham, DW Burke, CJ Esquerdo, GA Everett, ME Holman, MJ Nutzman, P Berlind, P Calkins, ML Falco, EE Winn, JN Johnson, JA Gazak, JZ AF Irwin, Jonathan Buchhave, Lars Berta, Zachory K. Charbonneau, David Latham, David W. Burke, Christopher J. Esquerdo, Gilbert A. Everett, Mark E. Holman, Matthew J. Nutzman, Philip Berlind, Perry Calkins, Michael L. Falco, Emilio E. Winn, Joshua N. Johnson, John A. Gazak, J. Zachary TI NLTT 41135: A FIELD M DWARF plus BROWN DWARF ECLIPSING BINARY IN A TRIPLE SYSTEM, DISCOVERED BY THE MEARTH OBSERVATORY SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: eclipsing; brown dwarfs; stars: individual (NLTT 41135); stars: low-mass ID LOW-MASS STARS; TRANSIT LIGHT-CURVE; DIGITAL SKY SURVEY; LIMB-DARKENING COEFFICIENTS; EXTRASOLAR GIANT PLANETS; SOLAR-TYPE STARS; EVOLUTIONARY MODELS; ACCURATE MASSES; DYNAMICAL MASS; MAGNETIC ACTIVITY AB We report the discovery of an eclipsing companion to NLTT 41135, a nearby M5 dwarf that was already known to have a wider, slightly more massive common proper motion companion, NLTT 41136, at 2 ''.4 separation. Analysis of combined-light and RV curves of the system indicates that NLTT 41135B is a (31-34) +/- 3M(Jup) brown dwarf (where the range depends on the unknown metallicity of the host star) on a circular orbit. The visual M dwarf pair appears to be physically bound, so the system forms a hierarchical triple, with masses approximately in the ratio 8:6:1. The eclipses are grazing, preventing an unambiguous measurement of the secondary radius, but follow-up observations of the secondary eclipse (e.g., with the James Webb Space Telescope) could permit measurements of the surface brightness ratio between the two objects, and thus place constraints on models of brown dwarfs. C1 [Irwin, Jonathan; Buchhave, Lars; Berta, Zachory K.; Charbonneau, David; Latham, David W.; Burke, Christopher J.; Esquerdo, Gilbert A.; Everett, Mark E.; Holman, Matthew J.; Nutzman, Philip] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Berlind, Perry; Calkins, Michael L.; Falco, Emilio E.] Smithsonian Astrophys Observ, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Winn, Joshua N.] MIT, Dept Phys, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Johnson, John A.; Gazak, J. Zachary] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. RP Irwin, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jirwin@cfa.harvard.edu OI Buchhave, Lars A./0000-0003-1605-5666; Charbonneau, David/0000-0002-9003-484X FU David and Lucile Packard Fellowship for Science and Engineering; National Science Foundation [AST-0807690]; NASA Kepler mission [NCC2-1390]; NSF [AST-0702821]; NASA; U.S. Government [NAG W-2166]; Alfred P. Sloan Foundation; U.S. Department of Energy; National Aeronautics and Space Administration; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England; American Museum of Natural History; Astrophysical Institute Potsdam; University of Basel; University of Cambridge; Case Western Reserve University; University of Chicago; Drexel University; Fermilab; Institute for Advanced Study; Japan Participation Group; Johns Hopkins University; Joint Institute for Nuclear Astrophysics; Kavli Institute for Particle Astrophysics and Cosmology; Korean Scientist Group; Chinese Academy of Sciences (LAMOST); Los Alamos National Laboratory; Max-Planck-Institute for Astronomy (MPIA); Max-Planck-Institute for Astrophysics (MPA); New Mexico State University; Ohio State University; University of Pittsburgh; University of Portsmouth; Princeton University; United States Naval Observatory; University of Washington FX The MEarth team gratefully acknowledges funding from the David and Lucile Packard Fellowship for Science and Engineering (awarded to DC). This material is based upon work supported by the National Science Foundation under grant number AST-0807690. L.B. and D.W.L. acknowledge partial support from the NASA Kepler mission under cooperative agreement NCC2-1390. J.A.J. thanks the NSF Astronomy and Astrophysics Postdoctoral Fellowship program for support in the years leading to the completion of this work, and acknowledges support from NSF grant AST-0702821. We thank Isabelle Baraffe for providing NextGen and COND models in the z band, Daniel Fabrycky for helpful discussions regarding dynamics, and Timothy Brown and the rest of the team at the Las Cumbres Observatory Global Telescope for their efforts in trying to obtain a resolved light curve of the system. The MEarth team is greatly indebted to the staff at the Fred Lawrence Whipple Observatory for their efforts in construction and maintenance of the facility, and would like to explicitly thank Wayne Peters, Ted Groner, Karen Erdman-Myres, Grace Alegria, Rodger Harris, Bob Hutchins, Dave Martina, Dennis Jankovsky, and Tom Welsh for their support. Finally, we thank the referee for a thorough and helpful report, which has substantially improved the manuscript.; This research is 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. This research has made extensive use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by NASA and the NSF, NASA's Astrophysics Data System (ADS), and the SIMBAD database, operated at CDS, Strasbourg, France. The Digitized Sky Surveys were produced at the Space Telescope Science Institute under U.S. Government grant NAG W-2166. The images of these surveys are based on photographic data obtained using the Oschin Schmidt Telescope on Palomar Mountain and the UK Schmidt Telescope. The plates were processed into the present compressed digital form with the permission of these institutions.; Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web Site is http://www.sdss.org/. The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington. NR 72 TC 23 Z9 23 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2010 VL 718 IS 2 BP 1353 EP 1366 DI 10.1088/0004-637X/718/2/1353 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 626OV UT WOS:000279976200063 ER PT J AU Gou, LJ McClintock, JE Steiner, JF Narayan, R Cantrell, AG Bailyn, CD Orosz, JA AF Gou, Lijun McClintock, Jeffrey E. Steiner, James F. Narayan, Ramesh Cantrell, Andrew G. Bailyn, Charles D. Orosz, Jerome A. TI THE SPIN OF THE BLACK HOLE IN THE SOFT X-RAY TRANSIENT A0620-00 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE accretion, accretion disks; black hole physics; stars: individual (A0620-00); X-rays: binaries ID ACCRETION DISK MODELS; INTERSTELLAR-MEDIUM; LMC X-1; BINARIES; CONTINUUM; MASS; INCLINATION; STATE; RADIATION; OUTBURST AB During its year-long outburst in 1975-76, the transient source A0620-00 reached an intensity of 50 Crab, an all-time record for any X-ray binary. The source has been quiescent since then. We have recently determined accurate values for the black hole (BH) mass, orbital inclination angle, and distance. Building on these results, we have measured the radius of the inner edge of the accretion disk around the BH primary by fitting its thermal continuum spectrum to our version of the relativistic Novikov-Thorne thin-disk model. We have thereby estimated the spin of the BH. Although our spin estimate depends on a single high-quality spectrum, which was obtained in 1975 by OSO-8, we are confident of our result because of the consistent values of the inner-disk radius that we have obtained for hundreds of observations of other sources: H1743-322, XTE J1550-564, and notably LMCX-3. We have determined the dimensionless spin parameter of the BH to be a(*) = 0.12 +/- 0.19, with a(*) < 0.49 and a(*) > -0.59 at the 3 sigma level of confidence. This result takes into account all sources of observational and model-parameter uncertainties. Despite the low spin, the intensity and properties of the radio counterpart, both in outburst and quiescence, attest to the presence of a strong jet. If jets are driven by BH spin, then current models indicate that jet power should be a steeply increasing function of a(*). Consequently, the low spin of A0620-00 suggests that its jet may be disk driven. C1 [Gou, Lijun; McClintock, Jeffrey E.; Steiner, James F.; Narayan, Ramesh] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Cantrell, Andrew G.; Bailyn, Charles D.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Orosz, Jerome A.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. RP Gou, LJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Narayan, Ramesh/0000-0002-1919-2730 FU NASA [NNX08AJ55G, NNX08AH32G]; Smithsonian Endowment Funds; NSF [AST-0805832] FX J.E.M. acknowledges support from NASA grant NNX08AJ55G and the Smithsonian Endowment Funds. R.N. was supported in part by NSF grant AST-0805832 and NASA grant NNX08AH32G. We thank the following individuals for help in locating and utilizing the OSO-8 X-ray spectrum: L. Angelini, G. Branduardi-Raymont, K. Pounds, J. Swank, and N. White. We thank J. McKinney, S. Murray, and an anonymous referee for helpful comments. This research has made exclusive use of data obtained from the High Energy Astrophysics Science Archive Research Center (HEASARC) at NASA/Goddard Space Flight Center. NR 46 TC 44 Z9 44 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD AUG 1 PY 2010 VL 718 IS 2 BP L122 EP L126 DI 10.1088/2041-8205/718/2/L122 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 636EI UT WOS:000280710700016 ER PT J AU Shi, H Zhao, JH Han, JL AF Shi, Hui Zhao, Jun-Hui Han, J. L. TI A BIPOLAR OUTFLOW FROM THE MASSIVE PROTOSTELLAR CORE W51e2-E SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE ISM: individual objects (W51e2); ISM: jets and outflows; stars: formation ID STAR-FORMATION; RADIO-CONTINUUM; W51; COLLAPSE; REGION AB We present high-resolution images of the bipolar outflow from W51e2, which are produced from the Submillimeter Array archival data observed for CO(3-2) and HCN(4-3) lines with angular resolutions of 0 ''.8 x 0 ''.6 and 0 ''.3 x 0 ''.2, respectively. The images show that the powerful outflow originates from the protostellar core W51e2-E rather than from the ultracompact H II region W51e2-W. The kinematic timescale of the outflow from W51e2-E is about 1000 yr, younger than the age (similar to 5000 yr) of the ultracompact H II region W51e2-W. A large mass-loss rate of similar to 1 x 10(-3) M(circle dot) yr(-1) and a high mechanical power of 120 L(circle dot) are inferred, suggesting that an O star or a cluster of B stars are forming in W51e2-E. The observed outflow activity along with the inferred large accretion rate indicates that at present W51e2-E is in a rapid phase of star formation. C1 [Shi, Hui; Han, J. L.] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. [Zhao, Jun-Hui] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Shi, H (reprint author), Chinese Acad Sci, Natl Astron Observ, 20A DaTun Rd, Beijing 100012, Peoples R China. EM shihui@nao.cas.cn; jzhao@cfa.harvard.edu; hil@nao.cas.cn FU National Natural Science Foundation (NNSF) of China [10773016, 10821061, 10833003]; National Key Basic Research Science Foundation of China [2007CB815403] FX We thank Prof. Ed Churchwell and the referee for helpful comments. H.S. and J.L.H. are supported by the National Natural Science Foundation (NNSF) of China (10773016, 10821061, and 10833003) and the National Key Basic Research Science Foundation of China (2007CB815403). NR 18 TC 13 Z9 13 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD AUG 1 PY 2010 VL 718 IS 2 BP L181 EP L184 DI 10.1088/2041-8205/718/2/L181 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 636EI UT WOS:000280710700028 ER PT J AU Steiner, JF McClintock, JE Remillard, RA Gou, LJ Yamada, S Narayan, R AF Steiner, James F. McClintock, Jeffrey E. Remillard, Ronald A. Gou, Lijun Yamada, Shin'ya Narayan, Ramesh TI THE CONSTANT INNER-DISK RADIUS OF LMC X-3: A BASIS FOR MEASURING BLACK HOLE SPIN SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE accretion, accretion disks; black hole physics; stars: individual (LMC X-3); X-rays: binaries ID X-RAY CONTINUUM; ACCRETION DISK; BINARIES; STATE; REFLECTION; DISCOVERY; MODEL; CALIBRATION; EMISSION; SPECTRUM AB The black hole binary system LMC X-3 has been observed by virtually every X-ray mission since the inception of X-ray astronomy. Among the persistent sources, LMC X-3 is uniquely both habitually soft and highly variable. Using a fully relativistic accretion disk model, we analyze hundreds of spectra collected during eight X-ray missions that span 26 years. For a selected sample of 391 RXTE spectra, we find that to within approximate to 2% the inner radius of the accretion disk is constant over time and unaffected by source variability. Even considering an ensemble of eight X-ray missions, we find consistent values of the radius to within approximate to 4%-6%. Our results provide strong evidence for the existence of a fixed inner-disk radius. The only reasonable inference is that this radius is closely associated with the general relativistic innermost stable circular orbit. Our findings establish a firm foundation for the measurement of black hole spin. C1 [Steiner, James F.; McClintock, Jeffrey E.; Gou, Lijun; Narayan, Ramesh] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Remillard, Ronald A.] MIT, MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Yamada, Shin'ya] Univ Tokyo, Dept Phys, Bunkyo Ku, Tokyo 1130033, Japan. RP Steiner, JF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jsteiner@cfa.harvard.edu OI Narayan, Ramesh/0000-0002-1919-2730 FU Smithsonian Institution; NASA [NNX08AJ55G, NNX08AH32G]; NSF [AST-0805832] FX 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. We thank Shane Davis and Laura Brenneman for their insightful analyses of the manuscript and suggestions. J.F.S. thanks Tim Oosterbroek for assisting with BeppoSAX LECS, and Ignacio de la Calle for advice on XMM. The authors thank Tomaso Belloni and Ken Ebisawa for contributing reduced archival data from EXOSAT, and Ginga and ASCA, respectively. J.F.S. was supported by the Smithsonian Institution Endowment Funds, and J.E.M. acknowledges support from NASA grant NNX08AJ55G. R.N. acknowledges support from NASA grant NNX08AH32G and NSF grant AST-0805832. NR 49 TC 72 Z9 73 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 AUG 1 PY 2010 VL 718 IS 2 BP L117 EP L121 DI 10.1088/2041-8205/718/2/L117 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 636EI UT WOS:000280710700015 ER PT J AU Vandenbroucke, J Buehler, R Ajello, M Bechtol, K Bellini, A Bolte, M Cheung, CC Civano, F Donato, D Fuhrmann, L Funk, S Healey, SE Hill, AB Knigge, C Madejski, GM Romani, RW Santander-Garcia, M Shaw, MS Steeghs, D Torres, MAP Van Etten, A Williams, KA AF Vandenbroucke, J. Buehler, R. Ajello, M. Bechtol, K. Bellini, A. Bolte, M. Cheung, C. C. Civano, F. Donato, D. Fuhrmann, L. Funk, S. Healey, S. E. Hill, A. B. Knigge, C. Madejski, G. M. Romani, R. W. Santander-Garcia, M. Shaw, M. S. Steeghs, D. Torres, M. A. P. Van Etten, A. Williams, K. A. TI DISCOVERY OF A GeV BLAZAR SHINING THROUGH THE GALACTIC PLANE SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: active ID LARGE-AREA TELESCOPE; VARIABLE RADIO-SOURCES; NORTHERN MILKY-WAY; GAMMA-RAY EMISSION; GHZ SOURCES; SKY SURVEY; CATALOG; SPECTRA; PATROL AB The Fermi Large Area Telescope (LAT) discovered a new gamma-ray source near the Galactic plane, Fermi J0109+6134, when it flared brightly in 2010 February. The low Galactic latitude (b = -1 degrees.2) indicated that the source could be located within the Galaxy, which motivated rapid multi-wavelength follow-up including radio, optical, and X-ray observations. We report the results of analyzing all 19 months of LAT data for the source, and of X-ray observations with both Swift and the Chandra X-ray Observatory. We determined the source redshift, z = 0.783, using a Keck Low-Resolution Imaging Spectrometer observation. Finally, we compiled a broadband spectral energy distribution (SED) from both historical and new observations contemporaneous with the 2010 February flare. The redshift, SED, optical line width, X-ray absorption, and multi-band variability indicate that this new GeV source is a blazar seen through the Galactic plane. Because several of the optical emission lines have equivalent width > 5 angstrom, this blazar belongs in the flat-spectrum radio quasar category. C1 [Vandenbroucke, J.; Buehler, R.; Ajello, M.; Bechtol, K.; Funk, S.; Healey, S. E.; Madejski, G. M.; Romani, R. W.; Shaw, M. S.; Van Etten, A.] Stanford Univ, Dept Phys, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol,Dept Phys, Stanford, CA 94305 USA. [Vandenbroucke, J.; Buehler, R.; Ajello, M.; Bechtol, K.; Funk, S.; Healey, S. E.; Madejski, G. M.; Romani, R. W.; Shaw, M. S.; Van Etten, A.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Bellini, A.] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy. [Bellini, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Bolte, M.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA. [Bolte, M.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Cheung, C. C.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. [Cheung, C. C.] Natl Acad Sci, Natl Res Council Res Associate, Washington, DC 20001 USA. [Civano, F.; Torres, M. A. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Donato, D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Fuhrmann, L.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Hill, A. B.] Univ Grenoble 1, CNRS, LAOG, UMR 5571, F-38041 Grenoble 09, France. [Knigge, C.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Santander-Garcia, M.] Inst Astrofis Canarias, E-38205 San Cristobal la Laguna, Tenerife, Spain. [Santander-Garcia, M.] Isaac Newton Grp Telescopes, E-38700 Sta Cruz De La Palms, Spain. [Santander-Garcia, M.] Univ La Laguna, Dept Astrofis, E-38205 Tenerife, Spain. [Steeghs, D.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Williams, K. A.] Univ Texas Austin, Dept Astron, Austin, TX 75712 USA. RP Vandenbroucke, J (reprint author), Stanford Univ, Dept Phys, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol,Dept Phys, Stanford, CA 94305 USA. EM justinv@stanford.edu; buehler@stanford.edu RI Steeghs, Danny/C-5468-2009; Funk, Stefan/B-7629-2015; OI Steeghs, Danny/0000-0003-0771-4746; Funk, Stefan/0000-0002-2012-0080; Hill, Adam/0000-0003-3470-4834; Williams, Kurtis/0000-0002-1413-7679 FU Kavli Foundation; INAF in Italy; CNES in France; NASA in the United States; DOE in the United States; CEA/Irfu in France; IN2P3/CNRS in France; ASI in Italy; INFN in Italy; MEXT in Japan; KEK in Japan; JAXA in Japan; K.A. Wallenberg Foundation, Sweden; Swedish Research Council, Sweden; National Space Board in Sweden FX We thank the Chandra and Swift teams for timely and high-quality X-ray observations. We are grateful for valuable comments on the manuscript from Berrie Giebels. J.V. is supported by a Kavli Fellowship from the Kavli Foundation. The Fermi LAT Collaboration acknowledges support from a number of agencies and institutes for both the development and the operation of the LAT as well as scientific data analysis. These include NASA and DOE in the United States, CEA/Irfu and IN2P3/CNRS in France, ASI and INFN in Italy, MEXT, KEK, and JAXA in Japan, and the K.A. Wallenberg Foundation, the Swedish Research Council, and the National Space Board in Sweden. Additional support from INAF in Italy and CNES in France for science analysis during the operations phase is also gratefully acknowledged. NR 40 TC 12 Z9 12 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD AUG 1 PY 2010 VL 718 IS 2 BP L166 EP L170 DI 10.1088/2041-8205/718/2/L166 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 636EI UT WOS:000280710700025 ER PT J AU Winn, JN Fabrycky, D Albrecht, S Johnson, JA AF Winn, Joshua N. Fabrycky, Daniel Albrecht, Simon Johnson, John Asher TI HOT STARS WITH HOT JUPITERS HAVE HIGH OBLIQUITIES SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE planetary systems; planets and satellites: formation; planet-star interactions; stars: rotation ID SPIN-ORBIT ALIGNMENT; EXOPLANETARY SYSTEM; SPECTROSCOPIC TRANSIT; PLANETARY SYSTEM; RETROGRADE ORBIT; HD 147506B; EVOLUTION; DISCOVERY; COMPANION; PROGRADE AB We show that stars with transiting planets for which the stellar obliquity is large are preferentially hot (T(eff) > 6250 K). This could explain why small obliquities were observed in the earliest measurements, which focused on relatively cool stars drawn from Doppler surveys, as opposed to hotter stars that emerged more recently from transit surveys. The observed trend could be due to differences in planet formation and migration around stars of varying mass. Alternatively, we speculate that hot-Jupiter systems begin with a wide range of obliquities, but the photospheres of cool stars realign with the orbits due to tidal dissipation in their convective zones, while hot stars cannot realign because of their thinner convective zones. This in turn would suggest that hot Jupiters originate from few-body gravitational dynamics and that disk migration plays at most a supporting role. C1 [Winn, Joshua N.; Albrecht, Simon] MIT, Dept Phys, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Fabrycky, Daniel] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Johnson, John Asher] CALTECH, Dept Astrophys, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA. RP Winn, JN (reprint author), MIT, Dept Phys, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. OI Fabrycky, Daniel/0000-0003-3750-0183 FU NASA [NNX09AD36G]; MIT; Tinsley Scholars program; National Aeronautics and Space Administration FX We thank Jeremy Goodman, Matija Cuk, Bill Cochran, Sally Dodson-Robinson, Andrew Howard, Geoff Marcy, Tim Morton, Fred Rasio, Dimitar Sasselov, and Richard Wade for helpful discussions. J.N.W. gratefully acknowledges support from the NASA Origins program through award NNX09AD36G and the MIT Class of 1942, as well as the Tinsley Scholars program and the hospitality of the Astronomy Department at the University of Texas, Austin. D.F. acknowledges support from the Michelson Fellowship, supported by the National Aeronautics and Space Administration and administered by the Michelson Science Center. S. Albrecht acknowledges support from an NWO Rubicon fellowship. NR 48 TC 284 Z9 284 U1 0 U2 10 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD AUG 1 PY 2010 VL 718 IS 2 BP L145 EP L149 DI 10.1088/2041-8205/718/2/L145 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 636EI UT WOS:000280710700021 ER PT J AU Gottlieb, CA McCarthy, MC Thaddeus, P AF Gottlieb, C. A. McCarthy, M. C. Thaddeus, P. TI VIBRATIONALLY EXCITED C6H SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE ISM: molecules; line: identification; molecular data; molecular processes; radio lines: ISM ID MOLECULAR LINE SURVEY; HYPERFINE-STRUCTURE; LASER SPECTROSCOPY; CARBON CHAINS; AB-INITIO; IRC+10216; RADICALS; SPECTRA; STATES; ENVELOPE AB Rotational spectra of the linear carbon chain radical C6H in two low-lying excited vibrational states were observed both at millimeter wavelengths in a low-pressure glow discharge and at centimeter wavelengths in a supersonic molecular beam. Two series of harmonically related lines with rotational constants within 0.3% of the (2)Pi ground state were assigned to the (2)Sigma and (2)Delta vibronic components of an excited bending vibrational level. Measurements of the intensities of the lines in the glow discharge indicate that the (2)Sigma component lies very close to ground, but the (2)Delta component is much higher in energy. The standard Hamiltonian for an isolated (2)Delta state with five spectroscopic constants reproduces the observed rotational spectrum, but several high-order distortion terms in the spin-rotation interaction are needed to reproduce the spectrum of the 2S component in C6H and C6D. The derived spectroscopic constants allow astronomers to calculate the rotational spectra of the (2)Sigma and (2)Delta states up to 260 GHz to within 0.1 km s(-1) or better in equivalent radial velocity. C1 [Gottlieb, C. A.; McCarthy, M. C.; Thaddeus, P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gottlieb, C. A.; McCarthy, M. C.; Thaddeus, P.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. RP Gottlieb, CA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI McCarthy, Michael/0000-0001-9142-0008 FU NSF [CHE-0701204]; NASA [NNX08AE05G] FX The authors thank H. S. P. Muller for helpful discussions during the course of this work. This work was supported in part by NSF grant CHE-0701204 and NASA grant NNX08AE05G. NR 35 TC 7 Z9 7 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD AUG PY 2010 VL 189 IS 2 BP 261 EP 269 DI 10.1088/0067-0049/189/2/261 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 642HO UT WOS:000281199800002 ER PT J AU Gutermuth, RA Megeath, ST Myers, PC Allen, LE Pipher, JL Fazio, GG AF Gutermuth, R. A. Megeath, S. T. Myers, P. C. Allen, L. E. Pipher, J. L. Fazio, G. G. TI A SPITZER SURVEY OF YOUNG STELLAR CLUSTERS WITHIN ONE KILOPARSEC OF THE SUN: CLUSTER CORE EXTRACTION AND BASIC STRUCTURAL ANALYSIS (vol 184, pg 18, 2009) SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Correction C1 [Gutermuth, R. A.; Myers, P. C.; Allen, L. E.; Fazio, G. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Megeath, S. T.] Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA. [Pipher, J. L.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. RP Gutermuth, RA (reprint author), Smith Coll, Northampton, MA 01063 USA. NR 1 TC 7 Z9 7 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD AUG PY 2010 VL 189 IS 2 BP 352 EP 352 DI 10.1088/0067-0049/189/2/352 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 642HO UT WOS:000281199800008 ER PT J AU Reynolds, KC Watanabe, H Strong, EE Sasaki, T Uematsu, K Miyake, H Kojima, S Suzuki, Y Fujikura, K Kim, S Young, CM AF Reynolds, Kyle C. Watanabe, Hiromi Strong, Ellen E. Sasaki, Takenor Uematsu, Katsuyuki Miyake, Hiroshi Kojima, Shigeaki Suzuki, Yohey Fujikura, Katsunori Kim, Stacy Young, Craig M. TI New Molluscan Larval Form: Brooding and Development in a Hydrothermal Vent Gastropod, Ifremeria nautilei (Provannidae) SO BIOLOGICAL BULLETIN LA English DT Article ID COLD SEEPS; CAENOGASTROPODA; REPRODUCTION AB Despite extreme differences between some shallow and deep-sea habitats. the developmental modes and larval forms of deep-sea animals are typically similar to those of their shallow-water relatives. Here we report one of the first documented exceptions to this general rule. The hydrothermal vent snail Ifremeria nautilei displays two novel life-history traits: (1) an unusual uniformly ciliated larva that we here name Waren's larva, and (2) internal brood protection in a modified metapodial pedal gland. Waren's larva emerges from the internal brood pouch as a fully ciliated lecithotrophic larva with a unique external cuticle. The larvae swim with their posterior end forward and metamorphose into typical veliger larvae after 15 days at room temperature. Waren's larva is the only known example of a free-swimming pre-veliger larval stage in the higher gastropods and is the first new gastropod larval form to be described in more than 100 years. C1 [Reynolds, Kyle C.; Kim, Stacy] Moss Landing Marine Labs, Moss Landing, CA 95039 USA. [Watanabe, Hiromi; Fujikura, Katsunori] Japan Agcy Marine Earth Sci & Technol, Yokosuka, Kanagawa 2370061, Japan. [Strong, Ellen E.] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20013 USA. [Sasaki, Takenor] Univ Tokyo, Univ Museum, Bunkyo Ku, Tokyo 1130033, Japan. [Uematsu, Katsuyuki] Marine Works Japan LTD, Yokosuka, Kanagawa 2370061, Japan. [Miyake, Hiroshi] Kitasato Univ, Sch Marine Biosci, Ofunato, Iwate 0220101, Japan. [Kojima, Shigeaki] Univ Tokyo, Ocean Res Inst, Nakano Ku, Tokyo 1648639, Japan. [Young, Craig M.] Univ Oregon, Oregon Inst Marine Biol, Charleston, OR 97420 USA. RP Reynolds, KC (reprint author), Moss Landing Marine Labs, 8272 Moss Landing Rd, Moss Landing, CA 95039 USA. EM kreynolds@mlml.calstate.edu RI Suzuki, Yohey/G-4980-2014 FU National Science Foundation [OCE-0241250, OCE-0527139]; JSPS; KAKENHI [18405006]; ChEss/Fondation Total; Dr. Earl H. Myers and Ethel M. Myers Oceanographic and Marine Biology Trust; David and Lucille Packard Foundation FX We are grateful to Anders Waren for bringing the brood pouch to our attention, for providing SEM images of some of the larvae, and for loaning samples from his own collection. We thank Paul Tyler for histological expertise and help with sample processing; OIMB and the Smithsonian Institution for SEM work; and Paul Greenhall, Marilyn Schotte, Gabriela Vega, Kamille Hammerstrom, Svetlana Maslakova, and Maya Wolf for assistance with handling specimens. The work was supported by National Science Foundation (Grants # OCE-0241250 and OCE-0527139), JSPS Research Fellowships for Young Scientists, KAKENHI (18405006), and grants from the ChEss/Fondation Total, Dr. Earl H. Myers and Ethel M. Myers Oceanographic and Marine Biology Trust, and the David and Lucille Packard Foundation. NR 24 TC 5 Z9 5 U1 2 U2 5 PU MARINE BIOLOGICAL LABORATORY PI WOODS HOLE PA 7 MBL ST, WOODS HOLE, MA 02543 USA SN 0006-3185 J9 BIOL BULL-US JI Biol. Bull. PD AUG PY 2010 VL 219 IS 1 BP 7 EP 11 PG 5 WC Biology; Marine & Freshwater Biology SC Life Sciences & Biomedicine - Other Topics; Marine & Freshwater Biology GA 648IF UT WOS:000281685300002 PM 20813984 ER PT J AU Mcdonald, KA Vaughn, D AF Mcdonald, Kathryn A. Vaughn, Dawn TI Abrupt Change in Food Environment Induces Cloning in Plutei of Dendraster excentricus SO BIOLOGICAL BULLETIN LA English DT Article ID ECHINODERM LARVAE; DEVELOPMENTAL PLASTICITY; MORPHOLOGICAL PLASTICITY; ASEXUAL REPRODUCTION; PHYTOPLANKTON BLOOMS; THIN-LAYERS; PLANKTON; GROWTH; RATES; ECHINOPLUTEI AB Asexual reproduction, or cloning, of planktonic echinoderm larvae has been observed in the laboratory and in nature, but little is known about its ecology. Here we examine the effects of algal food density and of a change in food density on the incidence of cloning in larvae of the sand dollar Dendraster excentricus. Results indicate that a change in food concentration can induce cloning in plutei. Cultures transferred from a low to a high algal ration at the time when primary larvae were developing the third (posterodorsal) pair of larval arms showed decreased postoral arm length, unusual morphologies, and increased larval density in culture. These dense cultures of smaller plutei were produced within 48 h of the food pulse. The result is consistent with the occurrence of a burst of cloning, possibly through anterior autotomization. A second feeding experiment demonstrated that anterior autotomization does occur in 4- to 6-arm plutei. Rather than constituting a developmental rarity, cloning may happen early and often in D. excentricus cohorts when environmental conditions favor rapid growth. C1 [Mcdonald, Kathryn A.; Vaughn, Dawn] Univ Washington, Dept Biol, Seattle, WA 98195 USA. [Mcdonald, Kathryn A.; Vaughn, Dawn] Univ Washington, Friday Harbor Labs, Friday Harbor, WA 98250 USA. RP Mcdonald, KA (reprint author), Smithsonian Trop Res Inst, MRC 0580-08,Unit 9100 Box 0948 DPO AA, Miami, FL 34002 USA. EM mcdonaldk2@si.edu FU Friday Harbor-ARCS Fellowship; NSF [OCE-0217304, OCE-0623102] FX We are grateful to R. R. Strathmann and R. Collin for their helpful comments on earlier drafts, and to two anonymous reviewers whose substantive comments greatly improved this manuscript. Our warm thanks to R. R. Strathmann, E. Dusek, and T. Clay for advice and discussion during these studies. This work was supported by a Friday Harbor-ARCS Fellowship (K. McDonald), NSF grant OCE-0217304 to R. R. Strathmann (K. McDonald), and NSF grant OCE-0623102 to R. R. Strathmann (D. Vaughn). NR 37 TC 5 Z9 5 U1 2 U2 15 PU MARINE BIOLOGICAL LABORATORY PI WOODS HOLE PA 7 MBL ST, WOODS HOLE, MA 02543 USA SN 0006-3185 J9 BIOL BULL-US JI Biol. Bull. PD AUG PY 2010 VL 219 IS 1 BP 38 EP 49 PG 12 WC Biology; Marine & Freshwater Biology SC Life Sciences & Biomedicine - Other Topics; Marine & Freshwater Biology GA 648IF UT WOS:000281685300006 PM 20813988 ER PT J AU Douglass, JK Wcislo, WT AF Douglass, John K. Wcislo, William T. TI An inexpensive and portable microvolumeter for rapid evaluation of biological samples SO BIOTECHNIQUES LA English DT Article DE allometry; body size; density; invertebrate; insect; microvolumetry; scaling; stereology; volume; zooplankton ID BRAIN ALLOMETRY; GROWTH; VOLUME; SIZE AB We describe an improved microvolumeter (MVM) for rapidly measuring volumes of small biological samples, including live zooplankton, embryos, and small animals and organs. Portability and low cost make this instrument suitable for widespread use, including at remote field sites. Beginning with Archimedes' principle, which states that immersing an arbitrarily shaped sample in a fluid-filled container displaces an equivalent volume, we identified procedures that maximize measurement accuracy and repeatability across a broad range of absolute volumes. Crucial steps include matching the overall configuration to the size of the sample, using reflected light to monitor fluid levels precisely, and accounting for evaporation during measurements. The resulting precision is at least 100 times higher than in previous displacement-based methods. Volumes are obtained much faster than by traditional histological or confocal methods and without shrinkage artifacts due to fixation or dehydration. Calibrations using volume standards confirmed accurate measurements of volumes as small as 0.06 mu L. We validated the feasibility of evaluating soft-tissue samples by comparing volumes of freshly dissected ant brains measured with the MVM and by confocal reconstruction. C1 [Douglass, John K.; Wcislo, William T.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Douglass, JK (reprint author), Smithsonian Trop Res Inst, Apartado Postal 0843-03092, Balboa, Ancon, Panama. EM douglassj@si.edu FU F.H. Levinson Fund; STRI FX We thank Annette Aiello, John Christy, Bill Eberhard, Jeremy Niven, Marc Seid, Willie Tobin, Mary Jane West-Eberhard, and Donald Windsor for discussions and anonymous reviewers for helpful comments that improved the manuscript. John Christy also shared workshop space and tools. Willie Tobin performed many of the larger volume measurements and helped fabricate sample receptacles and analyze initial data. Atta colombica were from a laboratory colony at the Smithsonian Tropical Research Institute (STRI). This work was supported by a grant from the F.H. Levinson Fund to the Laboratory of Behavior & Evolutionary Neurobiology at STRI (W.T.W., PI) and by STRI. NR 22 TC 2 Z9 2 U1 1 U2 3 PU BIOTECHNIQUES OFFICE PI NEW YORK PA 52 VANDERBILT AVE, NEW YORK, NY 10017 USA SN 0736-6205 J9 BIOTECHNIQUES JI Biotechniques PD AUG PY 2010 VL 49 IS 2 BP 566 EP 572 DI 10.2144/000113464 PG 7 WC Biochemical Research Methods; Biochemistry & Molecular Biology SC Biochemistry & Molecular Biology GA 726JZ UT WOS:000287719000013 PM 20701591 ER PT J AU Kaspari, M Stevenson, BS Shik, J Kerekes, JF AF Kaspari, Michael Stevenson, Bradley S. Shik, Jonathan Kerekes, Jennifer F. TI Scaling community structure: how bacteria, fungi, and ant taxocenes differentiate along a tropical forest floor SO ECOLOGY LA English DT Article DE ants; bacteria; biogeochemistry; diversity; fungi; niche; species composition ID LIFE-HISTORY; COPY NUMBER; FOOD WEBS; SOIL; DIVERSITY; SIZE; BIODIVERSITY; ECOLOGY; STOICHIOMETRY; DECOMPOSITION AB Taxa with smaller individuals tend to have shorter generation times and higher local abundance and diversity. The scaled specialization hypothesis (SSH) posits that taxocenes of smaller individuals should differentiate more rapidly and thoroughly along physiochemical gradients of a given age and extent. In a Panama rainforest, we evaluated how bacteria, fungi, and ants responded to two such gradients: one topographic and the other arising from nine years of NPK fertilization. Terminal restriction fragment length polymorphism (T-RFLP) delineated bacteria and fungi operational taxonomic units (OTUs); traditional taxonomy delineated the ants. Bacteria had higher local species richness than fungi and ants (averaging 48 vs. 30 vs. 6 OTUs in <0.25 m(2)). Bacteria OTUs were also more widely distributed (17% of OTUs were found on >= 50% of sample plots compared to 3% for fungi and ants). Consistent with SSH, bacterial composition differed across short-term (+N and +P) and long-term (topographic) gradients; fungal taxocenes differed only along the long-term gradient; and ant taxocenes were homogenous across both. Body size can help predict community responses to a changing environment. C1 [Kaspari, Michael; Shik, Jonathan] Univ Oklahoma, Dept Zool, Grad Program EEB, Norman, OK 73019 USA. [Kaspari, Michael] Smithsonian Trop Res Inst, Balboa, Panama. [Stevenson, Bradley S.] Univ Oklahoma, Dept Bot & Microbiol, Grad Program EEB, Norman, OK 73019 USA. [Kerekes, Jennifer F.] Univ Calif Berkeley, Dept Plant & Microbial Biol, Berkeley, CA 94720 USA. RP Kaspari, M (reprint author), Univ Oklahoma, Dept Zool, Grad Program EEB, Norman, OK 73019 USA. EM mkaspari@ou.edu RI Stevenson, Bradley/A-2786-2011; OI Stevenson, Bradley/0000-0001-9432-9744; Kaspari, Michael/0000-0002-9717-5768 FU National Geographic grant; University of Oklahoma; STRI FX This paper is dedicated to Michael Rosenzweig, who taught us the importance of scaling to biodiversity science. Oris Acevedo, Eldridge Bermingham, Allen Herre, and Joe Wright have provided continued support for our work at STRI. Christian Mulder and three anonymous reviewers greatly improved the manuscript. This work was funded by a National Geographic grant to M. Kaspari and start-up funding from the University of Oklahoma for B. S. Stevenson. NR 52 TC 7 Z9 8 U1 3 U2 33 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0012-9658 EI 1939-9170 J9 ECOLOGY JI Ecology PD AUG PY 2010 VL 91 IS 8 BP 2221 EP 2226 DI 10.1890/09-2089.1 PG 6 WC Ecology SC Environmental Sciences & Ecology GA 628WA UT WOS:000280153500005 PM 20836443 ER PT J AU Greenberg, R Olsen, B AF Greenberg, Russell Olsen, Brian TI Bill size and dimorphism in tidal-marsh sparrows: island-like processes in a continental habitat SO ECOLOGY LA English DT Article DE dominance hypothesis; ecological divergence; Emberizidae; niche variation; salt marsh birds ID SEXUAL-DIMORPHISM; MORPHOLOGICAL VARIATION; CHARACTER DISPLACEMENT; BIRDS; EVOLUTION; PATERNITY; LIZARDS; LENGTH; TIT AB Conditions favoring population divergence in trophic features, such as the low levels of species richness and interspecific competition found on islands, can be similar to conditions that increase their sexual dimorphism or overall variance. Male emberizid sparrows of tidal marshes have undergone parallel evolution of large bills. We tested for parallel increases between dimorphism and overall variation in bill size by comparing three groups totaling 30 sparrow subspecies: tidal-marsh sparrows, nontidal relatives of tidal-marsh taxa, and representative sparrow taxa. Bill size (and not other features) showed the following patterns in tidal-marsh sparrows compared to nontidal relatives or sparrows at large: (1) an increase; (2) a greater increase in males than females; (3) an increase in sexual dimorphism; and (4) greater variation in females. A high degree of sexual dimorphism in bill size is consistent with the hypothesis that low levels of interspecific and high levels of intraspecific competition select for intraspecific niche divergence. Alternatively, increased sexual selection in tidal-marsh sparrows, vis-a-vis high densities and hence increased male-male competition, may account for the differentially large increase in bill size in males. Relaxed natural selection due to high ecosystem productivity and low interspecific competition may explain why, in tidal-marsh sparrows, female bills have diverged less than males and show higher levels of variability at larger sizes. Both the niche divergence and sexual selection hypotheses depend upon processes, particularly increases in population density, that are similar to those often reported for island passerines. However, the low species diversity and increased intraspecific competition of salt marsh faunas is probably a result of abiotic constraints on colonization (tides and salinity) rather than the isolating distances of island biotas. Thus, both a shift in bill size and increases in its dimorphism and variability may be favored by high productivity and abiotic constraints. C1 [Greenberg, Russell] Smithsonian Migratory Bird Ctr, Natl Zool Pk, Washington, DC 20008 USA. [Olsen, Brian] Univ Maine, Sch Biol & Ecol, Orono, ME 04469 USA. RP Greenberg, R (reprint author), Smithsonian Migratory Bird Ctr, Natl Zool Pk, Washington, DC 20008 USA. EM greenbergr@si.edu OI Olsen, Brian/0000-0001-5608-2779 FU AirTran FX We thank the curatorial staff of the following museums for access to and loans of sparrow specimens: National Museum of Natural History, Dickey Collection of the University of California at Los Angeles, Los Angeles County Museum of Natural History, Museum of Vertebrate Zoology (MVZ), Philadelphia Academy of Natural Sciences, Delaware Museum of Natural History, Canadian Museum of Nature, Bell Museum of Natural Science (University of Minnesota), and the Royal Ontario Museum. We also thank the ORNIS network for providing easy online access to specimen catalogs for these collections. Y. Chan, D. Gill, J. C. Nordby, and the Point Reyes Bird Observatory provided unpublished mass data. We thank the Delaware Division of Fish and Wildlife, the Nature Conservancy, and H. Ternent for access to field locations. Animal handling in the field was approved under the Institutional Animal Care and Use Committee of the Smithsonian National Zoological Park permit number 04-10 and U.S. Federal Banding Permit number 22665. R. Sivinski assisted with statistical analysis. Y. Chan, D. Gill, C. Nordberg, and G. Shriver provided unpublished data. B. Ballentine, S. Clegg, D. Luther, J. Walters, R. Danner, and two anonymous reviewers provided valuable comments on earlier drafts. AirTran provided transportation to the MVZ through tickets donated to the National Zoological Park. NR 43 TC 18 Z9 18 U1 2 U2 25 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 AUG PY 2010 VL 91 IS 8 BP 2428 EP 2436 DI 10.1890/09-1136.1 PG 9 WC Ecology SC Environmental Sciences & Ecology GA 628WA UT WOS:000280153500026 PM 20836464 ER PT J AU Larjavaara, M Muller-Landau, HC AF Larjavaara, Markku Muller-Landau, Helene C. TI Rethinking the value of high wood density SO FUNCTIONAL ECOLOGY LA English DT Article DE bark; construction cost; decay resistance; maintenance cost; trunk respiration; strength; xylem implosion ID TROPICAL TREES; FOREST; STEM; RESPIRATION; STORAGE; DAMAGE AB P>1. Current thinking holds that wood density mediates a tradeoff between strength and economy of construction, with higher wood density providing higher strength but at higher cost. 2. Yet the further away wood fibres are from the central axis of the trunk, the more they increase the strength of the trunk; thus, a fat trunk of low-density wood can achieve greater strength at lower construction cost than a thin trunk of high-density wood. 3. What then are the countervailing advantages of high wood density? 4. We hypothesize that high wood density is associated with lower maintenance costs due to lower trunk surface area, as surface area correlates with maintenance respiration. 5. This advantage would be particularly important to long-lived trees and could in part explain why they tend to have high wood density. 6. High wood density has also been associated with lower risk of trunk breakage, xylem implosion and pathogen invasion, but we argue that these relationships are not causal and instead reflect correlated selection on other traits of value to long-lived trees. 7. This revaluation of the costs and benefits of high wood density has important implications for understanding tree life-history evolution, functional diversity, forest carbon stocks and the impacts of global change. C1 [Larjavaara, Markku; Muller-Landau, Helene C.] Smithsonian Trop Res Inst, CTFS Global Forest Carbon Res Initiat, Balboa, Panama. RP Larjavaara, M (reprint author), Smithsonian Trop Res Inst, CTFS Global Forest Carbon Res Initiat, Balboa, Panama. EM larjavaaram@si.edu OI Larjavaara, Markku/0000-0002-3484-889X FU HSBC FX We thank Dan Bebber, Michiel van Breugel, Petri Karenlampi, anonymous reviewers and especially David A. King for helpful comments. We gratefully acknowledge the financial support of the HSBC Climate Partnership. NR 26 TC 65 Z9 66 U1 2 U2 41 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0269-8463 J9 FUNCT ECOL JI Funct. Ecol. PD AUG PY 2010 VL 24 IS 4 BP 701 EP 705 DI 10.1111/j.1365-2435.2010.01698.x PG 5 WC Ecology SC Environmental Sciences & Ecology GA 624RL UT WOS:000279837700001 ER PT J AU Campbell, BA Carter, LM Campbell, DB Nolan, M Chandler, J Ghent, RR Hawke, BR Anderson, RF Wells, K AF Campbell, Bruce A. Carter, Lynn M. Campbell, Donald B. Nolan, Michael Chandler, John Ghent, Rebecca R. Hawke, B. Ray Anderson, Ross F. Wells, Kassandra TI Earth-based 12.6-cm wavelength radar mapping of the Moon: New views of impact melt distribution and mare physical properties SO ICARUS LA English DT Article DE Moon; Volcanism; Impact processes ID 70-CM WAVELENGTH; LUNAR; DEPOSITS; CRATER; REFLECTIVITY; GEOLOGY; EJECTA; FLOWS; BASIN; ICE AB We present results of a campaign to map much of the Moon's near side using the 12.6-cm radar transmitter at Arecibo Observatory and receivers at the Green Bank Telescope. These data have a single-look spatial resolution of about 40 m, with final maps averaged to an 80-m, four-look product to reduce image speckle. Focused processing is used to obtain this high spatial resolution over the entire region illuminated by the Arecibo beam. The transmitted signal is circularly polarized, and we receive reflections in both senses of circular polarization; measurements of receiver thermal noise during periods with no lunar echoes allow well-calibrated estimates of the circular polarization ratio (CPR) and the four-element Stokes vector. Radiometric calibration to values of the backscatter coefficient is ongoing. Radar backscatter data for the Moon provide information on regolith dielectric and physical properties, with particular sensitivity to ilmenite content and surface or buried rocks with diameter of about one-tenth the radar wavelength and larger. Average 12.6-cm circular polarization ratio (CPR) values for low- to moderate-TiO(2) mare basalt deposits are similar to those of rough terrestrial lava flows. We attribute these high values to abundant few-centimeter diameter rocks from small impacts and a significant component of subsurface volume scattering. An outflow deposit, inferred to be impact melt, from Glushko crater has CPR values near unity at 12.6-cm and 70-cm wavelengths and thus a very rugged near-surface structure at the decimeter to meter scale. This deposit does not show radar-brightness variations consistent with levees or channels, and appears to nearly overtop a massif, suggesting very rapid emplacement. Deposits of similar morphology and/or radar brightness are noted for craters such as Pythagoras, Rutherfurd, Theophilus, and Aristillus. Images of the north pole show that, despite recording the deposition of Orientale material, Byrd and Peary craters do not have dense patterns of radar-bright ejecta from small craters on their floors. Such patterns in Amundsen crater, near the south pole, were interpreted as diagnostic of abundant impact melt, so the fraction of Orientale-derived melt in the north polar smooth plains, 1000 km farther from the basin center, is inferred to be much lower. Published by Elsevier Inc. C1 [Campbell, Bruce A.; Carter, Lynn M.; Anderson, Ross F.] Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. [Campbell, Donald B.; Wells, Kassandra] Cornell Univ, Natl Astron & Ionosphere Ctr, Ithaca, NY 14853 USA. [Nolan, Michael] Arecibo Observ, Arecibo, PR 00612 USA. [Chandler, John] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Ghent, Rebecca R.] Univ Toronto, Dept Geol, Toronto, ON, Canada. [Hawke, B. Ray] Univ Hawaii, HIGP, Honolulu, HI 96822 USA. RP Campbell, BA (reprint author), Smithsonian Inst, Ctr Earth & Planetary Studies, MRC 315,POB 37012, Washington, DC 20013 USA. EM campbellb@si.edu RI Carter, Lynn/D-2937-2012; Nolan, Michael/H-4980-2012 OI Nolan, Michael/0000-0001-8316-0680 FU NASA FX We thank the staff at Arecibo Observatory and the Green Bank Telescope for their tremendous efforts in support of our radar mapping. The Arecibo Observatory is part of the National Astronomy and Ionosphere Center, which is operated by Cornell University under a cooperative agreement with the National Science Foundation (NSF). The Green Bank Telescope is part of the National Radio Astronomy Observatory, a facility of the NSF operated under cooperative agreement by Associated Universities, Inc. The lunar radar mapping is supported by a grant to B.A.C. from the NASA Planetary Astronomy Program. The comments of two anonymous reviewers helped to improve the manuscript. NR 38 TC 36 Z9 36 U1 1 U2 9 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD AUG PY 2010 VL 208 IS 2 BP 565 EP 573 DI 10.1016/j.icarus.2010.03.011 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 629GJ UT WOS:000280183000006 ER PT J AU Dunn, TL Mccoy, TJ Sunshine, JM McSween, HY AF Dunn, Tasha L. McCoy, Timothy J. Sunshine, J. M. McSween, Harry Y., Jr. TI A coordinated spectral, mineralogical, and compositional study of ordinary chondrites SO ICARUS LA English DT Article DE Asteroids; Spectroscopy; Meteorites ID REFLECTANCE SPECTROSCOPY; CHEMICAL-ANALYSES; NEAR-EARTH; METEORITES; OLIVINE; ASTEROIDS; IRRADIATION; PYROXENE; ITOKAWA AB Mineral compositions and abundances derived from visible/near-infrared (VIS/NIR or VNIR) spectra are used to classify asteroids, identify meteorite parent bodies, and understand the structure of the asteroid belt. Using a suite of 48 equilibrated (types 4-6) ordinary (H, L, and LL) chondrites containing orthopyroxene, clinopyroxene, and olivine, new relationships between spectra and mineralogy have been established. Contrary to previous suggestions, no meaningful correlation is observed between band parameters and cpx/(opx + cpx) ratios. We derive new calibrations for determining mineral abundances (ol/(ol + px)) and mafic silicate compositions (Fa in olivine, Fs in pyroxene) from VIS/NIR spectra. These calibrations confirm that band area ratio (BAR) is controlled by mineral abundances, while Band I center is controlled by mafic silicate compositions. Spectrally-derived mineralogical parameters correctly classify H, L and LL chondrites in 80% of cases, suggesting that these are robust relationships that can be applied to S(IV) asteroids with ordinary chondrites mineralogies. Comparison of asteroids and meteorites using these new mineralogical parameters has the advantage that H, L and LL chemical groups were originally defined on the basis of mafic silicate compositions. (C) 2010 Elsevier Inc. All rights reserved. C1 [Dunn, Tasha L.] Illinois State Univ, Dept Geog Geol, Normal, IL 61761 USA. [Dunn, Tasha L.; McSween, Harry Y., Jr.] Univ Tennessee, Planetary Geosci Inst, Dept Earth & Planetary Sci, Knoxville, TN 37902 USA. [McCoy, Timothy J.] Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20013 USA. [Sunshine, J. M.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Dunn, TL (reprint author), Illinois State Univ, Dept Geog Geol, Normal, IL 61761 USA. EM tldunn@ilstu.edu FU NASA [NNG06GG36G, NNX06AH69G] FX We would like to thank Gordon Cressey, at the Natural History Museum in London, for his assistance in the collection and interpretation of XRD modal data, and Takahiro Hiroi, at Brown University's Keck/NASA Reflectance Experiment Laboratory (RELAB), for collecting VNIR spectra of several samples examined in this study. Thanks also to the Smithsonian Institution and the Natural History Museum for providing powder samples for modal and spectral analysis. We would also like to thank Tom Burbine and Vishnu Reddy for their helpful reviews, which greatly improved this manuscript. This work was supported by NASA through cosmochemistry Grant NNG06GG36G to H.Y.M. and planetary geology and geophysics Grant NNX06AH69G to J.M.S. NR 41 TC 33 Z9 34 U1 0 U2 8 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD AUG PY 2010 VL 208 IS 2 BP 789 EP 797 DI 10.1016/j.icarus.2010.02.016 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 629GJ UT WOS:000280183000022 ER PT J AU Madden, AA Davis, MM Starks, PT AF Madden, A. A. Davis, M. M. Starks, P. T. TI First detailed report of brood parasitoidism in the invasive population of the paper wasp Polistes dominulus (Hymenoptera, Vespidae) in North America SO INSECTES SOCIAUX LA English DT Article DE Chalcoela iphitalis; Enemy release hypothesis; Parasitic moths; Invasion biology; Pyralidae ID GENUS; NEST AB The European paper wasp Polistes dominulus (Christ) is a model system in the fields of behavioral ecology, ecological immunology, and invasion biology. Since its introduction to the US in 1978, its invasion success has been attributed, in part, to a lack of parasites or parasitoids infecting this population. This is despite the number of parasites which infest the native population and the generalist polistine parasites and parasitoids documented in sympatric North American species. Multiple studies have cited low parasite pressure as evidence that the invasive population of P. dominulus is benefiting from a post-invasion release from enemies. Here, we present the first well documented case of parasitoidism of the invasive population of P. dominulus in North America. C1 [Madden, A. A.; Starks, P. T.] Tufts Univ, Dept Biol, Dana Lab, Medford, MA 02155 USA. [Davis, M. M.] Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Madden, AA (reprint author), Tufts Univ, Dept Biol, Dana Lab, Rm 120, Medford, MA 02155 USA. EM madden.anne@gmail.com; Philip.Starks@Tufts.edu FU Tufts University; USA National Science Foundation-REU FX This research was supported by a Tufts Institute of the Environment Fellowship from Tufts University to A. A. M. and a USA National Science Foundation-REU site award to Tufts University (DBI-0649190). The authors would like to thank Codman Farms for allowing for the collection of their nests; J. Soriano for his assistance with observations; M. A. Metz (USDA) for his assistance in identifying C. iphitalis; and two anonymous reviewers for valuable comments on an earlier version of this manuscript. The recent data capture efforts of J. A. Lewis facilitated in the relocation of specimens in alcohol. NR 25 TC 6 Z9 7 U1 0 U2 7 PU SPRINGER BASEL AG PI BASEL PA PICASSOPLATZ 4, BASEL, 4052, SWITZERLAND SN 0020-1812 J9 INSECT SOC JI Insect. Soc. PD AUG PY 2010 VL 57 IS 3 BP 257 EP 260 DI 10.1007/s00040-010-0079-0 PG 4 WC Entomology SC Entomology GA 611QJ UT WOS:000278834900002 ER PT J AU Perez-Ortega, B Fernandez-Marin, H Loiacono, MS Galgani, P Wcislo, WT AF Perez-Ortega, B. Fernandez-Marin, H. Loiacono, M. S. Galgani, P. Wcislo, W. T. TI Biological notes on a fungus-growing ant, Trachymyrmex cf. zeteki (Hymenoptera, Formicidae, Attini) attacked by a diverse community of parasitoid wasps (Hymenoptera, Diapriidae) SO INSECTES SOCIAUX LA English DT Article DE Diapriinae; Fungus-growing ants; Parasitoid wasps; Adaptive radiations; Trachymyrmex ID EVOLUTION; DEFENSE; REDUCE; BEE AB A number of wasps in the family Diapriidae, subfamily Diapriinae (Proctotrupoidea), are parasitoids that specialize on ant larvae. These wasps are abundant and diverse in the Neotropics, but little is known about their biology. We studied parasitism rates by an array of diapriine wasps that attack the larvae of fungus-growing ants, Trachymyrmex cf. zeteki, in a single population (near Gamboa, Panama). Relatively little is known about the biology and natural history of these ants, so we also present data on colony size and nest architecture. We excavated 136 colonies in central Panama from June to September 2006, and 20 nests from July 2009. We reared six wasp morphotypes; two of them in the genus Mimopriella Masner and Garcia, one Oxypria Kieffer, two Szelenyiopria Fabritius and one Acanthopria Ashmead. The mean intensity of larval parasitism per ant colony was 33.9% (2006), and its prevalence across all ant populations was 27.2% (2006 and 2009). Parasitism rates were not positively correlated with host colony size. A single case of super-parasitism was documented in which two Oxypria males were reared from the same host larva. C1 [Perez-Ortega, B.; Fernandez-Marin, H.; Galgani, P.; Wcislo, W. T.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Loiacono, M. S.] Univ Nacl La Plata, Div Entomol, Museo La Plata, Buenos Aires, DF, Argentina. RP Fernandez-Marin, H (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama. EM hermogenes_f@hotmail.com; WcisloW@si.edu FU Office of Academic Programs; Smithsonian Institution; Secretaria Nacional de Ciencia, Tecnologia e Innovacion, Panama; STRI FX We are grateful to Adam Smith, Simon Tierney and two anonymous reviewers for help with comments on the manuscript; to the Autoridad Nacional del Ambiente de la Republica de Panama for research, collecting, and export permits; and to the rest of the staff of the Smithsonian Tropical Research Institute (STRI) for logistical support. BPO received financial support from the Internship Program of the Office of Academic Programs at STRI; HFM was supported by a Post-doctoral Fellowship from the Smithsonian Institution, and a Postdoctoral fellowship from the Secretaria Nacional de Ciencia, Tecnologia e Innovacion, Panama. We gratefully acknowledge additional funding from the F.H. Levinson Fund, and general research funds from STRI to WTW. NR 21 TC 6 Z9 6 U1 0 U2 3 PU SPRINGER BASEL AG PI BASEL PA PICASSOPLATZ 4, BASEL, 4052, SWITZERLAND SN 0020-1812 EI 1420-9098 J9 INSECT SOC JI Insect. Soc. PD AUG PY 2010 VL 57 IS 3 BP 317 EP 322 DI 10.1007/s00040-010-0086-1 PG 6 WC Entomology SC Entomology GA 611QJ UT WOS:000278834900009 ER PT J AU Berke, SK AF Berke, Sarah K. TI Functional Groups of Ecosystem Engineers: A Proposed Classification with Comments on Current Issues SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Article ID KEYSTONE-SPECIES CONCEPT; ARENICOLA-MARINA; COMMUNITY STRUCTURE; LARVAL SETTLEMENT; LUGWORM EXCLUSION; BOUNDARY-LAYERS; GRAY WHALE; DISTURBANCE; ORGANISMS; WATER AB Ecologists have long known that certain organisms fundamentally modify, create, or define habitats by altering the habitat's physical properties. In the past 15 years, these processes have been formally defined as "ecosystem engineering", reflecting a growing consensus that environmental structuring by organisms represents a fundamental class of ecological interactions occurring in most, if not all, ecosystems. Yet, the precise definition and scope of ecosystem engineering remains debated, as one should expect given the complexity, enormity, and variability of ecological systems. Here I briefly comment on a few specific current points of contention in the ecosystem engineering concept. I then suggest that ecosystem engineering can be profitably subdivided into four narrower functional categories reflecting four broad mechanisms by which ecosystem engineering occurs: structural engineers, bioturbators, chemical engineers, and light engineers. Finally, I suggest some conceptual model frameworks that could apply broadly within these functional groups. C1 [Berke, Sarah K.] Univ Chicago, Dept Geophys Sci, Chicago, IL 60637 USA. [Berke, Sarah K.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Berke, SK (reprint author), Univ Chicago, Dept Geophys Sci, 5734 S Ellis Ave, Chicago, IL 60637 USA. EM skberke@gmail.com FU National Science Foundation [IOS-0938257, EAR-0922156]; Society for Integrative and Comparative Biology (Division of Ecology and Evolution and the Division of Invertebrate Zoology); American Microscopical Society; Smithsonian Environmental Research Center Marine Science Network Fellowship FX National Science Foundation (IOS-0938257); the Society for Integrative and Comparative Biology (Division of Ecology and Evolution and the Division of Invertebrate Zoology); American Microscopical Society; Smithsonian Environmental Research Center Marine Science Network Fellowship (to S.K.B. while organizing the symposium); National Science Foundation (EAR-0922156 to D. Jablonski, supported S.K.B. while writing). NR 80 TC 29 Z9 29 U1 2 U2 46 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD AUG PY 2010 VL 50 IS 2 BP 147 EP 157 DI 10.1093/icb/icq077 PG 11 WC Zoology SC Zoology GA 630NJ UT WOS:000280279800001 PM 21558195 ER PT J AU Breitburg, DL Crump, BC Dabiri, JO Gallegos, CL AF Breitburg, Denise L. Crump, Byron C. Dabiri, John O. Gallegos, Charles L. TI Ecosystem Engineers in the Pelagic Realm: Alteration of Habitat by Species Ranging from Microbes to Jellyfish SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Article ID SUBMERGED AQUATIC VEGETATION; CHESAPEAKE-BAY; EMILIANIA-HUXLEYI; ORGANIC-CARBON; COASTAL INLET; WATER-QUALITY; MARINE SNOW; BALTIC SEA; OCEAN; HYPOXIA AB Ecosystem engineers are species that alter the physical environment in ways that create new habitat or change the suitability of existing habitats for themselves or other organisms. In marine systems, much of the focus has been on species such as corals, oysters, and macrophytes that add physical structure to the environment, but organisms ranging from microbes to jellyfish and finfish that reside in the water column of oceans, estuaries, and coastal seas alter the chemical and physical environment both within the water column and on the benthos. By causing hypoxia, changing light regimes, and influencing physical mixing, these organisms may have as strong an effect as species that fall more clearly within the classical category of ecosystem engineer. In addition, planktonic species, such as jellyfish, may indirectly alter the physical environment through predator-mediated landscape structure. By creating spatial patterns of habitats that vary in their rates of mortality due to predation, planktonic predators may control spatial patterns and abundances of species that are the direct creators or modifiers of physical habitat. C1 [Breitburg, Denise L.; Gallegos, Charles L.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Crump, Byron C.] Univ Maryland, Ctr Environm Sci, Horn Pt Lab, Cambridge, MD 21613 USA. [Dabiri, John O.] CALTECH, Pasadena, CA 91125 USA. RP Breitburg, DL (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM breitburgd@si.edu OI Gallegos, Charles/0000-0001-5112-0166 FU Maryland Sea [R/P-54]; National Science Foundation [OCE0453905, OCE0961920, GSTCN0001A7, IOS-0938257]; The Society for Integrative and Comparative Biology Division of Ecology and Evolution; Division of Invertebrate Zoology; American Microscopy Society FX Support was provided by Maryland Sea Grant R/P-54 to D. Breitburg and National Science Foundation grants OCE0453905, OCE0961920, and GSTCN0001A7 to B. Crump for research described in this manuscript. We also thank the National Science Foundation (IOS-0938257), The Society for Integrative and Comparative Biology Division of Ecology and Evolution and the Division of Invertebrate Zoology, and the American Microscopy Society for supporting the symposium and publication. NR 79 TC 13 Z9 14 U1 0 U2 16 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 EI 1557-7023 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD AUG PY 2010 VL 50 IS 2 BP 188 EP 200 DI 10.1093/icb/icq051 PG 13 WC Zoology SC Zoology GA 630NJ UT WOS:000280279800004 PM 21558198 ER PT J AU DiMichele, WA Cecil, CB Montanez, IP Falcon-Lang, HJ AF DiMichele, William A. Cecil, C. Blaine Montanez, Isabel P. Falcon-Lang, Howard J. TI Cyclic changes in Pennsylvanian paleoclimate and effects on floristic dynamics in tropical Pangaea SO INTERNATIONAL JOURNAL OF COAL GEOLOGY LA English DT Article DE Upland flora; Conifers; Cordaitaleans; Coal; Paleosol; Glaciation ID CENTRAL APPALACHIAN BASIN; COAL-SWAMP VEGETATION; ROCK LAKE SHALE; NORTH-AMERICA; NOVA-SCOTIA; CORDAITALEAN TREES; FOSSIL RECORD; TRANSANTARCTIC MOUNTAINS; NORTHEASTERN OHIO; COLUMBIANA COUNTY AB Wetland floras narrowly define perceptions of Pennsylvanian tropical ecosystems, the so-called Coal Age. Such wetlands reflect humid to perhumid climate, leading to characterizations of Pennsylvanian tropics as everwet, swampy. These views are biased by the high preservation potential of wetlands. Sedimentation patterns, paleosols, and fossil floras indicate the presence of vegetation tolerant of subhumid to dry-subhumid, perhaps semi-arid climate in basins between peat formation times. Understanding the significance of this seasonally-dry vegetation has suffered from conceptual and terminological confusion. A clearer view has emerged as models for framing the data have improved. Basinal floras typical of seasonally-dry conditions, relatively low soil moisture regimes, are well documented but mainly from isolated deposits. Some of the earliest, dominated by primitive pteridosperms ("Flozfern" floras), occur in clastic rocks between European Early Pennsylvanian coal beds. lAter Early Pennsylvanian, fern-cordaitalean vegetation, different from coal floras, is preserved in marine goniatite bullions. Conifers are first suggested by late Mississippian Potoniesporites pollen. About the same time, in North America, broadleaf foliage, Lesleya and Megalopteris occur in basin-margin settings, on drought-prone limestone substrates. The best known, xeromorphic floras found between coal beds appear in the Middle through Late Pennsylvanian, containing conifers, cordaitaleans, and pteridosperms. The Middle Pennsylvanian appearances of this flora are mainly allochthonous, though parautochthonous occurrences have been reported. Parautochthonous assemblages are mostly Late Pennsylvanian. The conifer flora became dominant in western and central Pangaean equatorial lowlands in earliest Permian. Location of the humid-perhumid wetland flora during periods of relative dryness, though rarely discussed, is as, or more, perplexing than the spatial location of seasonally-dry floras through - time wetland plants had few migratory options and possibly survived in small refugia, within and outside of basins. Coupled oscillations in climate, sea level, and vegetation were driven most likely by glacial-interglacial fluctuations, perhaps controlled by orbital cyclicity. Published by Elsevier B.V. C1 [DiMichele, William A.] Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, MRC 121, Washington, DC 20560 USA. [Cecil, C. Blaine] US Geol Survey, Reston, VA 20192 USA. [Montanez, Isabel P.] Univ Calif Davis, Dept Geol, Davis, CA 95616 USA. [Falcon-Lang, Howard J.] Univ London, Dept Earth Sci, Egham TW20 0EX, Surrey, England. RP DiMichele, WA (reprint author), Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, MRC 121, Washington, DC 20560 USA. EM dimichel@si.edu RI Falcon-Lang, Howard/D-8465-2011; DiMichele, William/K-4301-2012 FU Smithsonian Institution; NSF [EAR-545654]; NERC at Royal Holloway FX This paper is dedicated to Professor Hermann Pfefferkorn for his contributions to the understanding of Carboniferous and Permian vegetation, particularly for his unflagging commitment to enlivening it in our imaginations. The senior author, in particular, owes much to Professor Pfefferkorn for his years of advice, guidance, and friendship. This work was supported by grants from the Smithsonian Institution endowment and scholarly studies funds to WD, NSF grant EAR-545654 to IPM, and a NERC Advanced Fellowship held at Royal Holloway to H F-L We thank Christopher deal and Stanislav Oplugtil for their constructive reviews of an earlier version of this paper. We also extend our thanks to Mark H. Scheihing and Christopher Wnuk for their encouragement, patience, and editorial improvements to the manuscript. NR 209 TC 66 Z9 66 U1 1 U2 29 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0166-5162 J9 INT J COAL GEOL JI Int. J. Coal Geol. PD AUG 1 PY 2010 VL 83 IS 2-3 SI SI BP 329 EP 344 DI 10.1016/j.coal.2010.01.007 PG 16 WC Energy & Fuels; Geosciences, Multidisciplinary SC Energy & Fuels; Geology GA 644BM UT WOS:000281345400019 ER PT J AU Gingerich, O AF Gingerich, Owen TI Atlas of the Messier Objects: Highlights of the Deep Sky. SO JOURNAL FOR THE HISTORY OF ASTRONOMY LA English DT Book Review C1 [Gingerich, Owen] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gingerich, O (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. EM ginger@cfa.harvard.edu NR 3 TC 0 Z9 0 U1 0 U2 0 PU SCIENCE HISTORY PUBLICATIONS LTD PI CAMBRIDGE PA 16 RUTHERFORD RD, CAMBRIDGE CB2 2HH, ENGLAND SN 0021-8286 J9 J HIST ASTRON JI J. Hist. Astron. PD AUG PY 2010 VL 41 BP 419 EP 420 PN 3 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA 634YX UT WOS:000280623400011 ER PT J AU Lewis, JJ Bowman, TE AF Lewis, Julian J. Bowman, Thomas E. TI THE SUBTERRANEAN ASELLIDS OF MARYLAND: DESCRIPTION OF CAECIDOTEA NORDENI, NEW SPECIES, AND NEW RECORDS OF C. HOLSINGERI AND C. FRANZI (CRUSTACEA: MALACOSTRACA: ISOPODA) SO JOURNAL OF CAVE AND KARST STUDIES LA English DT Article AB Five species of subterranean asellid are known from Maryland: Caecidotea pricei, C. franzi, C. holsingeri, C. mausi and C. vandeli. Caecidotea nordeni, n. sp. is a subterranean species described from Washington Co., Maryland and assigned to the hobbsi Group. A new locality for C. franzi in Kentucky is presented. This species was previously known from two caves in Maryland and Pennsylvania. The newly discovered population represents a range extension of over 400 km. The male pleopod 2 morphology of specimens from a Maryland population of the subterranean asellid C. holsingeri is compared with populations from three caves in West Virginia. The range of C holsingeri extends from eastern West Virginia and adjacent Virginia to Garrett Co., Maryland. C1 [Lewis, Julian J.] Cave Karst & Groundwater Biol Consulting LLC, Lewis & Associates, Borden, IN 47106 USA. [Bowman, Thomas E.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Lewis, JJ (reprint author), Cave Karst & Groundwater Biol Consulting LLC, Lewis & Associates, 17903 State Rd 60, Borden, IN 47106 USA. EM lewisbioconsult@aol.com FU Smithsonian Institution; Karst Waters Institute; Cave Conservancy of the Virginias FX Dr. Bowman's drawings and other materials were provided to me during a visit to the National Museum of Natural History funded by a Visiting Scientist Grant from the Smithsonian Institution. Ms. Marilyn Schotte sponsored that visit, as well as providing specimens from the museum collections. The manuscript was kindly reviewed by Dr. David C. Culver, Mr. Dan Feller, Dr. John R. Holsinger, Mr. Ellis Laudermilk and Ms. Marilyn Schotte. The description of Caecidotea nordeni was funded by the Karst Waters Institute and Cave Conservancy of the Virginias, kindly facilitated by Dr. David C. Culver. NR 14 TC 2 Z9 2 U1 0 U2 6 PU NATL SPELEOLOGICAL SOC PI HUNTSVILLE PA 2813 CAVE AVE, HUNTSVILLE, AL 35810-4431 USA SN 1090-6924 J9 J CAVE KARST STUD JI J. Cave Karst Stud. PD AUG PY 2010 VL 72 IS 2 BP 100 EP 104 DI 10.4311/jcks2009lsc0092 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 646XO UT WOS:000281578600005 ER PT J AU Ferrari, FD Ivanenko, VN Dahms, HU AF Ferrari, Frank D. Ivanenko, Viatcheslav N. Dahms, Hans-Uwe TI BODY ARCHITECTURE AND RELATIONSHIPS AMONG BASAL COPEPODS SO JOURNAL OF CRUSTACEAN BIOLOGY LA English DT Article DE basal Copepoda; body architecture; phylogeny ID POSTEMBRYONIC DEVELOPMENT; NAUPLIAR DEVELOPMENT; BRITTLE STAR; CRUSTACEA; ONTOGENY; CYCLOPOIDA; CALANOIDA; HARPACTICOIDA; MORPHOLOGY; EVOLUTION AB Most copepods exhibit one of three kinds of body architecture: I) six broad anterior trunk somites and five narrow posterior trunk somites of gymnopleans; 2) five broad anterior trunk somites and six narrow posterior trunk somites of many podopleans; or 3) four broad anterior trunk somites and seven narrow posterior trunk somites of thaumatopsylloids. A phylogenetic analysis using naupliar and post-naupliar characters, with Mystacocarida as the sister taxon of Copepoda, supports the hypothesis that the thaumatopsylloid architecture is the oldest. No narrow somite is transformed into a broad somite during post-naupliar development of thaumatopsylloids. Podopleans and gymnopleans begin their post-naupliar development with one trunk somite fewer than thaumatopsylloids. Podoplean architecture results when the anterior narrow somite of thaumatopsylloids is transformed to the posterior broad somite of podopleans during the first post-naupliar molt. Gymnoplean architecture, the youngest, results when the anterior narrow somite found on podopleans is transformed to the posterior broad somite during the second post-naupliar molt. These developmental transformations of body somites are assumed to explain the evolutionary origins of podoplean and gymnoplean body architectures. C1 [Ferrari, Frank D.] Smithsonian Inst, Natl Museum Nat Hist, IZ MSC, Suitland, MD 20746 USA. [Ivanenko, Viatcheslav N.] Moscow MV Lomonosov State Univ, Fac Biol, Dept Invertebrate Zool, Moscow 119899, Russia. [Dahms, Hans-Uwe] Sangmyung Univ, Green Life Sci Dept, Seoul 110743, South Korea. RP Ferrari, FD (reprint author), Smithsonian Inst, Natl Museum Nat Hist, IZ MSC, MRC 534,4210 Silver Hill Rd, Suitland, MD 20746 USA. EM ferrarif@si.edu; ivanenko@mail.bio.msu.ru; hansdahms@smu.ac.kr RI Ivanenko, Viatcheslav/B-8198-2008 OI Ivanenko, Viatcheslav/0000-0003-1255-0491 FU Russian Foundation for Basic Research [09-04-01523-a]; Ministry of Education and Science of the Russian Federation [02.740.11.0280, P1291]; Smithsonian Institution's Office of Fellowships FX VNI was supported by grants from the Russian Foundation for Basic Research (09-04-01523-a) and from the Ministry of Education and Science of the Russian Federation: 02.740.11.0280 & P1291), and H-UD by a grant from the Smithsonian Institution's Office of Fellowships. We thank Dr. John Fonsshell, Research Associate at the Smithsonian Institution's National Museum of Natural History, for help in collecting specimens of Derocheilocaris typicus. NR 103 TC 11 Z9 11 U1 0 U2 4 PU CRUSTACEAN SOC PI SAN ANTONIO PA 840 EAST MULBERRY, SAN ANTONIO, TX 78212 USA SN 0278-0372 J9 J CRUSTACEAN BIOL JI J. Crustac. Biol. PD AUG PY 2010 VL 30 IS 3 BP 465 EP 477 DI 10.1651/09-3220.1 PG 13 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 613HC UT WOS:000278969000015 ER PT J AU Garrish, V Cernusak, LA Winter, K Turner, BL AF Garrish, Valerie Cernusak, Lucas A. Winter, Klaus Turner, Benjamin L. TI Nitrogen to phosphorus ratio of plant biomass versus soil solution in a tropical pioneer tree, Ficus insipida SO JOURNAL OF EXPERIMENTAL BOTANY LA English DT Article DE Carbon isotope ratio; N:P ratio; nutrient supply; transpiration; tropical tree; water-use efficiency ID WATER-USE EFFICIENCY; CARBON-ISOTOPE DISCRIMINATION; N-P RATIOS; NUTRIENT LIMITATION; TRANSPIRATION EFFICIENCY; LEAF CONDUCTANCE; GROWTH; STOICHIOMETRY; AVAILABILITY; NUTRITION AB It is commonly assumed that the nitrogen to phosphorus (N:P) ratio of a terrestrial plant reflects the relative availability of N and P in the soil in which the plant grows. Here, this was assessed for a tropical pioneer tree, Ficus insipida. Seedlings were grown in sand and irrigated with nutrient solutions containing N:P ratios ranging from < 1 to > 100. The experimental design further allowed investigation of physiological responses to N and P availability. Homeostatic control over N:P ratios was stronger in leaves than in stems or roots, suggesting that N:P ratios of stems and roots are more sensitive indicators of the relative availability of N and P at a site than N:P ratios of leaves. The leaf N:P ratio at which the largest plant dry mass and highest photosynthetic rates were achieved was similar to 11, whereas the corresponding whole-plant N:P ratio was similar to 6. Plant P concentration varied as a function of transpiration rate at constant nutrient solution P concentration, possibly due to transpiration-induced variation in the mass flow of P to root surfaces. The transpiration rate varied in response to nutrient solution N concentration, but not to nutrient solution P concentration, demonstrating nutritional control over transpiration by N but not P. Water-use efficiency varied as a function of N availability, but not as a function of P availability. C1 [Cernusak, Lucas A.] Charles Darwin Univ, Sch Environm & Life Sci, Darwin, NT 0909, Australia. [Garrish, Valerie] McGill Univ, Dept Geog, Montreal, PQ H3A 1B1, Canada. [Winter, Klaus; Turner, Benjamin L.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Cernusak, LA (reprint author), Charles Darwin Univ, Sch Environm & Life Sci, Darwin, NT 0909, Australia. EM lucas.cernusak@cdu.edu.au RI Turner, Benjamin/E-5940-2011; Cernusak, Lucas/A-6859-2011 OI Turner, Benjamin/0000-0002-6585-0722; Cernusak, Lucas/0000-0002-7575-5526 FU Social Sciences and Humanities Research Council of Canada; Smithsonian Tropical Research Institute; Australian Postdoctoral Fellowship; Australian Research Council [DP0771427] FX We thank Jorge Aranda, Tania Romero, and Dayana Agudo for technical assistance with the experiment. Financial support for the project was provided by the Social Sciences and Humanities Research Council of Canada through a grant to VG, and by the Smithsonian Tropical Research Institute. LAC was supported by an Australian Postdoctoral Fellowship and Discovery grant (DP0771427) from the Australian Research Council. NR 44 TC 27 Z9 29 U1 5 U2 36 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0022-0957 J9 J EXP BOT JI J. Exp. Bot. PD AUG PY 2010 VL 61 IS 13 BP 3735 EP 3748 DI 10.1093/jxb/erq183 PG 14 WC Plant Sciences SC Plant Sciences GA 638OX UT WOS:000280905400022 PM 20591897 ER PT J AU Griffin, NL D'Aout, K Ryan, TM Richmond, BG Ketcham, RA Postnov, A AF Griffin, Nicole L. D'Aout, Kristiaan Ryan, Timothy M. Richmond, Brian G. Ketcham, Richard A. Postnov, Andrei TI Comparative forefoot trabecular bone architecture in extant hominids SO JOURNAL OF HUMAN EVOLUTION LA English DT Article DE Anisotropy; Bone volume fraction; Hallux; Metatarsal; Proximal phalanx ID ITERATIVE SELECTION METHOD; MICRO-COMPUTED TOMOGRAPHY; CANCELLOUS BONE; FEMORAL-HEAD; AUSTRALOPITHECUS-AFARENSIS; METATARSAL; PRIMATES; WALKING; FOOT; ORIENTATION AB The appearance of a forefoot push-off mechanism in the hominin lineage has been difficult to identify, partially because researchers disagree over the use of the external skeletal morphology to differentiate metatarsophalangeal joint functional differences in extant great apes and humans. In this study, we approach the problem by quantifying properties of internal bone architecture that may reflect different loading patterns in metatarsophalangeal joints in humans and great apes. High-resolution x-ray computed tomography data were collected for first and second metatarsal heads of Homo sapiens (n = 26), Pan paniscus (n = 17), Pan troglodytes (n = 19), Gorilla gorilla (n = 16), and Pongo pygmaeus (n = 20). Trabecular bone fabric structure was analyzed in three regions of each metatarsal head. While bone volume fraction did not significantly differentiate human and great ape trabecular bone structure, human metatarsal heads generally show significantly more anisotropic trabecular bone architectures, especially in the dorsal regions compared to the corresponding areas of the great ape metatarsal heads. The differences in anisotropy between humans and great apes support the hypothesis that trabecular architecture in the dorsal regions of the human metatarsals are indicative of a forefoot habitually used for propulsion during gait. This study provides a potential route for predicting forefoot function and gait in fossil hominins from metatarsal head trabecular bone architecture. (C) 2010 Elsevier Ltd. All rights reserved. C1 [Griffin, Nicole L.] Duke Univ, Dept Evolutionary Anthropol, Durham, NC 27710 USA. [D'Aout, Kristiaan] Univ Antwerp, Dept Biol, B-2020 Antwerp, Belgium. [D'Aout, Kristiaan] Royal Zool Soc Antwerp, Ctr Res & Conservat, Antwerp, Belgium. [Ryan, Timothy M.] Penn State Univ, Dept Anthropol, University Pk, PA 16802 USA. [Richmond, Brian G.] George Washington Univ, Ctr Adv Study Hominid Paleobiol, Washington, DC USA. [Richmond, Brian G.] Smithsonian Inst, Human Origins Program, Washington, DC 20560 USA. [Ketcham, Richard A.] Univ Texas Austin, Dept Geol Sci, Austin, TX USA. [Postnov, Andrei] Univ Antwerp, Dept Biomed Sci, B-2020 Antwerp, Belgium. [Postnov, Andrei] PN Lebedev Phys Inst, Moscow 117924, Russia. RP Griffin, NL (reprint author), Duke Univ, Dept Evolutionary Anthropol, POB 90383 Sci Dr, Durham, NC 27710 USA. EM nicole.griffin@duke.edu RI Ketcham, Richard/B-5431-2011; Postnov, Andrey/M-6906-2015; OI Ketcham, Richard/0000-0002-2748-0409; D'Aout, Kristiaan/0000-0002-6043-7744 FU GWU; Sigma Xi; L.S.B. Leakey Foundation; National Science Foundation [BCS-0726124, DGE-9987590, DGE-0801634]; Duke University FX We are grateful to Linda Gordon and Dr. Dave Hunt (NMNH), Dr. Emmanuel Gilissen (Museum for Central Africa), Dr. Owen Lovejoy (Libben Collection) for access to the collections used in this study and their assistance during data collection. Special thanks to Dr. Jessie Maisano at the HRXCT lab for all of her help, Dr. Nora DeClerk for permitting NG and KD to work in her microCT lab facility, and Dr. Christine Wall for providing NG a computer to run part of the analysis. We also extend our appreciation to Dr. Masato Nakatsukasa and Dr. Bernard Wood for reviewing earlier versions of this manuscript. NG would also wish to acknowledge Dr. Daniel Schmitt for his continuous support and guidance. Funding has been provided by the GWU Cotlow Field Research Fund, Sigma Xi Grant-in-Aid of Research, L.S.B. Leakey Foundation, the National Science Foundation: BCS-0726124, NSF IGERT DGE-9987590 and DGE-0801634, the GWU Selective Excellence Fellowship for Hominid Paleobiology, and Duke University. NR 63 TC 27 Z9 27 U1 2 U2 14 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0047-2484 J9 J HUM EVOL JI J. Hum. Evol. PD AUG PY 2010 VL 59 IS 2 BP 202 EP 213 DI 10.1016/j.jhevol.2010.06.006 PG 12 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 647LG UT WOS:000281619400004 PM 20655571 ER PT J AU Hershler, R Liu, HP Lang, BK AF Hershler, Robert Liu, Hsiu-Ping Lang, Brian K. TI TRANSFER OF COCHLIOPA TEXANA TO PYRGULOPSIS (HYDROBIIDAE) AND DESCRIPTION OF A THIRD CONGENER FROM THE LOWER PECOS RIVER BASIN SO JOURNAL OF MOLLUSCAN STUDIES LA English DT Article ID AMERICAN NYMPHOPHILINE GASTROPODS; MITOCHONDRIAL-DNA SEQUENCES; PHYLOGENETIC-RELATIONSHIPS; MOLECULAR SYSTEMATICS; AQUATIC GASTROPODS; RISSOOIDEA; MOLLUSCA; SNAILS; GENUS AB The Phantom Cave snail (Cochliopa texana), a little-studied rissooidean gastropod that is locally endemic within the lower Pecos River basin (Texas) and currently a candidate for addition to the Federal list of threatened and endangered species, is redescribed and transferred to the hydrobiid genus Pyrgulopsis, based on shell and anatomical characters. Specimens from the type locality (Phantom Lake Spring) and San Solomon Spring are larger than those from East Sandia Spring and also differ somewhat in shell shape and shape of the central cusps of the lateral radular teeth. However genetic (mtCOI, NDI) variation within and among these geographically proximal (613 km) populations was slight, providing no basis for the recognition of distinct conservation units of this imperiled species. We also describe Pyrgulopsis ignota n. sp., which was recently discovered in a different part of the lower Pecos River basin and initially confused with the Phantom Cave snail. These two species differ in shell shape, operculum morphology, and form and glandular ornament of the penis. They are also strongly differentiated genetically from each other and from (13) other regional congeners (pairwise sequence divergence.6.3% for both genes). A Bayesian phylogenetic analysis of the COI and NDI dataset indicated that these two snails are not closely related and that P. ignota occupies a basal position relative to other regional congeners. C1 [Hershler, Robert] Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20013 USA. [Liu, Hsiu-Ping] Metropolitan State Coll, Dept Biol, Denver, CO 80217 USA. [Lang, Brian K.] New Mexico Dept Game & Fish, Santa Fe, NM 87507 USA. RP Hershler, R (reprint author), Smithsonian Inst, Dept Invertebrate Zool, POB 37012,NHB W-305,MRC 163, Washington, DC 20013 USA. EM hershlerr@si.edu FU Upper Colorado Regional Office, Bureau of Reclamation [08-AA-40-2782] FX Collecting permits were provided by the Texas Parks and Wildlife Department (Phantom Lake and San Solomon Springs) and The Nature Conservancy (East Sandia and Caroline Springs). Tom Johnson, John Karges, David Riskind and Jason Wrinkle arranged for the permits and access to collection localities. Yolanda Villacampa measured shells and prepared the scanning electron micrographs. Karolyn Darrow prepared the anatomical drawings. Jessica Marn assisted with DNA extraction and amplification. This study was funded (in part) by an award (to R. H.) from the Upper Colorado Regional Office, Bureau of Reclamation (Interagency Acquisition No. 08-AA-40-2782), which was facilitated by Gary Dean. Fiscal support for B. K. L.'s fieldwork was provided by the United States Fish and Wildlife Service (Region 2) and New Mexico Department of Game and Fish under Section 6 grant E-56. We thank Winston Ponder and Associate Editor Diarmaid O'Foighil for comments that improved this manuscript. NR 38 TC 5 Z9 5 U1 0 U2 2 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 AUG PY 2010 VL 76 BP 245 EP 256 DI 10.1093/mollus/eyq002 PN 3 PG 12 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA 631AA UT WOS:000280317500004 ER PT J AU Schnell, NK Britz, R Johnson, GD AF Schnell, Nalani K. Britz, Ralf Johnson, G. David TI New Insights into the Complex Structure and Ontogeny of the Occipito-Vertebral Gap in Barbeled Dragonfishes (Stomiidae, Teleostei) SO JOURNAL OF MORPHOLOGY LA English DT Article DE Chauliodus; Eustomias; Leptostomias gladiator; myosepta; spino-occipital nerves; vertebral reduction; mesopelagic ID OSTEOLOGICAL DEVELOPMENT; TROPHIC ECOLOGY; NERVES; FISHES; CARTILAGE; HOMOLOGY; PISCES; BONE AB In all stomiid genera there is an occipito-vertebral gap between the skull and the first vertebra bridged only by the flexible notochord. Morphological studies from the early 20th century suggested that some stomiid genera have 1-10 of the anteriormost centra reduced or entire vertebrae missing in this region. Our study reviews this previous hypothesis. Using a new approach, we show that only in Chauliodus, Eustomias and Leptostomias gladiator vertebral centra are actually lost, with their respective neural arches and parapophyses persisting. We present results from a comparative analysis of the number and insertion sites of the anteriormost myosepta in 26 of the 28 stomiid genera. Generally in teleosts the first three myosepta are associated with the occiput, and the fourth is the first vertebral myoseptum. The insertion site of the fourth myoseptum plays an important role in this analysis, because it provides a landmark for the first vertebra. Lack of association of the fourth myoseptum with a vertebra is thus evidence that the first vertebra is reduced or absent. By counting the occipital and vertebral myosepta the number of reduced vertebrae in Chauliodus, Eustomias and Leptostomias gladiator can be inferred. Proper identification of the spino-occipital nerves provides an additional source of information about vertebral reduction. In all other stomiid genera the extensive occipito-vertebral gap is not a consequence of the reduction of vertebrae, but of an elongation of the notochord. The complex structure and ontogeny of the anterior part of the vertebral column of stomiids are discussed comparatively. J. Morphol. 271:1006-1022, 2010. (C) 2010 Wiley-Liss, Inc. C1 [Schnell, Nalani K.] Univ Tubingen, Dept Comparat Zool, D-72076 Tubingen, Germany. [Britz, Ralf] Nat Hist Museum, Dept Zool, London SW7 5BD, England. [Johnson, G. David] Smithsonian Inst, Div Fishes, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Schnell, NK (reprint author), Univ Tubingen, Dept Comparat Zool, Morgenstelle 28, D-72076 Tubingen, Germany. EM nalani.schnell@uni-tuebingen.de FU NMNH; SYNTHESYS (NHM) [GB-TAF-3239]; Herb and Evelyn Axelrod Chair in Systematic Ichthyology in the Division of Fishes (NMNH) FX Contract grant sponsor: Smithsonian Predoctoral Fellowship (NMNH); Contract grant sponsor: SYNTHESYS (NHM); Contract grant number: GB-TAF-3239; Contract grant sponsor: Herb and Evelyn Axelrod Chair in Systematic Ichthyology in the Division of Fishes (NMNH). NR 48 TC 10 Z9 11 U1 1 U2 5 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 AUG PY 2010 VL 271 IS 8 BP 1006 EP 1022 DI 10.1002/jmor.10858 PG 17 WC Anatomy & Morphology SC Anatomy & Morphology GA 631AE UT WOS:000280317900010 PM 20623652 ER PT J AU Guz, SS AF Guz, Savannah Schroll TI Recruitment, Development, and Retention of Information Professionals: Trends in Human Resources and Knowledge Management SO LIBRARY JOURNAL LA English DT Book Review C1 [Guz, Savannah Schroll] Smithsonian Lib, Washington, DC USA. NR 1 TC 0 Z9 0 U1 1 U2 6 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 AUG PY 2010 VL 135 IS 13 BP 110 EP 110 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 638IO UT WOS:000280887500309 ER PT J AU Guz, SS AF Guz, Savannah Schroll TI Technoliteracy, Discourse, and Social Practice: Frameworks and Applications in the Digital Age SO LIBRARY JOURNAL LA English DT Book Review C1 [Guz, Savannah Schroll] Smithsonian Lib, 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 AUG PY 2010 VL 135 IS 13 BP 110 EP 110 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 638IO UT WOS:000280887500311 ER PT J AU Guz, SS AF Guz, Savannah Schroll TI Homeland Security Preparedness and Information Systems: Strategies for Managing Public Policy SO LIBRARY JOURNAL LA English DT Book Review C1 [Guz, Savannah Schroll] Smithsonian Lib, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 1 PU REED BUSINESS INFORMATION PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD AUG PY 2010 VL 135 IS 13 BP 110 EP 110 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 638IO UT WOS:000280887500310 ER PT J AU Guz, SS AF Guz, Savannah Schroll TI Genetic Disorders Sourcebook, 4th edition SO LIBRARY JOURNAL LA English DT Book Review C1 [Guz, Savannah Schroll] Smithsonian Lib, 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 AUG PY 2010 VL 135 IS 13 BP 110 EP 110 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 638IO UT WOS:000280887500308 ER PT J AU Winters, KL van Herwerden, L Choat, JH Robertson, DR AF Winters, Kate L. van Herwerden, Lynne Choat, J. Howard Robertson, D. R. TI Phylogeography of the Indo-Pacific parrotfish Scarus psittacus: isolation generates distinctive peripheral populations in two oceans SO MARINE BIOLOGY LA English DT Article ID CORAL-REEF FISH; PHYLOGENETIC-RELATIONSHIPS; GENETIC-DIFFERENCES; CHLORURUS-SORDIDUS; SCARIDAE; DISTANCE; GROWTH; REGION; DIVERSIFICATION; CONNECTIVITY AB Phylogenetic, phylogeographic, population genetic and coalescence analyses were combined to examine the recent evolutionary history of the widespread Indo-Pacific parrotfish, Scarus psittacus, over a geographic range spanning three marine biogeographic realms. We sequenced 164 individuals from 12 locations spanning 17,000 km, from 55A(0)E to 143A(0)W, using 322 base pairs of mitochondrial control region (D-loop). S. psittacus displayed high haplotype (h = 0.83-0.98), but low nucleotide (< 1%) diversity. Most (> 83%) genetic variation was within populations. AMOVA revealed significant partitioning and identified five geographic groups. These included one central population and four populations peripheral to the centre. The central population occupied reefs from Western Australia to Tahiti and represented the central Indo-Pacific biogeographic realm. Cocos Keeling was distinct from central and western Indo-Pacific biogeographic realms occupying a position intermediate to these. Peripheral populations (Hawaii, Marquesas) represented the eastern Indo-Pacific biogeographic realm, while Seychelles represented the western Indo-Pacific biogeographic realm. All but the central population expanded (< 163 kya). Whilst all populations experienced major sea level and SST changes associated with Pleistocene glaciation cycles, the genetic structure of the central population was relatively homogenous unlike the remaining genetically distinctive populations. C1 [Winters, Kate L.; van Herwerden, Lynne; Choat, J. Howard] James Cook Univ, Mol Ecol & Evolut Lab, Sch Trop & Marine Biol, Townsville, Qld 4811, Australia. [Robertson, D. R.] Smithsonian Trop Res Inst, Balboa, Panama. RP van Herwerden, L (reprint author), James Cook Univ, Mol Ecol & Evolut Lab, Sch Trop & Marine Biol, Townsville, Qld 4811, Australia. EM kate.winters7@gmail.com; lynne.vanherwerden@jcu.edu.au; john.choat@jcu.edu.au; drr@stri.org RI van Herwerden, Lynne/I-1087-2012; Manager, MEEL/C-4732-2015 OI van Herwerden, Lynne/0000-0001-6717-8995; FU National Geographic Society, (Cocos Keeling, Marquesas); Queensland Government/Smithsonian Institution; Smithsonian Institution; Seychelles Fishing Authority; Cocos Keeling and Christmas Island National Parks; Department of Environment and Heritage Australia; Taiwan National Museum; Australian Institute of Marine Science; Lizard Island Research Station; University of Guam Marine Laboratory; University of Hawaii Marine Laboratory; James Cook University FX Funding and logistic support were provided by The National Geographic Society, (Cocos Keeling, Marquesas), The Queensland Government/Smithsonian Institution Collaborative Research Program on Reef Fishes, The Smithsonian Institution, The Seychelles Fishing Authority, Cocos Keeling and Christmas Island National Parks, Department of Environment and Heritage Australia, The Taiwan National Museum, The Australian Institute of Marine Science, The Lizard Island Research Station, the University of Guam Marine Laboratory; University of Hawaii Marine Laboratory and the James Cook University internal funding scheme. Tahiti specimens were collected by M. Meekan, W. Murray, R. Thorne, J. Robinson, J. Ackerman, W. Robbins, Li Shu Chen and L. Rocha. C. Birkeland provided logistic and field assistance, collection of specimens and access to Museum material. Collections on the GBR were carried out under GBRMPA Permit number G03/3871.1. S. Klanten, D. Blair and the JCU Molecular Ecology and Evolution Laboratory assisted with laboratory work and analysis. The work was carried out under James Cook University Ethics Approval No. A503. NR 63 TC 34 Z9 34 U1 1 U2 23 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0025-3162 J9 MAR BIOL JI Mar. Biol. PD AUG PY 2010 VL 157 IS 8 BP 1679 EP 1691 DI 10.1007/s00227-010-1442-4 PG 13 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 624RF UT WOS:000279836900002 ER PT J AU Wilson, L Keil, K McCoy, TJ AF Wilson, Lionel Keil, Klaus McCoy, Timothy J. TI Pyroclast loss or retention during explosive volcanism on asteroids: Influence of asteroid size and gas content of melt SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID AUBRITE PARENT BODY; SOLAR-SYSTEM; DIFFERENTIATED ASTEROIDS; ENSTATITE CHONDRITES; VOLATILE CONTENT; SILICATE MELTS; 4 VESTA; ERUPTIONS; PARTICLES; MAGMA AB We review the conditions under which explosive volcanism took place on early-forming differentiated asteroids. The pressure-dependent solubility of typical asteroid volatiles in melts implies that the gas driving explosive volcanism on asteroids less than approximately 100 km in diameter was probably present mainly as a free phase capable of accumulating into large gas bodies and, thus, causing slug flow in melts approaching the surface. In contrast, in asteroids larger than approximately 100 km the gas was probably present largely as a dispersion of small bubbles. We show that these gas distributions have implications for the size distribution of the pyroclastic droplets produced in explosive eruptions at the surface. All pyroclastic melt droplets are accelerated by the expanding gases, but their speeds lag the gas speed by a finite amount that is a function of the droplet size and density and the asteroid size and, hence, acceleration due to gravity. We compute pyroclast speeds and, by comparing them with escape velocities, we identify the critical pyroclast diameter on a given-size asteroid that distinguishes droplets lost to space from droplets that return to the surface. Identification of asteroidal pyroclasts and measurements of their sizes could throw light on the amounts of gas driving eruptions. C1 [Wilson, Lionel] Univ Lancaster, Lancaster Environm Ctr, Lancaster LA1 4YQ, England. [Keil, Klaus] Univ Hawaii Manoa, Sch Ocean & Earth Sci & Technol, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. [McCoy, Timothy J.] Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. RP Wilson, L (reprint author), Univ Lancaster, Lancaster Environm Ctr, Lancaster LA1 4YQ, England. EM l.wilson@lancaster.ac.uk FU NASA [NNX08AE08G, NNG06GF56G] FX This work was supported in part by the NASA Cosmochemistry Program, grant NNX08AE08G (K. Keil, P. I.) and by grant NNG06GF56G (T. McCoy, P. I.). This is Hawaii Institute of Geophysics and Planetology Publication no. 1857, and School of Ocean and Earth Science and Technology Publication no. 7953. NR 71 TC 9 Z9 9 U1 0 U2 1 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD AUG PY 2010 VL 45 IS 8 BP 1284 EP 1301 DI 10.1111/j.1945-5100.2010.01085.x PG 18 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 682UB UT WOS:000284427400005 ER PT J AU Ramirez, SR Nieh, JC Quental, TB Roubik, DW Imperatriz-Fonseca, VL Pierce, NE AF Ramirez, Santiago R. Nieh, James C. Quental, Tiago B. Roubik, David W. Imperatriz-Fonseca, Vera L. Pierce, Naomi E. TI A molecular phylogeny of the stingless bee genus Melipona (Hymenoptera: Apidae) SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Relaxed molecular clock; Penalized likelihood; Eusociality; Stingless bees; Honey bees; Melipona; Apis; Referential communication ID MITOCHONDRIAL-DNA SEQUENCE; HONEY-BEES; DIVERGENCE TIMES; CORBICULATE BEES; DANCE-LANGUAGE; FOSSIL BEE; COMMUNICATION; DISTANCE; APINAE; EUSOCIALITY AB Stingless bees (Meliponini) constitute a diverse group of highly eusocial insects that occur throughout tropical regions around the world. The meliponine genus Melipona is restricted to the New World tropics and has over 50 described species. Melipona, like Apis, possesses the remarkable ability to use representational communication to indicate the location of foraging patches. Although Melipona has been the subject of numerous behavioral, ecological, and genetic studies, the evolutionary history of this genus remains largely unexplored. Here, we implement a multigene phylogenetic approach based on nuclear, mitochondrial, and ribosomal loci, coupled with molecular clock methods, to elucidate the phylogenetic relationships and antiquity of subgenera and species of Melipona. Our phylogenetic analysis resolves the relationship among subgenera and tends to agree with morphology-based classification hypotheses. Our molecular clock analysis indicates that the genus Melipona shared a most recent common ancestor at least similar to 14-17 million years (My) ago. These results provide the groundwork for future comparative analyses aimed at understanding the evolution of complex communication mechanisms in eusocial Apidae. (C) 2010 Elsevier Inc. All rights reserved. C1 [Ramirez, Santiago R.; Quental, Tiago B.; Pierce, Naomi E.] Harvard Univ, Museum Comparat Zool, Cambridge, MA 02138 USA. [Nieh, James C.] Univ Calif San Diego, Div Biol Sci, Sect Ecol Behav & Evolut, La Jolla, CA 92093 USA. [Roubik, David W.] Smithsonian Trop Res Inst, Dpo, AA 34002 USA. [Roubik, David W.; Imperatriz-Fonseca, Vera L.] Univ Sao Paulo, Fac Filosofia Ciencias & Letras Ribeirao Preto, BR-14040090 Sao Paulo, Brazil. RP Ramirez, SR (reprint author), Univ Calif Berkeley, 137 Mulford Hall 3114, Berkeley, CA 94720 USA. EM sramirez@post.harvard.edu RI Ramirez, Santiago/B-4948-2012; Quental, Tiago/C-7077-2013; Imperatriz-Fonseca, Vera/H-5582-2012; OI Imperatriz-Fonseca, Vera/0000-0002-1079-2158; Nieh, James/0000-0001-6237-0726 FU ORBS (Opportunities for Research in the Behavioral Sciences Program); National Science Foundation [DEB 0608409, NSF-IBN 0316697, NSF DEB 0447242, NSF-IBN 0545856]; Putnam Expedition Fund FX We thank Paulo Nogueira-Neto and Jay Evans for providing crucial samples used in this study, Jennifer Davis and Jessica Girard for assistance in the laboratory, and Joao M.F. Camargo and Claus Rasmussen for their assistance in the identification of bee specimens. Beth Pringle provided useful comments on the manuscript. This project was supported by grants from ORBS (Opportunities for Research in the Behavioral Sciences Program), the National Science Foundation (NSF-DDIG, DEB 0608409, NSF-IBN 0316697, NSF DEB 0447242, and NSF-IBN 0545856) and grants from the Putnam Expedition Fund to J.C.N., S.R.R., and N.E.P. Samples were collected in Brazil under the Permit No. 057/2003 (IBAMA) and Peru under Permit No. 005141 (AG-INRENA). NR 56 TC 23 Z9 24 U1 4 U2 26 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 AUG PY 2010 VL 56 IS 2 BP 519 EP 525 DI 10.1016/j.ympev.2010.04.026 PG 7 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 612IF UT WOS:000278890100002 PM 20433931 ER PT J AU Xie, L Yi, TS Li, R Li, DZ Wen, J AF Xie, Lei Yi, Ting-Shuang Li, Rong Li, De-Zhu Wen, Jun TI Evolution and biogeographic diversification of the witch-hazel genus (Hamamelis L., Hamamelidaceae) in the Northern Hemisphere SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Hamamelidaceae; Hamamelis; Biogeography; trnL-F; psaA-ycf3; rps16; matK; arpB-rbcL; psbA-trnH; ITS; ETS; Phylogeny; Disjunct distribution; Fossils ID NUCLEAR RIBOSOMAL DNA; INTERNAL TRANSCRIBED SPACER; EASTERN ASIA; HISTORICAL BIOGEOGRAPHY; PHYLOGENETIC-RELATIONSHIPS; MOLECULAR PHYLOGENY; TAXONOMIC RICHNESS; UNIVERSAL PRIMERS; GEOGRAPHIC RANGE; TEMPERATE PLANTS AB The evolution of the eastern Asian and eastern North American disjunction of the witch-hazel genus Hamamelis L (Hamamelidaceae) was examined through phylogenetic and biogeographic analyses. Phylogenetic relationships of all Hamamelis species were reconstructed using parsimony and Bayesian analyses of sequence data from six plastid (trnL-F, psaA-ycf3, rps16, matK, atpB-rbcL, and psbA-trnH) and two nuclear (ITS and ETS) DNA regions. The phylogeny was then used to infer the biogeographic origin and subsequent diversification using both event-based (DIVA) and maximum likelihood (LAGRANGE) methods incorporating fossil data. The times of divergence within Hamamelis were estimated with the Bayesian approach using the program BEAST. A very low level of molecular variation was detected in both the plastid and the nuclear DNA regions within Hamamelis. The combined analyses resulted in a phylogeny of the genus with higher resolution and support values. Hamamelis was supported to be monophyletic with H. mollis from eastern China diverged first in the genus. All North American species formed a clade and was sister to the eastern Asian H. japonica. Within the North American clade, H. mexicana was sister to H. vernalis, and the recently described species H. ovalis was found to be closely related to the widespread species H. virginiana. The stem age of Hamamelis was estimated to be at the Eocene (51.2 mya, with 95% HDP: 49.0-54.6 mya), and the crown age of the genus was dated to be at the late Miocene (9.7 mya, with 95% HDP: 3.6-18.1 mya, or 10.6 mya, with 95% HDP: 4.2-19.6 mya). The disjunction between the eastern Asian and the eastern North American species was dated to be 7.1 mya (95% HDP: 3.1-13.6 mya) or 7.7 mya (95% HDP: 3.4-13.6 mya). Biogeographic analyses incorporating fossils resulted in more equally possible solutions at the stem lineage of Hamamelis than those including extant species only. Eastern Asia is inferred to be the most-likely area for the origin of Hamamelis. The current disjunction was due to the extinction in western North America and Europe from Eocene to late Miocene, and later migration from eastern Asia into North America. The Bering land bridge was hypothesized to have played an important role in the evolution of this disjunction. The current species diversity of the genus was the result of relatively recent diversification events during the late Miocene rather than long accumulation of lineages from the early Tertiary. Published by Elsevier Inc. C1 [Xie, Lei; Yi, Ting-Shuang; Li, Rong; Li, De-Zhu; Wen, Jun] Chinese Acad Sci, Key Lab Biodivers & Biogeog, Plant Germplasm & Genom Ctr, Germplasm Bank Wild Species, Kunming 650204, Peoples R China. [Xie, Lei] Beijing Forestry Univ, Coll Biol Sci & Biotechnol, Beijing 100083, Peoples R China. [Li, Rong; Wen, Jun] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, MRC 166, Washington, DC 20013 USA. RP Yi, TS (reprint author), Chinese Acad Sci, Key Lab Biodivers & Biogeog, Plant Germplasm & Genom Ctr, Germplasm Bank Wild Species, Kunming 650204, Peoples R China. EM tingshuangyi@mail.kib.ac.cn; wenj@si.edu OI li, de zhu/0000-0002-4990-724X FU National Natural Science Foundation of China [30828001]; John D. and Catherine T. MacArthur Foundation FX We thank Rob Nicolson, Alan Weakley and W.-B. Yu for help with obtaining samples, and two anonymous reviewers and Associate Editor Lena Hileman for constructive comments. This study was supported by the National Natural Science Foundation of China to J. Wen and T. Yi (project no. 30828001), and grants from the John D. and Catherine T. MacArthur Foundation to J. Wen, Rick Ree and Greg Mueller. NR 136 TC 19 Z9 19 U1 5 U2 44 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1055-7903 J9 MOL PHYLOGENET EVOL JI Mol. Phylogenet. Evol. PD AUG PY 2010 VL 56 IS 2 BP 675 EP 689 DI 10.1016/j.ympev.2010.02.018 PG 15 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 612IF UT WOS:000278890100017 PM 20171295 ER PT J AU Zeng, CX Zhang, YX Triplett, JK Yang, JB Li, DZ AF Zeng, Chun-Xia Zhang, Yu-Xiao Triplett, Jimmy K. Yang, Jun-Bo Li, De-Zhu TI Large multi-locus plastid phylogeny of the tribe Arundinarieae (Poaceae: Bambusoideae) reveals ten major lineages and low rate of molecular divergence SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Arundinarieae; China; Chloroplast DNA regions; Large sample size; Phylogenetic analysis ID GRASS FAMILY POACEAE; DNA-SEQUENCE DATA; CHLOROPLAST DNA; NONCODING REGIONS; WOODY BAMBOOS; THAMNOCALAMUS GROUP; UNIVERSAL PRIMERS; ALLIES GRAMINEAE; GBSSI GENE; NUCLEAR AB The temperate bamboos (tribe Arundinarieae) are notorious for being taxonomically extremely difficult. China contains some of the world's greatest diversity of the tribe Arundinarieae, with most genera and species endemic. Previous investigation into phylogenetic relationships of the temperate bamboos revealed several major clades, but emphasis on the species-level relationships among taxa in North America and Japan. To further elucidate relationships among the temperate bamboos, a very broad sampling of Chinese representatives was examined. We produced 9463 bp of sequences from eight non-coding chloroplast regions for 146 species in 26 genera and 5 outgroups. The loci sequenced were atpl/H, psaA-ORF170, rp132-trnL, rpoB-trnC, rps16-trnQ trnD/T, trnS/G, and trnT/L. Phylogenetic analyses using maximum parsimony and Bayesian inference supported the monophyly of Arundinarieae. The two major subtribes, Arundinariinae and Shibataeinae, defined on the basis of different synflorescence types, were indicated to be polyphyletic. Most genera in this tribe were confirmed to be paraphyletic or polyphyletic. The cladograms suggest that Arundinarieae is divided into ten major lineages. In addition to six lineages suggested in a previous molecular study (Bergbamboes, the African alpine bamboos, Chimonocalamus, the Shibataea clade, the Phyllostachys clade, and the Arundinaria clade), four additional lineages were recovered in our results, each represented by a single species: Gaoligongshania megalothyrsa, Indocalamus sinicus, lndocalamus wilsonii. Thamnocalamus spathiflorus. Our analyses also indicate that (1) even more than 9000 bp of fast-evolving plastid sequence data cannot resolve the inter- and infra-relationships among and within the ten lineages of the tribe Arundinarieae; (2) an extensive sampling is indispensable for phylogeny reconstruction in this tribe, especially given that many genera appear to be paraphyletic or polyphyletic. Perhaps the ideal way to further illuminate relationships among the temperate bamboos is to sample multiple nuclear loci or whole chloroplast sequences in order to obtain sufficient variation. (c) 2010 Elsevier Inc. All rights reserved. C1 [Zeng, Chun-Xia; Zhang, Yu-Xiao; Yang, Jun-Bo; Li, De-Zhu] Chinese Acad Sci, Kunming Inst Bot, Key Lab Biodivers & Biogeog, Kunming 650204, Yunnan, Peoples R China. [Zeng, Chun-Xia; Zhang, Yu-Xiao] Chinese Acad Sci, Grad Univ, Beijing 100049, Peoples R China. [Zeng, Chun-Xia; Zhang, Yu-Xiao; Yang, Jun-Bo; Li, De-Zhu] Gerrnplasm Bank Wild Species, Plant Germplasm & Genom Ctr, Kunming 650204, Yunnan, Peoples R China. [Triplett, Jimmy K.] Smithsonian Inst, Dept Biol, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Li, DZ (reprint author), Chinese Acad Sci, Kunming Inst Bot, Key Lab Biodivers & Biogeog, Kunming 650204, Yunnan, Peoples R China. EM dzl@mail.kib.ac.cn OI li, de zhu/0000-0002-4990-724X FU National Basic Research Program of China (973 Program) [2007CB411601]; National Natural Science Foundation of China [30770154]; Chinese Academy of Sciences [KSCX2-YW-N-029]; National Geographic Society (U.S.A.) [7336-02]; National Science Foundation (U.S.A.) [DEB-0515712] FX This study was supported by the National Basic Research Program of China (973 Program, Grant No.: 2007CB411601) and the National Natural Science Foundation of China (Grant No: 30770154), also partly supported by the Knowledge Innovation Program of the Chinese Academy of Sciences (Grant No.: KSCX2-YW-N-029), and grants from the National Geographic Society (U.S.A.) (7336-02 to Lynn G. Clark and De-Zhu Li) and the National Science Foundation (U.S.A.) (DEB-0515712 to Lynn G. Clark). We are indebted to Professor Yu-Long Ding of Nanjing Forestry University; to Professor Nian-He Xia, Dr. Yun-Fei Deng, and Mr. Ru-Shun Lin of South China Botanical Garden, Chinese Academy of Sciences (CAS); to Professor Tong-Pei Yi and Mr. Lin Yang of Sichuan Agricultural University; and to Professors Shui-Sheng You and Shi-Pin Chen of Fujian Agriculture and Forestry University for their essential and generous help during field work. We would also like to thank Drs. Zhen-Hua Guo, Han-Qi Yang, Lian-Ming Gao, Jin-Mei Lu, Hong-Tao Li and other colleagues at the Key Laboratory of Biodiversity and Biogeography of the Kunming Institute of Botany, CAS for much practical and theoretical help throughout the course of this research. We also specially thank Dr. Lei Xie at the College of Biological Sciences and Biotechnology, Beijing Forestry University for his valuable suggestions for revising the manuscript. NR 102 TC 31 Z9 38 U1 2 U2 13 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 AUG PY 2010 VL 56 IS 2 BP 821 EP 839 DI 10.1016/j.ympev.2010.03.041 PG 19 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 612IF UT WOS:000278890100030 PM 20381627 ER PT J AU Smith, N Povich, MS Whitney, BA Churchwell, E Babler, BL Meade, MR Bally, J Gehrz, RD Robitaille, TP Stassun, KG AF Smith, Nathan Povich, Matthew S. Whitney, Barbara A. Churchwell, Ed Babler, Brian L. Meade, Marilyn R. Bally, John Gehrz, Robert D. Robitaille, Thomas P. Stassun, Keivan G. TI Spitzer Space Telescope observations of the Carina nebula: the steady march of feedback-driven star formation SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: formation; stars: luminosity function, mass function; stars: pre-main-sequence; H II regions; ISM: evolution; ISM: individual objects: NGC 3372 ID YOUNG STELLAR OBJECTS; 2-DIMENSIONAL RADIATIVE-TRANSFER; INFRARED ARRAY CAMERA; SPECTRAL ENERGY-DISTRIBUTIONS; WOLF-RAYET STARS; INTERSTELLAR CLOUDS; DUST FORMATION; ETA-CARINAE; PHOTODISSOCIATION REGIONS; PROTOSTELLAR ENVELOPES AB We report the first results of imaging the Carina nebula (NGC 3372) with the Infrared Array Camera (IRAC) onboard the Spitzer Space Telescope, providing a photometry catalogue of over 44 000 point sources as well as a catalogue of over 900 candidate young stellar objects (YSOs) based on tits to their spectral energy distributions (SEDs). We discuss several aspects of the extended emission, including the structure of dozens of dust pillars that result when a clumpy molecular cloud is shredded by feedback from massive stars. There are surprisingly few of the 'extended green objects' (EGOs) that are normally taken as signposts of outflow activity in Spitzer data, and not one of the dozens of Herbig-Haro jets detected optically are seen as EGOs. EGOs are apparently poor tracers of outflow activity in strongly irradiated environments, due to the effects of massive star feedback. A population of 'extended red objects' tends to be found around late O-type and early B-type stars, some with clear bow-shock morphology. These are dusty shocks where stellar winds collide with photoevaporative flows off nearby clouds. Finally, the relative distributions of O-type stars, small star clusters and subclusters of YSOs as compared to the dust pillars show that while some YSOs are located within dust pillars, many more stars and YSOs reside just outside pillar heads. We suggest that pillars are transient phenomena, part of a continuous outwardly propagating wave of star formation driven by feedback from massive stars. As the pillars are destroyed, they leave newly formed stars in their wake, and these are then subsumed into the young OB association. The YSOs are found predominantly in the cavity between pillars and massive stars, arguing that their formation was in fact triggered. Altogether, the current generation of YSOs shows no strong deviation from a normal initial mass function (IMF). The number of YSOs is consistent with a roughly constant star-formation rate over the past similar to 3 Myr, implying that propagating star formation in pillars constitutes an important mechanism to construct unbound OB associations. These accelerated pillars may give birth to massive O-type stars that, after several million years, could appear to have formed in isolation. C1 [Smith, Nathan] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Povich, Matthew S.; Churchwell, Ed; Babler, Brian L.; Meade, Marilyn R.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Povich, Matthew S.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16801 USA. [Whitney, Barbara A.] Space Sci Inst, Boulder, CO 80301 USA. [Bally, John] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Gehrz, Robert D.] Univ Minnesota, Dept Astron, Minneapolis, MN 55454 USA. [Robitaille, Thomas P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Stassun, Keivan G.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. RP Smith, N (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. EM nathans@astro.berkeley.edu OI Babler, Brian/0000-0002-6984-5752; Robitaille, Thomas/0000-0002-8642-1329 FU NASA [1256406, 1215746]; NSF [AST-0901646]; JPL/Caltech to the University of Minnesota FX This work was based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through awards issued by JPL/Caltech as part of GO programs 3420 and 20452. MSP was supported by an NSF Astronomy & Astroplysics Fellowship under award AST-0901646. BAW was supported by NASA through the Spitzer Space Telescope Theoretical Research Programs, through a contract issued by the JPL/Caltech under a contract with NASA. RDG was supported by NASA through contracts no. 1256406 and 1215746 issued by JPL/Caltech to the University of Minnesota. NR 99 TC 70 Z9 70 U1 2 U2 4 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD AUG 1 PY 2010 VL 406 IS 2 BP 952 EP 974 DI 10.1111/j.1365-2966.2010.16792.x PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 636EE UT WOS:000280710300017 ER PT J AU Rabl, P Kolkowitz, SJ Koppens, FHL Harris, JGE Zoller, P Lukin, MD AF Rabl, P. Kolkowitz, S. J. Koppens, F. H. L. Harris, J. G. E. Zoller, P. Lukin, M. D. TI A quantum spin transducer based on nanoelectromechanical resonator arrays SO NATURE PHYSICS LA English DT Article ID NUCLEAR-SPIN; TRAPPED IONS; MULTIPARTICLE ENTANGLEMENT; QUBITS; COMPUTER; DIAMOND; STATES; ELECTRON; DYNAMICS AB Isolated electronic and nuclear spins in solids are at present being actively explored for potential quantum-computing applications. Spin degrees of freedom provide an excellent quantum memory, owing to their weak magnetic interactions with the environment. For the same reason, however, it is difficult to achieve controlled interactions of spins over distances larger than tens of nanometres. Here we propose a new realization of a quantum data bus for spin qubits where spins are coupled to the motion of magnetized mechanical resonators through magnetic-field gradients. Provided that the mechanical system is charged, the magnetic moments associated with spin qubits can be effectively amplified to enable a coherent spin-spin coupling over long distances through Coulomb forces. Our approach is applicable to a wide class of electronic spin qubits, which can be localized near magnetized tips and can be used for the implementation of hybrid quantum-computing architectures. C1 [Rabl, P.; Lukin, M. D.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Kolkowitz, S. J.; Koppens, F. H. L.; Lukin, M. D.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Harris, J. G. E.] Yale Univ, Dept Phys & Appl Phys, New Haven, CT 06520 USA. [Zoller, P.] Austrian Acad Sci, Inst Quantum Opt & Quantum Informat, A-6020 Innsbruck, Austria. [Zoller, P.] Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria. RP Rabl, P (reprint author), Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. EM prabl@cfa.harvard.edu RI Rabl, Peter/F-2810-2012; Zoller, Peter/O-1639-2014; OI Rabl, Peter/0000-0002-2560-8835; Zoller, Peter/0000-0003-4014-1505; Koppens, Frank/0000-0001-9764-6120 FU ITAMP; NSF; CUA; DARPA; Packard Foundation; SFB FOQUS; EU Networks FX We gratefully acknowledge discussion with M. Aspelmeyer and K. Schwab. This work is supported by ITAMP, NSF, CUA, DARPA and the Packard Foundation. P.Z. acknowledges support by SFB FOQUS and EU Networks. NR 50 TC 178 Z9 180 U1 6 U2 46 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 1745-2473 J9 NAT PHYS JI Nat. Phys. PD AUG PY 2010 VL 6 IS 8 BP 602 EP 608 DI 10.1038/NPHYS1679 PG 7 WC Physics, Multidisciplinary SC Physics GA 634DI UT WOS:000280559300017 ER PT J AU Baeza, JA AF Antonio Baeza, J. TI The symbiotic lifestyle and its evolutionary consequences: social monogamy and sex allocation in the hermaphroditic shrimp Lysmata pederseni SO NATURWISSENSCHAFTEN LA English DT Article DE Sex allocation; Monogamy; Symbiosis; Hermaphrodite; Caribbean; Sponge; Lysmata ID PROTANDRIC SIMULTANEOUS HERMAPHRODITISM; CORAL-REEF FISH; MARINE SHRIMP; WURDEMANNI CARIDEA; SPERM COMPETITION; MATING TACTICS; SIZE; HIPPOLYTIDAE; DECAPODA; SYSTEM AB Sex allocation theory predicts female-biased sex allocation for simultaneous hermaphrodites with a monogamous mating system. Mating systems theory predicts that monogamy is advantageous in environments where refuges are discrete, scarce, relatively small, and when predation risk is high outside of these refuges. These predictions were tested with the Caribbean shrimp Lysmata pederseni, a simultaneous hermaphrodite which has an early male phase and lives inside tubes of the sponge Callyspongia vaginalis. This host sponge is a scarce resource that, together with the high predation risk typical of tropical environments, should favor monogamy in the shrimp. Field observations demonstrated that shrimps were frequently encountered as pairs within these tube sponges. Pairs were equally likely to comprise two hermaphrodites or one hermaphrodite and one male. Several of these pairs were observed for long periods of time in the field. Experiments demonstrated that hermaphrodites tolerated other hermaphrodites but not males in their host sponge. These results suggest that pairs of hermaphroditic L. pederseni are socially monogamous; they share the same host individual and might reproduce exclusively with their host partners for long periods of time. Nevertheless, males appeared less likely to establish long-term associations with hermaphrodites as indicated by the rate of their disappearance from their hosts ( greater than that of hermaphrodites). Sex allocation was female biased in monogamous hermaphrodites. On average, hermaphrodites invested 34 times more to female than to male reproductive structures. Monogamy and female-biased sex allocation seem to be evolutionary consequences of adopting a symbiotic lifestyle in simultaneous hermaphrodites. C1 [Antonio Baeza, J.] Univ Catolica Norte, Fac Ciencias Mar, Dept Biol Marina, Larrondo 1281, Coquimbo, Chile. [Antonio Baeza, J.] Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. [Antonio Baeza, J.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Baeza, JA (reprint author), Univ Catolica Norte, Fac Ciencias Mar, Dept Biol Marina, Larrondo 1281, Coquimbo, Chile. EM baezaa@si.edu OI Baeza, Juan Antonio/0000-0002-2573-6773 FU Marine Science Network; National Geographic Society FX Many thanks to Sherry Reed and Carla Piantoni for their great help during sampling and to Mike Carpenter for his patience with the scheduling of trips to Carrie Bow, Belize. Special thanks go to Tuck Hines and Valerie Paul for funding traveling to the various sampling localities. This research was funded by a Marine Science Network Grant (Smithsonian Institution) through the Johnson and Hunterdon Oceanographic Research Endowment and by a Committee for Research and Exploration Grant of the National Geographic Society. Drs. Sven Thatje, John Lawrence, and James J. Roper and three anonymous referees critically reviewed the English as well as the content and provided very helpful comments. This is contribution number 826 and 865 of the SMSFP and the CCRE, respectively. NR 56 TC 19 Z9 20 U1 1 U2 15 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0028-1042 EI 1432-1904 J9 NATURWISSENSCHAFTEN JI Naturwissenschaften PD AUG PY 2010 VL 97 IS 8 BP 729 EP 741 DI 10.1007/s00114-010-0689-4 PG 13 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 630LE UT WOS:000280273800005 PM 20552156 ER PT J AU Jonsson, P Primack, JR AF Jonsson, Patrik Primack, Joel R. TI Accelerating dust temperature calculations with graphics-processing units SO NEW ASTRONOMY LA English DT Article DE Dust; Radiative transfer; Methods: numerical ID RADIATIVE-TRANSFER CODE; N-BODY SIMULATIONS; DIRTY MODEL; EMISSION; DISTRIBUTIONS; EXTINCTION AB When calculating the infrared spectral energy distributions (SEDs) of galaxies in radiation-transfer models, the calculation of dust grain temperatures is generally the most time-consuming part of the calculation. Because of its highly parallel nature, this calculation is perfectly suited for massively parallel general-purpose graphics-processing units (GPUs). This paper presents an implementation of the calculation of dust grain equilibrium temperatures on GPUs in the Monte-Carlo radiation transfer code SUNRISE, using the CUDA API. The GPU can perform this calculation 69 times faster than the eight CPU cores, showing great potential for accelerating calculations of galaxy SEDs. (C) 2009 Elsevier B.V. All rights reserved. C1 [Jonsson, Patrik; Primack, Joel R.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. RP Jonsson, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-51, Cambridge, MA 02138 USA. EM pjonsson@cfa.harvard.edu; joel@scipp.ucsc.edu OI Primack, Joel/0000-0001-5091-5098 FU Nvidia Professor Partnership Program [C1060]; Jet Propulsion Laboratory [30183]; NASA [HST-AR-10958 -11758, NAS5-26555] FX The Nvidia Professor Partnership Program kindly donated a Tesla C1060 in support of this project, and we thank David Luebke, Chris Henze, and Chris Hayward for discussions about how to port various parts of SUNRISE to GPUs. We also thank the anonymous referee for constructive comments that helped both the clarity of the presentation and the efficiency of the calculation. PJ was supported by Spitzer Theory Grant 30183 from the Jet Propulsion Laboratory and by programs HST-AR-10958 & -11758, provided by NASA through grants from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. NR 19 TC 28 Z9 28 U1 1 U2 1 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1384-1076 EI 1384-1092 J9 NEW ASTRON JI New Astron. PD AUG PY 2010 VL 15 IS 6 BP 509 EP 514 DI 10.1016/j.newast.2009.12.008 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 597IX UT WOS:000277751400002 ER PT J AU Balunas, MJ Kinghorn, AD AF Balunas, Marcy J. Kinghorn, A. Douglas TI Natural Compounds with Aromatase Inhibitory Activity: An Update SO PLANTA MEDICA LA English DT Review DE breast cancer; aromatase; natural compounds; plants; marine organisms; fungi ID LUPULUS L. FLAVONOIDS; BREAST-CANCER CELLS; 17-BETA-HYDROXYSTEROID-DEHYDROGENASE ACTIVITIES; CONSTITUENTS; EXPRESSION; GROWTH; DERIVATIVES; MODULATION; THERAPY; HEALTH AB Several synthetic aromatase inhibitors are currently in clinical use for the treatment of postmenopausal women with hormone-receptor positive breast cancer. However, these treatments may lead to untoward side effects and so the search for new aromatase inhibitors continues, especially those for which the activity is promoter-specific, targeting the breast-specific promoters I.3 and II. Recently, numerous natural compounds have been found to inhibit aromatase in noncellular, cellular, and in vivo studies. These investigations, covering the last two years, as well as additional studies that have focused on the evaluation of natural compounds as promoter-specific aromatase inhibitors or as aromatase inducers, are described in this review. C1 [Balunas, Marcy J.] Sch Pharm, Div Med Chem, Dept Pharmaceut Sci, Storrs, CT 06269 USA. Univ Calif San Diego, Ctr Marine Biotechnol & Biomed, Scripps Inst Oceanog, San Diego, CA 92103 USA. Inst Invest Cient, Clayton, Panama. Serv Alta Tecnol, Clayton, Panama. Smithsonian Trop Res Inst, Ancon, Panama. Ohio State Univ, Coll Pharm, Div Med Chem & Pharmacognosy, Columbus, OH 43210 USA. RP Balunas, MJ (reprint author), Sch Pharm, Div Med Chem, Dept Pharmaceut Sci, 69 N Eagleville Rd,Unit 3092, Storrs, CT 06269 USA. EM marcy.balunas@uconn.edu OI Kinghorn, A. Douglas/0000-0002-6647-8707 FU The Ohio State University Comprehensive Cancer Center Molecular Carcinogenesis; Chemoprevention Program; NIH [R01 CA73698]; NCI, NIH [P01 CA48112] FX Funding for research described in this review that was carried out at The Ohio State University was supported, in part, by The Ohio State University Comprehensive Cancer Center Molecular Carcinogenesis and Chemoprevention Program, awarded to A.D.K. We are grateful to Dr. Robert W. Brueggemeier, College of Pharmacy, The Ohio State University, for his collaboration in these studies, through NIH grant R01 CA73698 (to R. W. Brueggemeier). The collection of Brassaoipsis glomerulata studied by the authors was funded through program project P01 CA48112 (Principal Investigator, J.M. Pezzuto), awarded by NCI, NIH. This review was written while M.J.B. was supported through a NIH Fogarty International Center (FIC) International Research Scientist Development Award (IRSDA) K01 award (TW008002). NR 44 TC 19 Z9 21 U1 0 U2 13 PU GEORG THIEME VERLAG KG PI STUTTGART PA RUDIGERSTR 14, D-70469 STUTTGART, GERMANY SN 0032-0943 J9 PLANTA MED JI Planta Med. PD AUG PY 2010 VL 76 IS 11 BP 1087 EP 1093 DI 10.1055/s-0030-1250169 PG 7 WC Plant Sciences; Chemistry, Medicinal; Integrative & Complementary Medicine; Pharmacology & Pharmacy SC Plant Sciences; Pharmacology & Pharmacy; Integrative & Complementary Medicine GA 631TK UT WOS:000280370900007 PM 20635310 ER PT J AU Lehner, MJ Coehlo, NK Zhang, ZW Bianco, FB Wang, JH Rice, JA Protopapas, P Alcock, C Axelrod, T Byun, YI Chen, WP Cook, KH de Pater, I Kim, DW King, SK Lee, T Marshall, SL Schwamb, ME Wang, SY Wen, CY AF Lehner, M. J. Coehlo, N. K. Zhang, Z. -W. Bianco, F. B. Wang, J. -H. Rice, J. A. Protopapas, P. Alcock, C. Axelrod, T. Byun, Y. -I. Chen, W. P. Cook, K. H. de Pater, I. Kim, D. -W. King, S. -K. Lee, T. Marshall, S. L. Schwamb, M. E. Wang, S. -Y. Wen, C. -Y. TI The TAOS Project: Statistical Analysis of Multi-Telescope Time Series Data SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID KUIPER-BELT OBJECTS; AMERICAN OCCULTATION SURVEY; STELLAR OCCULTATIONS; OORT CLOUD; SEARCH; STARS AB The Taiwanese-American Occultation Survey (TAOS) monitors fields of up to similar to 1000 stars at 5 Hz simultaneously with four small telescopes to detect occultation events from small (similar to 1 km) Kuiper Belt Objects (KBOs). The survey presents a number of challenges, in particular the fact that the occultation events we are searching for are extremely rare and are typically manifested as slight flux drops for only one or two consecutive time series measurements. We have developed a statistical analysis technique to search the multi-telescope data set for simultaneous flux drops which provides a robust false-positive rejection and calculation of event significance. In this article, we describe in detail this statistical technique and its application to the TAOS data set. C1 [Lehner, M. J.; Zhang, Z. -W.; Wang, J. -H.; King, S. -K.; Lee, T.; Wang, S. -Y.; Wen, C. -Y.] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. [Lehner, M. J.; Bianco, F. B.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Lehner, M. J.; Bianco, F. B.; Protopapas, P.; Alcock, C.; Kim, D. -W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Coehlo, N. K.; Rice, J. A.] Univ Calif Berkeley, Dept Stat, Berkeley, CA 94720 USA. [Zhang, Z. -W.; Wang, J. -H.; Chen, W. P.] Natl Cent Univ, Inst Astron, Jhongli 320, Taoyuan County, Taiwan. [Bianco, F. B.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Bianco, F. B.] Las Cumbres Observ Global Telescope Network Inc, Santa Barbara, CA 93117 USA. [Protopapas, P.; Kim, D. -W.] Harvard Univ, Initiat Innovat Comp, Cambridge, MA 02138 USA. [Axelrod, T.] Steward Observ, Tucson, AZ 85721 USA. [Byun, Y. -I.; Kim, D. -W.] Yonsei Univ, Dept Astron, Seoul 120749, South Korea. [Cook, K. H.; Marshall, S. L.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94550 USA. [de Pater, I.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Marshall, S. L.] Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA. [Schwamb, M. E.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. RP Lehner, MJ (reprint author), Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 106, Taiwan. EM mlehner@asiaa.sinica.edu.tw RI Lee, Typhoon/N-8347-2013; OI Lehner, Matthew/0000-0003-4077-0985 FU National Science Foundation [AS-88-TP-A02, DMS-0636667, AST-0501681, NNG04G113G]; National Central University [NSC 96-2112-M-008-024-MY3] FX This work was supported in part by the thematic research program AS-88-TP-A02 at Academia Sinica. N. K. C.'s work was supported in part by the National Science Foundation under grant DMS-0636667. Work at the Harvard College Observatory was supported in part by the National Science Foundation under grant AST-0501681 and by NASA under grant NNG04G113G. The work at National Central University was supported by the grant NSC 96-2112-M-008-024-MY3. J. A. R.'s work was supported in part by the National Science Foundation under grant AST-00507254. S. L. M.'s work was performed under the auspices of the US Department of Energy by Lawrence Livermore National Laboratory in part under Contract W-7405-Eng-48 and by Stanford Linear Accelerator Center under Contract DE-AC02-76SF00515. Y. I. B. acknowledges the support of National Research Foundation of Korea through Grant 2009-0075376. K. H. C.'s work was performed under the auspices of the US Department of Energy by Lawrence Livermore National Laboratory in part under Contract W-7405-Eng-48 and in part under Contract DE-AC52-07NA27344. NR 27 TC 6 Z9 6 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6280 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD AUG PY 2010 VL 122 IS 894 BP 959 EP 975 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 634EG UT WOS:000280561700010 ER PT J AU Lutikov, OA Temkin, IE Shurygin, BN AF Lutikov, O. A. Temkin, I. E. Shurygin, B. N. TI Phylogeny and evolution of ontogeny of the family Oxytomidae Ichikawa, 1958 (Mollusca: Bivalvia) SO STRATIGRAPHY AND GEOLOGICAL CORRELATION LA English DT Article DE bivalves; Oxytomidae; taxonomy; ontogeny; phylogeny; Mesozoic AB We described ontogenies and reconstructed morphogeneses of hinges in some supraspecific taxa of the bivalve family Oxytomidae Ichikawa, 1958 from the Mesozoic of Russia. The phylogeny of the family is reconstructed using evolutionary and cladistic methods. The appearance of the endemic genus Arctotis Bodylevsky, 1960 in the epicontinental seas of Siberia can be explained in terms of gradual transformations of the ligament and byssal apparatus in the Northern Siberian members of Praemeleagrinella Lutikov et Shurygin, 2009 and Praearctotis Lutikov et Shurygin, 2009. C1 [Lutikov, O. A.] Sci Res Inst Paleontol Stratig & Sedimentol, St Petersburg, Russia. [Temkin, I. E.] Smithsonian Inst, Washington, DC 20013 USA. [Temkin, I. E.] Amer Museum Nat Hist, Div Invertebrate Zool, New York, NY 10024 USA. [Shurygin, B. N.] Russian Acad Sci, Siberian Branch, Inst Petr Geol & Geophys, Novosibirsk 630090 90, Russia. RP Lutikov, OA (reprint author), Sci Res Inst Paleontol Stratig & Sedimentol, St Petersburg, Russia. EM niipss@mail.ru; ilya_temkin@hotmail.com; ShuryginBN@ipgg.nsc.ru FU Russian Foundation for Basic Research [09-05-136]; Russian Academy of Sciences [15, 17 ONZ] FX The study was supported by grant no. 09-05-136 of the Russian Foundation for Basic Research and by Programs 15 and 17 ONZ, Russian Academy of Sciences. NR 23 TC 1 Z9 1 U1 1 U2 2 PU MAIK NAUKA/INTERPERIODICA/SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013-1578 USA SN 0869-5938 J9 STRATIGR GEO CORREL+ JI Stratigr. Geol. Correl. PD AUG PY 2010 VL 18 IS 4 BP 376 EP 391 DI 10.1134/S0869593810040027 PG 16 WC Geology; Paleontology SC Geology; Paleontology GA 640MZ UT WOS:000281057000002 ER PT J AU Dorr, LJ Wiersema, JH AF Dorr, Laurence J. Wiersema, John H. TI Names of American vascular plants published in Loefling's Iter Hispanicum (1758) and its German translation (1766) SO TAXON LA English DT Editorial Material DE Iter Hispanicum; Alexander Bernhard Kolpin; Carl Linnaeus; Pehr Loefling; South America; Venezuela ID THEOPHRASTACEAE; REVISION AB Loefling's Iter Hispanicum (1758) and its subsequent translations, editions, issues, and facsimiles are analyzed for their impact on the nomenclature of American vascular plants. The book, edited by Linnaeus and posthumously published, contains descriptions of plants found in Venezuela (as well as in the Iberian Peninsula). For American plants the original volume (1758) is the source of 31 new genera, 15 new species, and one replaced name, and a German translation (1766) is the source of an additional two new species. Many of these nomenclatural innovations have been ignored, overlooked, or intentionally suppressed, some for centuries. Other names in the her Hispanicum have been misinterpreted. We examine the reasons for considering these 49 names to be validly published and the nomenclatural ramifications. In the interests of nomenclatural stability we are forced to conclude that the names of at least ten taxa described by Loefling should be rejected: Ayenia sidiformis Loefl., Cofer Loefl., Cruzeta Loefl., Cruzeta hispanica Loefl., Edechia inermis Loefl., E. spinosa L. Justicia putata Loefl., Menais Loefl., Muco Loefl., and Samyda parviflora Loefl. Likewise the names of two species described by Linnaeus that are tied to the her Hispanicum should be rejected: Menais topiaria L. and Spermacoce suffruticosa L. Finally, we select neotypes for Gaura fruticosa Loefl., Salvinia michelii Loefl., and Waltheria melochioides Loefl. C1 [Dorr, Laurence J.] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. [Wiersema, John H.] USDA ARS, BARC W, Natl Germplasm Resources Lab, Beltsville, MD 20705 USA. RP Dorr, LJ (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, MRC 166,POB 37012, Washington, DC 20013 USA. EM dorrl@si.edu NR 107 TC 3 Z9 3 U1 0 U2 0 PU INT ASSOC PLANT TAXONOMY PI VIENNA PA C/O UNIV VIENNA, INST BOTANY, RENNWEG 14, A-1030 VIENNA, AUSTRIA SN 0040-0262 J9 TAXON JI Taxon PD AUG PY 2010 VL 59 IS 4 BP 1245 EP 1262 PG 18 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA 637YJ UT WOS:000280854300022 ER PT J AU Stringer, CE Rains, MC Kruse, S Whigham, D AF Stringer, Christina E. Rains, Mark C. Kruse, Sarah Whigham, Dennis TI Controls on Water Levels and Salinity in a Barrier Island Mangrove, Indian River Lagoon, Florida SO WETLANDS LA English DT Article DE Conductivity; Electrical resistivity; Evapotranspiration; Hypersalinity; Salt pan ID NUTRIENT ENRICHMENT; RHIZOPHORA-MANGLE; RED MANGROVE; GROWTH; DEUTERIUM; RESPONSES; SEEDLINGS; DYNAMICS; ESTUARY; FOREST AB We examined controls on water levels and salinity in a mangrove on a carbonate barrier island along the Indian River Lagoon, east-central Florida. Piezometers were installed at 19 sites throughout the area. Groundwater was sampled at 17 of these sites seasonally for three years. Head measurements were taken at the other two sites at 15-minute intervals for one year. Water levels in the mangrove are almost always lower than lagoon water levels. Spectral analysis of water levels showed that mangrove groundwater levels are not tidally influenced. Salinities vary spatially, with values of similar to 10 psu in uplands, similar to 30 psu in regularly-flushed mangroves, and similar to 75 psu in irregularly-flushed mangroves. Cation and anion concentrations and stable isotope compositions indicate that water salinities are largely controlled by enrichment due to evapotranspiration. A shore-perpendicular electrical resistivity survey showed that the freshwater lens is restricted to uplands and that hypersaline waters extend deeply below the mangrove. These results indicate that evapotranspiration lowers water levels in the mangrove, which causes Indian River Lagoon water to flow into the mangrove where it evapoconcentrates and descends, forming a thick layer of high-salinity water below the mangrove. C1 [Stringer, Christina E.; Rains, Mark C.; Kruse, Sarah] Univ S Florida, Dept Geol, Tampa, FL 33620 USA. [Whigham, Dennis] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Stringer, CE (reprint author), Univ S Florida, Dept Geol, Tampa, FL 33620 USA. EM cestring@mail.usf.edu OI Whigham, Dennis/0000-0003-1488-820X FU Smithsonian Marine Sciences Network FX This study was supported by the Smithsonian Marine Sciences Network. This is contribution #811 from the Smithsonian Marine Station at Fort Pierce. Beth Fratesi, Kathryn Murphy, Pamela Stringer, Chris Reich, Jason Greenwood, and students in the USF Applied Geophysics course in Spring 2007 all helped with field data collection. We are grateful to Peter Swarzenski and the United States Geological Survey for the loan of the resistivity system and processing software. Jon Sumrall assisted by drafting Fig. 10. NR 39 TC 3 Z9 3 U1 1 U2 22 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0277-5212 J9 WETLANDS JI Wetlands PD AUG PY 2010 VL 30 IS 4 BP 725 EP 734 DI 10.1007/s13157-010-0072-4 PG 10 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA 646TG UT WOS:000281565300008 ER PT J AU Zhang, P Sadeghpour, HR Dalgarno, A AF Zhang, P. Sadeghpour, H. R. Dalgarno, A. TI Structure and spectroscopy of ground and excited states of LiYb SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID ALKALI-METAL ATOMS; OF-THE-ART; POLAR-MOLECULES; WAVE-FUNCTIONS; BASIS-SETS; SPIN; ENERGY; GRADIENTS; ELEMENTS; HELIUM AB Multireference configuration interaction and coupled cluster calculations have been carried out to determine the potential energy curves for the ground and low-lying excited states of the LiYb molecule. The scalar relativistic effects have been included by means of the Douglas-Kroll Hamiltonian and effective core potential and the spin-orbit couplings have been evaluated by the full microscopic Breit-Pauli operator. The LiYb permanent dipole moment, static dipole polarizability, and Franck-Condon factors have been determined. Perturbations of the vibrational spectrum due to nonadiabatic interactions are discussed. (C) 2010 American Institute of Physics. [doi:10.1063/1.3462245] C1 [Zhang, P.; Sadeghpour, H. R.; Dalgarno, A.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Dalgarno, A (reprint author), Harvard Smithsonian Ctr Astrophys, ITAMP, 60 Garden St, Cambridge, MA 02138 USA. EM adalgarno@cfa.harvard.edu FU Chemical Science, Geoscience, and Bioscience Division of the Office of Basic Energy Science, Office of Science, U.S. Department of Energy; NSF [TG-Phy 090079] FX The research of A.D. and P.Z. is supported by the Chemical Science, Geoscience, and Bioscience Division of the Office of Basic Energy Science, Office of Science, U.S. Department of Energy, and of H.R.S. by a NSF grant to ITAMP. We thank Y. Takahashi for helpful discussions and Z.-C. Yan for providing the Li atomic spectrum data. NSF Teragrid Grant No. TG-Phy 090079 was used for the computations. NR 52 TC 31 Z9 32 U1 0 U2 10 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0021-9606 J9 J CHEM PHYS JI J. Chem. Phys. PD JUL 28 PY 2010 VL 133 IS 4 AR 044306 DI 10.1063/1.3462245 PG 10 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 637YM UT WOS:000280854600025 PM 20687649 ER PT J AU Kotov, AA Ferrari, FD AF Kotov, Alexey A. Ferrari, Frank D. TI The taxonomic research of Jules Richard on Cladocera (Crustacea: Branchiopoda) and his collection at the National Museum of Natural History, USA SO ZOOTAXA LA English DT Article DE Anomopoda; Ctenopoda; systematics; taxonomy; museum collections; lectotype ID PLEUROXUS ANOMOPODA; SPECIES CLADOCERA; LEBERIS-SMIRNOV; SP-NOV; CHYDORIDAE; GENUS; REVISION; DIFFERENTIATION; MACROTHRICIDAE; REDESCRIPTION AB Jules Richard (1863-1945) contributed significantly to cladoceran taxonomy before he became Director of the Musee Oceanographique de Monaco and assistant to Prince Albert I-er de Monaco. His collection, including slides and samples preserved in ethanol, was purchased by E. A. Birge, subsequently incorporated into the collection of David G. Frey, and later gifted to the National Museum of Natural History, Smithsonian Institution. A list of publications of Richard about cladocerans is presented, as well a list of all new taxa described by him (three genera and 37 taxa of species rank), with information about type localities, synonymies and taxonomic comments. Lectotypes and in some cases paralectotypes are selected for Daphnia (Ctenodaphnia) bolivari Richard, 1888; D. (Daphnia) curvirostris insulana Moniez in Richard, 1896; Bosmina japonica Poppe & Richard, 1890; Grimaldina brazzai Richard, 1892 and Alona sarsi Richard, 1891. Syntypes exist for Alona moniezi Richard, 1888 and Pleuroxus letourneuxi (Richard, 1888). The ethanol samples of Richard that may contain species for which there are no types are discussed. In addition, samples in the collection of David G. Frey from type localities of Richard's species are noted. These samples could be important for future revisions of the Richard's taxa. A redescription of Pleuroxus letourneuxi (Chydoridae, Chydorinae) is given; Bosmina japonica Poppe & Richard, 1890 (Bosminidae), a junior synonym of B. longirostris (O. F. Muller, 1776), also is redescribed. C1 [Kotov, Alexey A.] AN Severtsov Inst Ecol & Evolut, Moscow 119071, Russia. [Ferrari, Frank D.] Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Museum Support Ctr, Suitland, MD 20746 USA. RP Kotov, AA (reprint author), AN Severtsov Inst Ecol & Evolut, Leninsky Prospect 33, Moscow 119071, Russia. EM alexey-a-kotov@yandex.ru; ferrarif@si.edu RI Kotov, Alexey/B-1549-2010 OI Kotov, Alexey/0000-0002-8863-6438 FU Russian Foundation for Basic Research [09-04-00201-a] FX The study was undertaken during two short-term visits of AAK to National Museum of Natural History supported by awards from the Office of Fellowships, Smithsonian Institution, and was supported in part by the Russian Foundation for Basic Research (grant 09-04-00201-a), Biodiversity Program of the Presidium of Russian Academy of Sciences (project 1.1.8.) and Russian Science Support Foundation (all to AAK). We are grateful to Professor H. J. Dumont for the editing of the text, Professor N. N. Smirnov and Dr K. Van Damme for valuable consultations at different phases of this investigation. We thank Dr. D. J. Taylor for sharing sequence data and interpretations; Prof. V. Korinek, Prof. D. B. Berner and Dr A. Cabrinovic provided valuable information about the taxonomic status and location of specimens. Dr. D. M. Damkaer provided access to an unpublished manuscript chapter on Jules Richard. NR 85 TC 10 Z9 11 U1 0 U2 4 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD JUL 28 PY 2010 IS 2551 BP 37 EP 64 PG 28 WC Zoology SC Zoology GA 632EF UT WOS:000280402900002 ER PT J AU Burns, JM Janzen, DH Hallwachs, W Hajibabaei, M Hebert, PDN AF Burns, John M. Janzen, Daniel H. Hallwachs, Wnnie Hajibabaei, Mehrdad Hebert, Paul D. N. TI GENITALIA, DNA BARCODES, LARVAL FACIES, AND FOODPLANTS PLACE THE MIMETIC SPECIES NEOXENIADES MOLION IN RHINTHON (HESPERIIDAE: HESPERIINAE) SO JOURNAL OF THE LEPIDOPTERISTS SOCIETY LA English DT Article DE mimicry; Rhinthon molion; new combination; secondary sex character; Zingiberales; Marantaceae ID SKIPPER BUTTERFLIES; GENUS AB Fades can fool taxonomists as well as predators. Neoxeniades motion (Codman)-one of the many, large neotropical skippers in the major mimicry group that includes all the cryptic species of the Astraptes fidget-at-or complex is misclassified. It really relates to a species of Rhinthon that differs greatly from it in facies and size. In both sexes, the genitalia of Rhinthon motion, new combination, and R. once (Plotz) are nearly identical, even down to a peculiar titillator on the left side of the aedeagus of the male. Males also share a secondary sex character along vein 2A of the forewing. DNA barcodes unite R. once and R. motion in a tight, two-taxon cluster: their sequence divergence is about 3.5%. Caterpillars of the two species are alike but distinguishable, and, in Costa Rica, they have been found feeding on various native species of Marantaceae-seven of which are the same and also on one and the same introduced species of Cannaceae (these are closely related plant families grouped in the order Zingiberales). Because Rhinthon is widespread and relatively speciose in Central and South America, it can no longer be considered a genus primarily of the Greater Antilles. DNA barcodes, which are useful for identifying known species and for indicating possible cryptic species, are useful in this study (in combination with other, more traditional, taxonomic characters) for pulling suppo sedly unrelated species together into the same genus. C1 [Burns, John M.] Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, Washington, DC 20013 USA. [Janzen, Daniel H.; Hallwachs, Wnnie] Univ Penn, Dept Biol, Philadelphia, PA 19104 USA. [Hajibabaei, Mehrdad; Hebert, Paul D. N.] Univ Guelph, Dept Integrat Biol, Guelph, ON N1G 2W1, Canada. RP Burns, JM (reprint author), Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, POB 37012,MRC 127,Room E-515, Washington, DC 20013 USA. EM burnsj@si.edu; djanzen@sas.upenn.edu; whallwac@sas.upenn.edu; mhajibab@uoguelph.ca; phebert@uoguelph.ca RI Hebert, Paul/C-4161-2013 OI Hebert, Paul/0000-0002-3081-6700 FU National Museum of Natural History; National Science Foundation [BSR 9024770, DEB 9306296, 9400829, 9705072, 0072730, 0515699]; Gordon and Betty Moore Foundation; Genome Canada through the Ontario Genomics Institute FX We thank Donald Harvey for dissecting genitalia and Young Sohn for drawing them, Kane Darrow for photographing adults and their secondary sex character and for setting the table and plates, ACG parataxonomists for finding caterpillars and rearing adults, Tanya Dapkey for plucking and shipping LEGS AWAY/FOR DNA (capitals denote the two-line, printed, black-on-yellow label affixed to adult specimens delegged for barcoding), and Olaf Mielke for reviewing the manuscript. Support for this study came from the National Museum of Natural History Small Grants Program (J.M.B.); from National Science Foundation grants BSR 9024770 and DEB 9306296, 9400829, 9705072, 0072730, and 0515699 (D.H.J.); and from grants from the Gordon and Betty Moore Foundation and Genome Canada through the Ontario Genomics Institute (P.D.N.H.). NR 13 TC 6 Z9 7 U1 0 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 JUL 27 PY 2010 VL 64 IS 2 BP 69 EP 78 PG 10 WC Entomology SC Entomology GA 633JI UT WOS:000280497600002 ER PT J AU Kurka, M Feist, J Horner, DA Rudenko, A Jiang, YH Kuhnel, KU Foucar, L Rescigno, TN McCurdy, CW Pazourek, R Nagele, S Schulz, M Herrwerth, O Lezius, M Kling, MF Schoffler, M Belkacem, A Dusterer, S Treusch, R Schneider, BI Collins, LA Burgdorfer, J Schroter, CD Moshammer, R Ullrich, J AF Kurka, M. Feist, J. Horner, D. A. Rudenko, A. Jiang, Y. H. Kuehnel, K. U. Foucar, L. Rescigno, T. N. McCurdy, C. W. Pazourek, R. Nagele, S. Schulz, M. Herrwerth, O. Lezius, M. Kling, M. F. Schoeffler, M. Belkacem, A. Duesterer, S. Treusch, R. Schneider, B. I. Collins, L. A. Burgdoerfer, J. Schroeter, C. D. Moshammer, R. Ullrich, J. TI Differential cross sections for non-sequential double ionization of He by 52 eV photons from the Free Electron Laser in Hamburg, FLASH SO NEW JOURNAL OF PHYSICS LA English DT Article ID 2-PHOTON DOUBLE-IONIZATION; EXTREME-ULTRAVIOLET; COHERENT RADIATION; HELIUM AB Two-photon double ionization of He is studied at the Free Electron Laser in Hamburg (FLASH) by inspecting He(2+) momentum ((P) over right arrow (He(2+))) distributions at 52 eV photon energy. We demonstrate that recoil ion momentum distributions can be used to infer information about highly correlated electron dynamics and find the first experimental evidence for 'virtual sequential ionization'. The experimental data are compared with the results of two calculations, both solving the time-dependent Schrodinger equation. We find good overall agreement between experiment and theory, with significant differences for cuts along the polarization direction that cannot be explained by the experimental resolution alone. C1 [Kurka, M.; Rudenko, A.; Jiang, Y. H.; Kuehnel, K. U.; Foucar, L.; Schroeter, C. D.; Moshammer, R.; Ullrich, J.] Max Planck Inst Kernphys, D-69117 Heidelberg, Germany. [Kurka, M.; Rudenko, A.; Foucar, L.; Ullrich, J.] CFEL, Max Planck Adv Study Grp, D-22607 Hamburg, Germany. [Feist, J.; Pazourek, R.; Nagele, S.; Burgdoerfer, J.] Vienna Univ Technol, Inst Theoret Phys, A-1040 Vienna, Austria. [Feist, J.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. [Horner, D. A.; Collins, L. A.] Los Alamos Natl Lab, Div Theoret, Los Alamos, NM 87545 USA. [Rescigno, T. N.; McCurdy, C. W.; Schoeffler, M.; Belkacem, A.] Univ Calif Berkeley, Lawrence Berkeley Lab, Chem Sci & Ultrafast Xray Sci Lab, Berkeley, CA 94720 USA. [McCurdy, C. W.] Univ Calif Davis, Dept Appl Sci, Davis, CA 95616 USA. [McCurdy, C. W.] Univ Calif Davis, Dept Chem, Davis, CA 95616 USA. [Schulz, M.] Missouri Univ Sci & Technol, Dept Phys, Rolla, MO 65409 USA. [Schulz, M.] LAMOR, Rolla, MO 65409 USA. [Herrwerth, O.; Lezius, M.; Kling, M. F.] Max Planck Inst Quantum Opt, D-85748 Garching, Germany. [Duesterer, S.; Treusch, R.] DESY, D-22607 Hamburg, Germany. [Schneider, B. I.] Natl Sci Fdn, Div Phys, Off Cyberinfrastruct, Arlington, VA 22230 USA. [Schneider, B. I.] NIST, Div Electron & Opt Phys, Gaithersburg, MD 20899 USA. RP Kurka, M (reprint author), Max Planck Inst Kernphys, D-69117 Heidelberg, Germany. EM moritz.kurka@mpi-hd.mpg.de RI Nagele, Stefan/E-6938-2011; Rudenko, Artem/C-7412-2009; Feist, Johannes/J-7394-2012; Kling, Matthias/D-3742-2014; Schoeffler, Markus/B-6261-2008; Treusch, Rolf/C-3935-2015 OI Nagele, Stefan/0000-0003-1213-0294; Rudenko, Artem/0000-0002-9154-8463; Feist, Johannes/0000-0002-7972-0646; Treusch, Rolf/0000-0001-8479-8862; Schoeffler, Markus/0000-0001-9214-6848; FU Max-Planck Advanced Study Group at CFEL; DFG [JI 110/2-1]; US DOE; OBES, Division of Chemical Sciences [DE-AC02-05CH11231]; NSF [PHY-0604628]; FWF-Austria [SFB016] FX The authors are greatly indebted to the scientific and technical team at FLASH, in particular, the machine operators and run coordinators, striving for optimal beamtime conditions. Support from the Max-Planck Advanced Study Group at CFEL is gratefully acknowledged. YHJ acknowledges support from DFG project no. JI 110/2-1. Work at LBNL was performed under the auspices of the US DOE and supported by the OBES, Division of Chemical Sciences under contract no. DE-AC02-05CH11231. CWM acknowledges support from the NSF (grant no. PHY-0604628). The V team acknowledges support from the NSF TeraGrid computational facilities at the Texas Advanced Computing Center (TACC) and at the National Institute for Computational Science (NICS), and institutional computing resources at Los Alamos National Laboratory for computer time to perform the computations. Work at Vienna University of Technology was supported by the FWF-Austria (grant no. SFB016). JF acknowledges support from the NSF through a grant to ITAMP. OH, ML and MFK acknowledge support from the DFG via the Emmy-Noether programme and the Cluster of Excellence: Munich Centre for Advanced Photonics. NR 48 TC 37 Z9 37 U1 0 U2 17 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 1367-2630 J9 NEW J PHYS JI New J. Phys. PD JUL 27 PY 2010 VL 12 AR 073035 DI 10.1088/1367-2630/12/7/073035 PG 17 WC Physics, Multidisciplinary SC Physics GA 642RG UT WOS:000281233600002 ER PT J AU Pritchard, JR Loeb, A AF Pritchard, Jonathan R. Loeb, Abraham TI Constraining the unexplored period between the dark ages and reionization with observations of the global 21 cm signal SO PHYSICAL REVIEW D LA English DT Article ID HIGH-REDSHIFT; PARAMETER-ESTIMATION; INTERGALACTIC MEDIUM; EPOCH; RADIATION; MHZ; FOREGROUNDS; BRIGHTNESS; EMISSION AB Observations of the frequency dependence of the global brightness temperature of the redshifted 21 cm line of neutral hydrogen may be possible with single dipole experiments. In this paper, we develop a Fisher matrix formalism for calculating the sensitivity of such instruments to the 21 cm signal from reionization and the dark ages. We show that rapid reionization histories with duration Delta z less than or similar to 2 can be constrained, provided that local foregrounds can be well modeled by low order polynomials. It is then shown that observations in the range nu = 50-100 MHz can feasibly constrain the Ly alpha and x-ray emissivity of the first stars forming at z similar to 15-25, provided that systematic temperature residuals can be controlled to less than 1 mK. Finally, we demonstrate the difficulty of detecting the 21 cm signal from the dark ages before star formation. C1 [Pritchard, Jonathan R.; Loeb, Abraham] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Pritchard, JR (reprint author), Harvard Smithsonian Ctr Astrophys, MS-51,60 Garden St, Cambridge, MA 02138 USA. EM jpritchard@cfa.harvard.edu OI Pritchard, Jonathan/0000-0003-4127-5353 FU NASA through the Space Telescope Science Institute [HST-HF-01211.01-A, NAS 5-26555, NNA09DB30A, NNX08AL43G]; NSF [AST-0907890] FX We would like to thank J. Bowman and A. de Oliveira-Costa for useful conversations. Figure 3 was generated using HEALPIX [48] and the global sky model software of Ref. [32]. J. R. P. is supported by NASA under Hubble Grant No. HST-HF-01211.01-A through the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under Contract No. NAS 5-26555. A. L. acknowledges funding from NSF Grant No. AST-0907890 and NASA Grant Nos. NNA09DB30A and NNX08AL43G. NR 42 TC 64 Z9 64 U1 0 U2 0 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1550-7998 J9 PHYS REV D JI Phys. Rev. D PD JUL 23 PY 2010 VL 82 IS 2 AR 023006 DI 10.1103/PhysRevD.82.023006 PG 12 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 629WW UT WOS:000280232400001 ER PT J AU Smith, AR Seid, MA Jimenez, LC Wcislo, WT AF Smith, Adam R. Seid, Marc A. Jimenez, Lissette C. Wcislo, William T. TI Socially induced brain development in a facultatively eusocial sweat bee Megalopta genalis (Halictidae) SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE brain organization; social evolution; social brain; Machiavellian intelligence; neural plasticity; mushroom bodies ID DIVISION-OF-LABOR; MUSHROOM BODIES; ECUADORIA HYMENOPTERA; VOLUME CHANGES; INSECT BRAIN; HONEYBEE; BODY; PLASTICITY; EXPERIENCE; EVOLUTION AB Changes in the relative size of brain regions are often dependent on experience and environmental stimulation, which includes an animal's social environment. Some studies suggest that social interactions are cognitively demanding, and have examined predictions that the evolution of sociality led to the evolution of larger brains. Previous studies have compared species with different social organizations or different groups within obligately social species. Here, we report the first intraspecific study to examine how social experience shapes brain volume using a species with facultatively eusocial or solitary behaviour, the sweat bee Megalopta genalis. Serial histological sections were used to reconstruct and measure the volume of brain areas of bees behaving as social reproductives, social workers, solitary reproductives or 1-day-old bees that are undifferentiated with respect to the social phenotype. Social reproductives showed increased development of the mushroom body (an area of the insect brain associated with sensory integration and learning) relative to social workers and solitary reproductives. The gross neuroanatomy of young bees is developmentally similar to the advanced eusocial species previously studied, despite vast differences in colony size and social organization. Our results suggest that the transition from solitary to social behaviour is associated with modified brain development, and that maintaining dominance, rather than sociality per se, leads to increased mushroom body development, even in the smallest social groups possible (i.e. groups with two bees). Such results suggest that capabilities to navigate the complexities of social life may be a factor shaping brain evolution in some social insects, as for some vertebrates. C1 [Smith, Adam R.; Seid, Marc A.; Jimenez, Lissette C.; Wcislo, William T.] Smithsonian Trop Res Inst, Balboa, Panama. [Smith, Adam R.; Seid, Marc A.; Jimenez, Lissette C.; Wcislo, William T.] MRC 0580 12, Unit 9100, Dpo, AA 34002 USA. RP Smith, AR (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Panama. EM arsmith2@gmail.com; wcislow@si.edu FU Secretaria Nacional de Ciencia y Technologia e Innovacion de la Republica de Panama (SENACYT) [COl06-003]; Smithsonian Tropical Research Institute (STRI) Laboratory of Behaviour and Evolutionary Neurobiology; Smithsonian Institution; STRI FX We thank John Douglass and Simon Tierney for helpful discussions and comments on the manuscript. Financial support was provided by grant no. COl06-003 from the Secretaria Nacional de Ciencia y Technologia e Innovacion de la Republica de Panama (SENACYT) to W. T. W. and A. R. S., the F. H. Levinson Fund through its support of the Smithsonian Tropical Research Institute (STRI) Laboratory of Behaviour and Evolutionary Neurobiology (W. T. W., principal investigator), the Smithsonian Institution's Scholarly Studies Programme (W. T. W., principal investigator) and general research funds from STRI to W. T. W. A. R. S. was supported by a Smithsonian Institution Post-doctoral fellowship during the writing of this paper. Ricardo Cossio assisted in fieldwork through STRI's internship programme. We are grateful to the Autoridad Nacional del Medio Ambiente (ANAM) of the Republic of Panama for research permits and to the STRI staff for logistical support. NR 61 TC 27 Z9 28 U1 3 U2 22 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 J9 P ROY SOC B-BIOL SCI JI Proc. R. Soc. B-Biol. Sci. PD JUL 22 PY 2010 VL 277 IS 1691 BP 2157 EP 2163 DI 10.1098/rspb.2010.0269 PG 7 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 608FX UT WOS:000278569700008 PM 20335213 ER PT J AU Yanoviak, SP Munk, Y Kaspari, M Dudley, R AF Yanoviak, Stephen P. Munk, Yonatan Kaspari, Mike Dudley, Robert TI Aerial manoeuvrability in wingless gliding ants (Cephalotes atratus) SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE aerodynamics; appendages; arboreal; behaviour; Formicidae; tropics ID TROPICAL RAIN-FOREST; CANOPY ANTS; BEHAVIOR; DESCENT; HYMENOPTERA; FORMICIDAE; ORIGINS; FLIGHT AB In contrast to the patagial membranes of gliding vertebrates, the aerodynamic surfaces used by falling wingless ants to direct their aerial descent are unknown. We conducted ablation experiments to assess the relative contributions of the hindlegs, midlegs and gaster to gliding success in workers of the Neotropical arboreal ant Cephalotes atratus (Hymenoptera: Formicidae). Removal of hindlegs significantly reduced the success rate of directed aerial descent as well as the glide index for successful flights. Removal of the gaster alone did not significantly alter performance relative to controls. Equilibrium glide angles during successful targeting to vertical columns were statistically equivalent between control ants and ants with either the gaster or the hindlegs removed. High-speed video recordings suggested possible use of bilaterally asymmetric motions of the hindlegs to effect body rotations about the vertical axis during targeting manoeuvre. Overall, the control of gliding flight was remarkably robust to dramatic anatomical perturbations, suggesting effective control mechanisms in the face of adverse initial conditions (e. g. falling upside down), variable targeting decisions and turbulent wind gusts during flight. C1 [Yanoviak, Stephen P.] Univ Arkansas, Dept Biol, Little Rock, AR 72204 USA. [Munk, Yonatan; Dudley, Robert] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. [Kaspari, Mike; Dudley, Robert] Smithsonian Trop Res Inst, Balboa, Panama. [Kaspari, Mike] Univ Oklahoma, Dept Zool, EEB Grad Program, Norman, OK 73019 USA. RP Yanoviak, SP (reprint author), Univ Arkansas, Dept Biol, 2801 S Univ Ave, Little Rock, AR 72204 USA. EM spyanoviak@ualr.edu OI Kaspari, Michael/0000-0002-9717-5768 FU National Science Foundation [IOS-0837866, IOS-0843120]; National Geographic Society [CRE 7896-05] FX We thank O. Acevedo, P. Bucur, P. Jensen and S. Madigosky for logistical support, and A. Courtemanch for assistance in the field. The Smithsonian Tropical Research Institute, the Panamanian Autoridad Nacional del Ambiente (ANAM), and the Peruvian Instituto Nacional de Recursos Naturales (INRENA) provided research permits. The Amazon Conservatory for Tropical Studies and Amazon Explorama Lodges facilitated access to field sites in Peru. Y. Zeng and A. Jusufi provided helpful comments on the manuscript. This research was supported in part by grants from the National Science Foundation (IOS-0837866 to R. D. and IOS-0843120 to S. Y.) and from the National Geographic Society (CRE 7896-05). NR 22 TC 15 Z9 15 U1 0 U2 10 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 J9 P ROY SOC B-BIOL SCI JI Proc. R. Soc. B-Biol. Sci. PD JUL 22 PY 2010 VL 277 IS 1691 BP 2199 EP 2204 DI 10.1098/rspb.2010.0170 PG 6 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 608FX UT WOS:000278569700013 PM 20236974 ER PT J AU Keto, E Zhang, QZ AF Keto, Eric Zhang, Qizhou TI The standard model of star formation applied to massive stars: accretion discs and envelopes in molecular lines SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: individual: IRAS 20126+4104; stars: massive ID (PROTO)STAR IRAS 20126+4104; RADIATIVE-TRANSFER; HII-REGIONS; OUTFLOW; IRAS-20126+4104; AMMONIA; SYSTEM; DISKS; JET; G10.6-0.4 AB We address the question of whether the formation of high-mass stars is similar to or differs from that of solar mass stars through new molecular line observations and modelling of the accretion flow around the massive protostar IRAS20126+4104. We combine new observations of NH3(1,1) and (2,2) made at the Very Large Array (VLA), new observations of CH3CN(13-12) made at the Submillimeter Array, previous VLA observations of NH3(3,3) and NH3(4,4) and previous Plateau de Bure observations of C34S(2-1), C34S(5-4) and CH3CN(12-11) to obtain a data set of molecular lines covering 15-419 K in excitation energy. We compare these observations against simulated molecular line spectra predicted from a model for high-mass star formation based on a scaled-up version of the standard disc-envelope paradigm developed for accretion flows around low-mass stars. We find that in accord with the standard paradigm, the observations require both a warm, dense, rapidly rotating disc and a cold, diffuse infalling envelope. This paper suggests that accretion processes around 10 M-circle dot stars are similar to those of solar mass stars. C1 [Keto, Eric; Zhang, Qizhou] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02420 USA. RP Keto, E (reprint author), Harvard Smithsonian Ctr Astrophys, 160 Garden St, Cambridge, MA 02420 USA. EM keto@cfa.harvard.edu; qzhang@cfa.harvard.edu OI Zhang, Qizhou/0000-0003-2384-6589 NR 39 TC 25 Z9 25 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUL 21 PY 2010 VL 406 IS 1 BP 102 EP 111 DI 10.1111/j.1365-2966.2010.16672.x PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 623TI UT WOS:000279766800029 ER PT J AU Ludlow, AD Navarro, JF Springel, V Vogelsberger, M Wang, J White, SDM Jenkins, A Frenk, CS AF Ludlow, Aaron D. Navarro, Julio F. Springel, Volker Vogelsberger, Mark Wang, Jie White, Simon D. M. Jenkins, Adrian Frenk, Carlos S. TI Secondary infall and the pseudo-phase-space density profiles of cold dark matter haloes SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: numerical; dark matter ID LAMBDA-CDM HALOES; GALAXY CLUSTERS; INNER STRUCTURE; UNIVERSE; SIMULATIONS; DEPENDENCE; EVOLUTION; COLLAPSE; REDSHIFT; SHAPE AB We use N-body simulations to investigate the radial dependence of the density, , and velocity dispersion, Sigma, in cold dark matter (CDM) haloes. In particular, we explore how closely Q equivalent to /Sigma 3, a surrogate measure of the phase-space density, follows a power law in radius. Our study extends earlier work by considering, in addition to spherically averaged profiles, local Q estimates for individual particles, Q(i); profiles based on the ellipsoidal radius dictated by the triaxial structure of the halo, Q(i)(r'); and by carefully removing substructures in order to focus on the profile of the smooth halo, Qs. The resulting Qs(i)(r') profiles follow closely a power law near the centre, but show a clear upturn from this trend near the virial radius, r(200). The location and magnitude of the deviations are in excellent agreement with the predictions from Bertschinger's spherical secondary-infall similarity solution. In this model, Q proportional to r-1.875 in the inner, virialized regions, but departures from a power-law occur near r(200) because of the proximity of this radius to the location of the first shell crossing - the shock radius in the case of a collisional fluid. Particles there have not yet fully virialized, and so Q departs from the inner power-law profile. Our results imply that the power-law nature of Q profiles only applies to the inner regions and cannot be used to predict accurately the structure of CDM haloes beyond their characteristic scale radius. C1 [Ludlow, Aaron D.] Argelander Inst Astron, D-53121 Bonn, Germany. [Ludlow, Aaron D.; Navarro, Julio F.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 5C2, Canada. [Springel, Volker; Vogelsberger, Mark; Wang, Jie; White, Simon D. M.] Max Planck Inst Astrophys, D-85740 Garching, Germany. [Vogelsberger, Mark] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Wang, Jie; Jenkins, Adrian; Frenk, Carlos S.] Univ Durham, Dept Phys, Inst Computat Cosmol, Durham DH1 3LE, England. RP Ludlow, AD (reprint author), Argelander Inst Astron, Hugel 71, D-53121 Bonn, Germany. EM aludlow@astro.uni-bonn.de OI Jenkins, Adrian/0000-0003-4389-2232 FU Canada's NSERC; Royal Society; STFC FX The simulations for the Aquarius Project were carried out at the Leibniz Computing Center, Garching, Germany, the Computing Center of the Max-Plank-Society in Garching, the Institute for Computational Cosmology in Durham, and on the 'STELLA' supercomputer of the LOFAR experiment at the University of Groningen. All other simulations were performed at the Computing Centre of the Canadian Institute for Theoretical Astrophysics in Toronto. ADL acknowledges financial support from Canada's NSERC and technical assistance from the CITA support staff. CSF acknowledges a Royal Society Wolfson Research Merit Award and financial support from an STFC rolling grant to the ICC. NR 46 TC 31 Z9 31 U1 0 U2 1 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUL 21 PY 2010 VL 406 IS 1 BP 137 EP 146 DI 10.1111/j.1365-2966.2010.16678.x PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 623TI UT WOS:000279766800032 ER PT J AU Jimenez-Serra, I Caselli, P Tan, JC Hernandez, AK Fontani, F Butler, MJ van Loo, S AF Jimenez-Serra, I. Caselli, P. Tan, J. C. Hernandez, A. K. Fontani, F. Butler, M. J. van Loo, S. TI Parsec-scale SiO emission in an infrared dark cloud SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: formation; ISM: individual objects: G035; 39-00; 33; ISM: molecules ID FILAMENTARY MOLECULAR CLOUDS; MASS STAR-FORMATION; INITIAL CONDITIONS; GALACTIC-CENTER; HELICAL FIELDS; DENSE CLOUDS; SHOCKS; OUTFLOW; PRECURSORS; CHEMISTRY AB We present high-sensitivity 2 x 4 arcmin2 maps of the J = 2 -> 1 rotational lines of SiO, CO, 13CO and C18O, observed towards the filamentary infrared dark cloud (IRDC) G035.39-00.33. Single-pointing spectra of the SiO J = 2 -> 1 and J = 3 -> 2 lines towards several regions in the filament are also reported. The SiO images reveal that SiO is widespread along the IRDC (size >= 2 pc), showing two different components: one bright and compact arising from three condensations (N, E and S) and the other weak and extended along the filament. While the first component shows broad lines (linewidths of similar to 4-7 km s-1) in both SiO J = 2 -> 1 and SiO J = 3 -> 2, the second one is only detected in SiO J = 2 -> 1 and has narrow lines (similar to 0.8 km s-1). The maps of CO and its isotopologues show that low-density filaments are intersecting the IRDC and appear to merge towards the densest portion of the cloud. This resembles the molecular structures predicted by flow-driven, shock-induced and magnetically-regulated cloud formation models. As in outflows associated with low-mass star formation, the excitation temperatures and fractional abundances of SiO towards N, E and S increase with velocity from similar to 6 to 40 K and from similar to 10-10 to >= 10-8, respectively, over a velocity range of similar to 7 km s-1. Since 8 mu m and 24 mu m sources and/or extended 4.5 mu m emission are detected in N, E and S, broad SiO is likely produced in outflows associated with high-mass protostars. The excitation temperatures and fractional abundances of the narrow SiO lines, however, are very low (similar to 9 K and similar to 10-11, respectively), and consistent with the processing of interstellar grains by the passage of a shock with v(s) similar to 12 km s-1. This emission could be generated (i) by a large-scale shock, perhaps remnant of the IRDC formation process, (ii) by decelerated or recently processed gas in large-scale outflows driven by 8- and 24-mu m sources or (iii) by an undetected and widespread population of lower mass protostars. High-angular-resolution observations are needed to disentangle between these three scenarios. C1 [Jimenez-Serra, I.; Caselli, P.; van Loo, S.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Jimenez-Serra, I.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Tan, J. C.; Hernandez, A. K.; Butler, M. J.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Fontani, F.] Inst Radio Astron Millimetr, F-38406 St Martin Dheres, France. RP Jimenez-Serra, I (reprint author), Univ Leeds, Sch Phys & Astron, EC Stoner Bldg, Leeds LS2 9JT, W Yorkshire, England. EM ijimenez-serra@cfa.harvard.edu OI Fontani, Francesco/0000-0003-0348-3418; Van Loo, Sven/0000-0003-4746-8500 FU NSF [AST-0645412]; Swiss National Science Foundation [PP002 - 110504]; European Community [227290] FX We acknowledge the IRAM staff, and in particular H. Wiesemeyer, for the help provided during the observations. We also thank Professor J. Martin-Pintado for helpful discussions on the different mechanisms that can produce widespread SiO in star-forming regions and an anonymous referee for his/her careful reading of the manuscript. JCT acknowledges support from NSF CAREER grant AST-0645412. FF acknowledges support by Swiss National Science Foundation grant (PP002 - 110504). This effort/activity is supported by the European Community Framework Programme 7, Advanced Radio Astronomy in Europe, grant agreement no.: 227290. NR 50 TC 50 Z9 50 U1 1 U2 3 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUL 21 PY 2010 VL 406 IS 1 BP 187 EP 196 DI 10.1111/j.1365-2966.2010.16698.x PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 623TI UT WOS:000279766800036 ER PT J AU Koljonen, KII Hannikainen, DC McCollough, ML Pooley, GG Trushkin, SA AF Koljonen, K. I. I. Hannikainen, D. C. McCollough, M. L. Pooley, G. G. Trushkin, S. A. TI The hardness-intensity diagram of Cygnus X-3: revisiting the radio/X-ray states SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion; accretion discs; binaries: close; X-rays: binaries; X-rays: individual: Cygnus X-3; X-rays: stars ID X-RAY; SPECTRAL VARIABILITY; VLBI OBSERVATIONS; RELATIVISTIC JET; EMISSION-LINES; CYG X-3; 8.3 GHZ; MICROQUASARS; SCATTERING; OUTBURSTS AB Cygnus X-3 is one of the brightest X-ray and radio sources in the Galaxy and is well known for its erratic behaviour in X-rays as well as in the radio, occasionally producing major radio flares associated with relativistic ejections. However, even after many years of observations in various wavelength bands Cyg X-3 still eludes clear physical understanding. Studying different emission bands simultaneously in microquasars has proved to be a fruitful approach towards understanding these systems, especially by shedding light on the accretion disc/jet connection. We continue this legacy by constructing a hardness-intensity diagram (HID) from archival Rossi X-ray Timing Explorer data and linking simultaneous radio observations to it. We find that surprisingly Cyg X-3 sketches a similar shape in the HID to that seen in other transient black hole X-ray binaries during outburst but with distinct differences. Together with the results of this analysis and previous studies of Cyg X-3, we conclude that the X-ray states can be assigned to six distinct states. This categorization relies heavily on the simultaneous radio observations and we identify one new X-ray state, the hypersoft state, similar to the ultrasoft state, which is associated with the quenched radio state during which there is no or very faint radio emission. Recent observations of GeV flux observed from Cyg X-3 during a soft X-ray and/or radio quenched state at the onset of a major radio flare hint that a very energetic process is at work during this time, which is also when the hypersoft X-ray state is observed. In addition, Cyg X-3 shows flaring with a wide range of hardness. C1 [Koljonen, K. I. I.; Hannikainen, D. C.] Aalto Univ Metsahovi Radio Observ, Kylmala 02540, Finland. [Hannikainen, D. C.] Univ Turku, Tuorla Observ, Piikkio 21500, Finland. [McCollough, M. L.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Pooley, G. G.] Univ Cambridge, Cavendish Lab, Astrophys Lab, Cambridge CB3 0HE, England. [Trushkin, S. A.] RAS, Special Astrophys Observ, Karachaevo Cherkassian 36916, Nizhnij Arkhyz, Russia. RP Koljonen, KII (reprint author), Aalto Univ Metsahovi Radio Observ, Metsahovintie 114, Kylmala 02540, Finland. EM karri@kurp.hut.fi OI Koljonen, Karri/0000-0002-9677-1533 FU Academy of Finland [125189, 212656]; NASA [NNG06GE72G, NNX06AB94G, NAS8-03060]; Russian Foundation for Basic Research [08-02-00504-a] FX The authors thank the referee for careful reading of the manuscript and useful suggestions that improved the paper. The authors also thank Osmi Vilhu for enlightening discussions. KIIK gratefully acknowledges a grant from Jenny ja Antti Wihurin saatio and Acadamy of Finland grant (project no. 125189). DCH acknowledges Academy of Finland grant (project no. 212656). MLM wished to acknowledge support from NASA under grant/contract NNG06GE72G, NNX06AB94G and NAS8-03060. SAT acknowledges support from Russian Foundation for Basic Research, grant 08-02-00504-a. 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. NR 52 TC 24 Z9 24 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUL 21 PY 2010 VL 406 IS 1 BP 307 EP 319 DI 10.1111/j.1365-2966.2010.16722.x PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 623TI UT WOS:000279766800046 ER PT J AU Heyl, JS Gill, R Hernquist, L AF Heyl, Jeremy S. Gill, Ramandeep Hernquist, Lars TI Cosmic rays from pulsars and magnetars SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: neutron; cosmic rays ID SOFT GAMMA-REPEATERS; MAGNETIZED NEUTRON-STARS; X-RAY; SOLAR-NEIGHBORHOOD; EMISSION; DISCOVERY; BIRTHRATE; ELECTRONS; ENERGIES; MODEL AB We compare the expected abundance of cosmic ray electrons and positrons from pulsars and magnetars. We assume that the distribution of infant pulsars and magnetars follows that of high-mass stars in the Milky Way and that the production rate of cosmic rays is proportional to the spin-down and magnetic-decay power of pulsars and magnetars, respectively. In combination with primary and secondary cosmic ray leptons from other sources (especially supernova remnants), we find that both magnetars and pulsars can easily account for the observed cosmic ray spectrum, in particular the dip seen by HESS (High-Energy Stereoscopic System) at several TeV and the increase in positron fraction found by PAMELA (Payload for Antimatter Exploration and Light Nuclei Astrophysics). C1 [Heyl, Jeremy S.; Gill, Ramandeep] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Heyl, JS (reprint author), Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. EM heyl@phas.ubc.ca FU NSERC; CFI; BCKDF FX This research was supported by funding from NSERC, CFI and BCKDF and made use of the NASA ADS. NR 30 TC 4 Z9 4 U1 0 U2 1 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUL 21 PY 2010 VL 406 IS 1 BP L25 EP L29 DI 10.1111/j.1745-3933.2010.00874.x PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 623TI UT WOS:000279766800006 ER PT J AU Risaliti, G Elvis, M Bianchi, S Matt, G AF Risaliti, G. Elvis, M. Bianchi, S. Matt, G. TI Chandra monitoring of UGC 4203: the structure of the X-ray absorber SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: individual (UGC 4203); galaxies: AGN ID ACTIVE GALACTIC NUCLEI; BROAD-LINE REGIONS; BLACK-HOLE MASSES; NGC 1365; SEYFERT-2 GALAXIES; SPECTRAL-ANALYSIS; PHOENIX GALAXY; EMISSION; QUASARS; AGN AB We present a Chandra monitoring campaign of the highly variable Seyfert galaxy UGC 4203 (the 'Phoenix Galaxy') which revealed variations in the X-ray absorbing column density on time-scales of 2 weeks. This is the third, clear case, after NGC 1365 and NGC 7582, of dramatic N(H) variability on short time-scales observed in a 'changing look' source, i.e. an active galactic nuclei (AGN) observed in the past in both a reflection-dominated and a Compton-thin state. The inferred limits on the distance of the X-ray absorber from the centre suggest that the X-ray 'torus' could be one and the same with the broad emission line region. This scenario, first proposed for an 'ad hoc' picture for NGC 1365, may be the common structure of the circumnuclear medium in AGN. C1 [Risaliti, G.] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. [Risaliti, G.; Elvis, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bianchi, S.; Matt, G.] Univ Roma Tre, Dipartimento Fis, I-00146 Rome, Italy. RP Risaliti, G (reprint author), Osserv Astrofis Arcetri, INAF, Largo E Fermi 5, I-50125 Florence, Italy. EM grisaliti@cfa.harvard.edu RI Bianchi, Stefano/B-4804-2010; OI Bianchi, Stefano/0000-0002-4622-4240; Risaliti, Guido/0000-0002-3556-977X FU NASA [G08-9107X, G09-0105X] FX 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). This work has been partially funded by NASA grants G08-9107X and G09-0105X. NR 32 TC 31 Z9 31 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUL 21 PY 2010 VL 406 IS 1 BP L20 EP L24 DI 10.1111/j.1745-3933.2010.00873.x PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 623TI UT WOS:000279766800005 ER PT J AU Steinhardt, CL Elvis, M AF Steinhardt, Charles L. Elvis, Martin TI The quasar mass-luminosity plane - III. Smaller errors on virial mass estimates SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion; accretion discs; black hole physics; galaxies: evolution; galaxies: nuclei; quasars: general ID BLACK-HOLE MASSES; ACTIVE GALACTIC NUCLEI; ENERGY-DISTRIBUTIONS; EDDINGTON RATIO; EVOLUTION; CATALOG AB We use 62 185 quasars from the Sloan Digital Sky Survey (SDSS) DR5 sample to explore the quasar mass-luminosity plane view of virial mass estimation. Previous work shows deviations of similar to 0.4 dex between virial and reverberation masses. The decline in quasar number density for the highest Eddington ratio quasars at each redshift provides an upper bound of between 0.13 and 0.29 dex for virial mass estimate statistical uncertainties. Across different redshift bins, the maximum possible Mg ii mass uncertainties average 0.15 dex, while H beta uncertainties average 0.21 dex and C iv uncertainties average 0.27 dex. Any physical spread near the high-Eddington-ratio boundary will produce a more restrictive bound. A comparison of the sub-Eddington boundary slope using H beta and Mg ii masses finds better agreement with uncorrected Mg ii masses than with recently proposed corrections. The best agreement for these bright objects is produced by a multiplicative correction by a factor of 1.19, smaller than the factor of 1.8 previously reported as producing the best agreement for the entire SDSS sample. C1 [Steinhardt, Charles L.; Elvis, Martin] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Steinhardt, CL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM csteinha@cfa.harvard.edu FU Chandra [G07-8136A] FX The authors would like to thank Norm Murray, Ue-Li Pen, Bradley Peterson, Yue Shen, Michael Strauss and Jonathan Trump for valuable comments. This work was supported in part by Chandra grant number G07-8136A. NR 26 TC 14 Z9 14 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUL 21 PY 2010 VL 406 IS 1 BP L1 EP L5 DI 10.1111/j.1745-3933.2010.00866.x PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 623TI UT WOS:000279766800001 ER PT J AU Lin, TY Finkbeiner, DP Dobler, G AF Lin, Tongyan Finkbeiner, Douglas P. Dobler, Gregory TI The electron injection spectrum determined by anomalous excesses in cosmic ray, gamma ray, and microwave data SO PHYSICAL REVIEW D LA English DT Article ID DARK-MATTER; LEPTONS; GALAXY; EARTH; FIELD AB Recent cosmic ray, gamma ray, and microwave signals observed by Fermi, PAMELA, and WMAP indicate an unexpected primary source of e(+)e(-) at 10-1000 GeV. We fit these data to "standard backgrounds'' plus a new source, assumed to be a separable function of position and energy. For the spatial part, we consider three cases: annihilating dark matter, decaying dark matter, and pulsars. In each case, we use GALPROP to inject energy in log-spaced energy bins and compute the expected cosmic ray and photon signals for each bin. We then fit a linear combination of energy bins, plus backgrounds, to the data. We use a nonparametric fit, with no prior constraints on the spectrum except smoothness and non-negativity. In addition, we consider arbitrary modifications to the energy spectrum of the ordinary primary source function, fixing its spatial part, finding this alone to be inadequate to explain the PAMELA or WMAP signals. We explore variations in the fits due to choice of magnetic field, primary electron injection index, spatial profiles, propagation parameters, and fit regularization method. Dark matter annihilation fits well, where our fit finds a mass of similar to 1 TeV and a boost factor times energy fraction of similar to 70. While it is possible for dark matter decay and pulsars to fit the data, unconventionally high magnetic fields and radiation densities are required near the Galactic center to counter the relative shallowness of the assumed spatial profiles. We also fit to linear combinations of these three scenarios, though the fit is much less constrained. C1 [Lin, Tongyan; Finkbeiner, Douglas P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lin, Tongyan; Finkbeiner, Douglas P.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Dobler, Gregory] Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA. RP Lin, TY (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM tongyan@physics.harvard.edu FU FAS Research Computing Group at Harvard; NSF; NASA [NNX10AD85G] FX We are grateful to Ilias Cholis, Marco Cirelli, Tracy Slatyer, and Neal Weiner for helpful discussions and comments on this paper. The computations in this paper were run on the Odyssey cluster supported by the FAS Research Computing Group at Harvard. T.L. is supported by NSF. D.P.F. is partially supported by NASA Theory Grant No. NNX10AD85G. This research made use of the NASA Astrophysics Data System (ADS) and the IDL Astronomy User's Library at Goddard [67]. NR 62 TC 12 Z9 12 U1 0 U2 1 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1550-7998 J9 PHYS REV D JI Phys. Rev. D PD JUL 21 PY 2010 VL 82 IS 2 AR 023518 DI 10.1103/PhysRevD.82.023518 PG 19 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 629DR UT WOS:000280175400001 ER PT J AU Lidz, A Faucher-Giguere, CA Dall'Aglio, A McQuinn, M Fechner, C Zaldarriaga, M Hernquist, L Dutta, S AF Lidz, Adam Faucher-Giguere, Claude-Andre Dall'Aglio, Aldo McQuinn, Matthew Fechner, Cora Zaldarriaga, Matias Hernquist, Lars Dutta, Suvendra TI A MEASUREMENT OF SMALL-SCALE STRUCTURE IN THE 2.2 <= z <= 4.2 Ly alpha FOREST SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: theory; intergalactic medium; large-scale structure of universe ID EQUATION-OF-STATE; COLD DARK-MATTER; TEMPERATURE-DENSITY RELATION; PHOTOIONIZED INTERGALACTIC MEDIUM; QSO ABSORPTION-SPECTRA; DIGITAL SKY SURVEY; POWER-SPECTRUM; RADIATIVE-TRANSFER; HYDROGEN REIONIZATION; HELIUM REIONIZATION AB The amplitude of fluctuations in the Ly alpha forest on small spatial scales is sensitive to the temperature of the intergalactic medium (IGM) and its spatial fluctuations. The temperature of the IGM and its spatial variations contain important information about hydrogen and helium reionization. We present a new measurement of the small-scale structure in the Ly alpha forest from 40 high resolution, high signal-to-noise ratio, VLT spectra for absorbing gas at redshifts between 2.2 <= z <= 4.2. We convolve each Ly alpha forest spectrum with a suitably chosen Morlet wavelet filter, which allows us to extract the amount of small-scale structure in the forest as a function of position across each spectrum. We monitor contamination from metal line absorbers. We present a first comparison of these measurements with high-resolution hydrodynamic simulations of the Ly alpha forest that track more than 2 billion particles. This comparison suggests that the IGM temperature close to the cosmic mean density (T-0) peaks at a redshift near z = 3.4, at which point it is greater than 20,000 K at greater than or similar to 2 sigma confidence. The temperature at lower redshift is consistent with the fall-off expected from adiabatic cooling (T-0 alpha (1 + z)(2)), after the peak temperature is reached near z = 3.4. In our highest redshift bin, centered around z = 4.2, the results favor a temperature of T-0 = 15-20,000 K. However, owing mostly to uncertainties in the mean transmitted flux at this redshift, a cooler IGM model with T-0 = 10,000 K is only disfavored at the 2 sigma level here, although such cool IGM models are strongly discrepant with the z approximate to 3-3.4 measurement. We do not detect large spatial fluctuations in the IGM temperature at any redshift covered by our data set. The simplest interpretation of our measurements is that He II reionization completes sometime near z approximate to 3.4, although statistical uncertainties are still large. Our method can be fruitfully combined with future He II Ly alpha forest measurements. C1 [Lidz, Adam] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Lidz, Adam; Faucher-Giguere, Claude-Andre; McQuinn, Matthew; Zaldarriaga, Matias; Hernquist, Lars; Dutta, Suvendra] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Dall'Aglio, Aldo] Astrophys Inst Potsdam, D-14482 Potsdam, Germany. [Fechner, Cora] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. [Zaldarriaga, Matias] Inst Adv Study, Sch Nat Sci, Princeton, NJ 08540 USA. [Zaldarriaga, Matias] Harvard Univ, Jefferson Lab Phys, Cambridge, MA 02138 USA. RP Lidz, A (reprint author), Univ Penn, Dept Phys & Astron, 209 S 33rd St, Philadelphia, PA 19104 USA. EM alidz@sas.upenn.edu FU NSERC; Canadian Space Agency; David and Lucile Packard Foundation; Alfred P. Sloan Foundation [AST-0506556, NNG05GJ40G] FX We thank Jamie Bolton, Mark Dijkstra, Nick Gnedin, Lam Hui, Hy Trac, and Matteo Viel for helpful conversations. We are especially grateful to the referee, Joop Schaye, whose report greatly improved the manuscript. Cosmological simulations were run on the Odyssey supercomputer at Harvard University. C.A.F.G. acknowledges support during the course of this work from a NSERC graduate fellowship and the Canadian Space Agency. Support was provided, in part, by the David and Lucile Packard Foundation, the Alfred P. Sloan Foundation, and grants AST-0506556 and NNG05GJ40G. NR 71 TC 64 Z9 64 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 JUL 20 PY 2010 VL 718 IS 1 BP 199 EP 230 DI 10.1088/0004-637X/718/1/199 PG 32 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 631IU UT WOS:000280340800019 ER PT J AU Attrill, GDR AF Attrill, Gemma D. R. TI DISPELLING ILLUSIONS OF REFLECTION: A NEW ANALYSIS OF THE 2007 MAY 19 CORONAL "WAVE" EVENT SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: activity; Sun: corona; Sun: coronal mass ejections (CMEs); Sun: UV radiation; Sun: X-rays, gamma rays ID EIT WAVES; MASS EJECTION; SOHO/EIT OBSERVATIONS; SOLAR CORONA; SHOCK-WAVES; STEREO; CMES; TRANSIENT; FILAMENT; DIMMINGS AB A new analysis of the 2007 May 19 coronal wave-coronal mass ejection-dimmings event is offered employing base difference extreme-ultraviolet (EUV) images. Previous work analyzing the coronal wave associated with this event concluded strongly in favor of purely an MHD wave interpretation for the expanding bright front. This conclusion was based to a significant extent on the identification of multiple reflections of the coronal wave front. The analysis presented here shows that the previously identified "reflections" are actually optical illusions and result from a mis-interpretation of the running difference EUV data. The results of this new multiwavelength analysis indicate that two coronal wave fronts actually developed during the eruption. This new analysis has implications for our understanding of diffuse coronal waves and questions the validity of the analysis and conclusions reached in previous studies. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Attrill, GDR (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU NASA [NNX09AB11G] FX I appreciate the helpful comments from the referee which clarified this work. I would also like to sincerely thank N. Gopalswamy, A. Veronig, and P. Gallagher for discussions concerning the analysis of this complex event. I am extremely grateful to L. van Driel-Gesztelyi, P. Demoulin, L. Culhane, L. Harra, O. Cohen, N. Nitta, A. Engell, M. Wills-Davey, and the SSXG group at SAO for discussion developing various aspects of this work. My thanks also to C. Mostl for initiating discussion regarding the interplanetary component of this CME event, and the connection with the low coronal counterpart. The STEREO/SECCHI data are produced by an international consortium: NRL, LMSAL, NASA, GSFC (USA); RAL (UK); MPS (Germany); CSL (Belgium); and IOTA, IAS (France). SOHO is a project of international cooperation between ESA and NASA. This research has made use of NASA's Astrophysics Data System Bibliographic Services. I acknowledge NASA grant NNX09AB11G which supported this work. NR 53 TC 25 Z9 26 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2010 VL 718 IS 1 BP 494 EP 501 DI 10.1088/0004-637X/718/1/494 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 631IU UT WOS:000280340800043 ER PT J AU Sand, DJ Seth, A Olszewski, EW Willman, B Zaritsky, D Kallivayalil, N AF Sand, David J. Seth, Anil Olszewski, Edward W. Willman, Beth Zaritsky, Dennis Kallivayalil, Nitya TI A DEEPER LOOK AT LEO IV: STAR FORMATION HISTORY AND EXTENDED STRUCTURE SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: dwarf; Local Group ID DWARF SPHEROIDAL GALAXY; MILKY-WAY SATELLITE; BLUE STRAGGLER STARS; DIGITAL SKY SURVEY; COLOR-MAGNITUDE DIAGRAM; LOCAL GROUP; STELLAR POPULATIONS; GLOBULAR-CLUSTERS; URSA-MAJOR; FORNAX AB We present MMT/Megacam imaging of the Leo IV dwarf galaxy in order to investigate its structure and star formation history, and to search for signs of association with the recently discovered Leo V satellite. Based on parameterized fits, we find that Leo IV is round, with is an element of < 0.23 (at the 68% confidence limit) and a half-light radius of r(h) similar or equal to 130 pc. Additionally, we perform a thorough search for extended structures in the plane of the sky and along the line of sight. We derive our surface brightness detection limit by implanting fake structures into our catalog with stellar populations identical to that of Leo IV. We show that we are sensitive to stream-like structures with surface brightness mu(r) less than or similar to 29.6 mag arcsec(-2), and at this limit we find no stellar bridge between Leo IV (out to a radius of similar to 0.5 kpc) and the recently discovered, nearby satellite Leo V. Using the color-magnitude fitting package StarFISH, we determine that Leo IV is consistent with a single age (similar to 14 Gyr), single metallicity ([Fe/H] similar to -2.3) stellar population, although we cannot rule out a significant spread in these values. We derive a luminosity of M(V) = -5.5 +/- 0.3. Studying both the spatial distribution and frequency of Leo IV's " blue plume" stars reveals evidence for a young (similar to 2 Gyr) stellar population which makes up similar to 2% of its stellar mass. This sprinkling of star formation, only detectable in this deep study, highlights the need for further imaging of the new Milky Way satellites along with theoretical work on the expected, detailed properties of these possible " reionization fossils." C1 [Sand, David J.; Seth, Anil] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Olszewski, Edward W.; Zaritsky, Dennis] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Kallivayalil, Nitya] MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. EM dave.j.sand@gmail.com FU NSF [AST-0807498, AST-0307492]; NASA [NNG05GE82G] FX We are grateful to the referee, Nicolas Martin, for his constructive report. Many thanks to Maureen Conroy, Nathalie Martimbeau, Brian McLeod, and the whole Megacam team for the timely help in reducing our Leo IV data. D.J.S. is grateful to Jay Strader for his excellent scientific advice, and for providing his co-calibrated M3 and M13 BHB sequence. We are grateful to Evan Kirby, Josh Simon, and Marla Geha for providing their kinematic and metallicity data on Leo IV. Yazan Momany kindly provided his blue plume frequency data. D.J.S. is grateful to Matthew Walker and Nelson Caldwell for providing a careful reading of the paper, along with useful comments. E.O. was partially supported by NSF grant AST-0807498. D.Z. acknowledges support from NASA LTSA award NNG05GE82G and NSF grant AST-0307492. NR 50 TC 25 Z9 25 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2010 VL 718 IS 1 BP 530 EP 542 DI 10.1088/0004-637X/718/1/530 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 631IU UT WOS:000280340800048 ER PT J AU Winn, JN Johnson, JA Howard, AW Marcy, GW Bakos, GA Hartman, J Torres, G Albrecht, S Narita, N AF Winn, Joshua N. Johnson, John Asher Howard, Andrew W. Marcy, Geoffrey W. Bakos, Gaspar A. Hartman, Joel Torres, Guillermo Albrecht, Simon Narita, Norio TI THE HAT-P-13 EXOPLANETARY SYSTEM: EVIDENCE FOR SPIN-ORBIT ALIGNMENT AND A THIRD COMPANION SO ASTROPHYSICAL JOURNAL LA English DT Article DE planets and satellites: dynamical evolution and stability; planets and satellites: formation; planets and satellites: individual (HAT-P-13b, c, d); planets and satellites: interiors; stars: rotation ID PLANETARY SYSTEM; TIDAL EVOLUTION; SEARCH; HD-83443; CURVES; MODELS AB We present new radial velocity (RV) measurements of HAT-P-13, a star with two previously known companions: a transiting giant planet "b" with an orbital period of 3 days and a more massive object "c" on a 1.2 yr, highly eccentric orbit. For this system, dynamical considerations would lead to constraints on planet b's interior structure, if it could be shown that the orbits are coplanar and apsidally locked. By modeling the Rossiter-McLaughlin effect, we show that planet b's orbital angular momentum vector and the stellar spin vector are well aligned on the sky (lambda = 1.9 +/- 8.6 deg). The refined orbital solution favors a slightly eccentric orbit for planet b (e = 0.0133 +/- 0.0041), although it is not clear whether it is apsidally locked with c's orbit (Delta omega = 36(-36)(+27) deg). We find a long-term trend in the star's RV and interpret it as evidence for an additional body "d," which may be another planet or a low-mass star. Predictions are given for the next few inferior conjunctions of c, when transits may happen. C1 [Winn, Joshua N.; Albrecht, Simon] MIT, Dept Phys, Cambridge, MA 02139 USA. [Winn, Joshua N.; Albrecht, Simon] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Winn, Joshua N.; Narita, Norio] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA. [Johnson, John Asher] CALTECH, Dept Astrophys, Pasadena, CA 91125 USA. [Howard, Andrew W.; Marcy, Geoffrey W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Howard, Andrew W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Bakos, Gaspar A.; Hartman, Joel; Torres, Guillermo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Narita, Norio] Natl Inst Nat Sci, Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. RP Winn, JN (reprint author), MIT, Dept Phys, Cambridge, MA 02139 USA. RI Howard, Andrew/D-4148-2015; OI Howard, Andrew/0000-0001-8638-0320; Hartman, Joel/0000-0001-8732-6166 FU NASA [NNX09AD36G, NNX08AF23G, NNX09AF59G]; MIT Class; Space Sciences Laboratory at UC Berkeley; NSF [AST-0702843, NSF PHY05-51164]; Netherlands Organisation for Scientific Research (NWO); Japan Society for Promotion of Science (JSPS) [PD: 20-8141]; W. M. Keck Foundation FX J.N.W. gratefully acknowledges support from the NASA Origins program through award NNX09AD36G and the MIT Class of 1942. A. W. H. acknowledges a Townes Postdoctoral Fellowship from the Space Sciences Laboratory at UC Berkeley. G. A. B. was supported by NASA grant NNX08AF23G and an NSF Astronomy & Astrophysics Postdoctoral Fellowship (AST-0702843). G. T. acknowledges partial support from NASA grant NNX09AF59G. S. A. acknowledges the support of the Netherlands Organisation for Scientific Research (NWO). N. N. was supported by a Japan Society for Promotion of Science (JSPS) Fellowship for Research (PD: 20-8141). J. N. W. and N. N. were also supported in part by the National Science Foundation under Grant No. NSF PHY05-51164 (KITP program "The Theory and Observation of Exoplanets" at UCSB).; 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, and was made possible by the generous financial support of the W. M. Keck Foundation. We extend special thanks to those of Hawaiian ancestry on whose sacred mountain of Mauna Kea we are privileged to be guests. Without their generous hospitality, the Keck observations presented herein would not have been possible. NR 28 TC 50 Z9 50 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2010 VL 718 IS 1 BP 575 EP 582 DI 10.1088/0004-637X/718/1/575 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 631IU UT WOS:000280340800052 ER PT J AU Smith, RK Hughes, JP AF Smith, Randall K. Hughes, John P. TI IONIZATION EQUILIBRIUM TIMESCALES IN COLLISIONAL PLASMAS SO ASTROPHYSICAL JOURNAL LA English DT Article DE atomic data; atomic processes; plasmas ID SUPER-NOVA REMNANTS; X-RAY-EMISSION; RATE COEFFICIENTS; HOT PLASMA; MODELS; DISCOVERY; SPECTRA; SUZAKU; IRON; IONS AB Astrophysical shocks or bursts from a photoionizing source can disturb the typical collisional plasma found in galactic interstellar media or the intergalactic medium. The spectrum emitted by this plasma contains diagnostics that have been used to determine the time since the disturbing event, although this determination becomes uncertain as the elements in the plasma return to ionization equilibrium. A general solution for the equilibrium timescale for each element arises from the elegant eigenvector method of solution to the problem of a non-equilibrium plasma described by Masai and Hughes & Helfand. In general, the ionization evolution of an element Z in a constant electron temperature plasma is given by a coupled set of Z + 1 first-order differential equations. However, they can be recast as Z uncoupled first-order differential equations using an eigenvector basis for the system. The solution is then Z separate exponential functions, with the time constants given by the eigenvalues of the rate matrix. The smallest of these eigenvalues gives the scale of the slowest return to equilibrium independent of the initial conditions, while conversely the largest eigenvalue is the scale of the fastest change in the ion population. These results hold for an ionizing plasma, a recombining plasma, or even a plasma with random initial conditions, and will allow users of these diagnostics to determine directly if their best-fit result significantly limits the timescale since a disturbance or is so close to equilibrium as to include an arbitrarily long time. C1 [Smith, Randall K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hughes, John P.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. RP Smith, RK (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rsmith@cfa.harvard.edu; jph@physics.rutgers.edu RI XRAY, SUZAKU/A-1808-2009 FU Chandra GO Theory [TM4-5004X] FX We thank the anonymous referee for suggesting determining the minimum timescale as well as the maximum, and also acknowledge helpful discussions with Terrance Gaetz and John Raymond. Support for this project came from the Chandra GO Theory program, grant TM4-5004X. NR 15 TC 55 Z9 55 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2010 VL 718 IS 1 BP 583 EP 585 DI 10.1088/0004-637X/718/1/583 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 631IU UT WOS:000280340800053 ER PT J AU Massardi, M Ekers, RD Ellis, SC Maughan, B AF Massardi, M. Ekers, R. D. Ellis, S. C. Maughan, B. TI HIGH ANGULAR RESOLUTION OBSERVATION OF THE SUNYAEV-ZEL'DOVICH EFFECT IN THE MASSIVE z approximate to 0.83 CLUSTER Cl J0152-1357 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE cosmological parameters; galaxies: clusters: individual (C1 J0152-1357); techniques: interferometric ID LUMINOUS GALAXY CLUSTER; HIGH-REDSHIFT CLUSTERS; X-RAY-CLUSTERS; HUBBLE-CONSTANT; RX J0152.7-1357; RX-J0152.7-1357; CHANDRA; Z=0.83; IMAGES AB X-ray observations of galaxy clusters at high redshift (z greater than or similar to 0.5) indicate that they are more morphologically complex and less virialized than those at low redshift. We present the first subarcminute resolution synthesis observations at 18 GHz of the Sunyaev-Zel'dovich (SZ) effect for Cl J0152-1357 using the Australia Telescope Compact Array. Cl J0152-1357 is a massive cluster at redshift z = 0.83 and has a complex structure including several merging subclumps which have been studied at optical, X-ray, and radio wavelengths. Our high-resolution observations indicate a clear displacement of the maximum SZ effect from the peak of X-ray emission for the most massive subclump. This result shows that the cluster gas within the cluster substructures is not virialized in Cl J0152-1357, and we suggest that it is still recovering from a recent merger event. A similar offset of the SZ effect has recently been seen in the "bullet cluster" and in RX J1347-1145. This non-equilibrium situation implies that high-resolution observations are necessary to investigate galaxy cluster evolution and to extract cosmological constraints from a comparison of the SZ effect and X-ray signals. C1 [Massardi, M.] INAF, Osservatorio Astron Padova, I-35122 Padua, Italy. [Massardi, M.; Ekers, R. D.] Australia Telescope Natl Facil, CSIRO Astron & Space Sci, Epping, NSW 1710, Australia. [Ellis, S. C.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Ellis, S. C.] Anglo Australian Observ, Epping, NSW 2121, Australia. [Maughan, B.] Univ Bristol, HH Wills Phys Lab, Bristol BS8 1TL, Avon, England. [Maughan, B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02140 USA. RP Massardi, M (reprint author), INAF, Osservatorio Astron Padova, Vicolo Osservatorio 5, I-35122 Padua, Italy. EM marcella.massardi@oapd.inaf.it FU Italian ASI/INAF [I/072/09/0]; ARC through the University of Sydney [0776384] FX Partial financial support for this research has been provided to M. M. by the Italian ASI/INAF Agreement I/072/09/0 for the Planck LFI Activity of Phase E2 and I/016/07/0 "COFIS". S.C.E. is funded by ARC FF grant 0776384 through the University of Sydney.; We thank the staff at the Australia Telescope Compact Array site, Narrabri (NSW), for the valuable support they provide in running the telescope. The Australia Telescope Compact Array is part of the Australia Telescope, which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. NR 36 TC 8 Z9 8 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUL 20 PY 2010 VL 718 IS 1 BP L23 EP L26 DI 10.1088/2041-8205/718/1/L23 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 619LD UT WOS:000279430800005 ER PT J AU Brahms, N Tscherbul, TV Zhang, P Klos, J Sadeghpour, HR Dalgarno, A Doyle, JM Walker, TG AF Brahms, N. Tscherbul, T. V. Zhang, P. Klos, J. Sadeghpour, H. R. Dalgarno, A. Doyle, J. M. Walker, T. G. TI Formation of Van Der Waals Molecules in Buffer-Gas-Cooled Magnetic Traps SO PHYSICAL REVIEW LETTERS LA English DT Article ID VANDERWAALS MOLECULES; OPTICAL LATTICES; ULTRACOLD ATOMS; SPECTROSCOPY; CLUSTER; BINDING; ENERGY; STATES; PAIRS; SPIN AB We predict that a large class of helium-containing cold polar molecules form readily in a cryogenic buffer gas, achieving densities as high as 10(12) cm(-3). We explore the spin relaxation of these molecules in buffer-gas-loaded magnetic traps and identify a loss mechanism based on Landau-Zener transitions arising from the anisotropic hyperfine interaction. Our results show that the recently observed strong T-6 thermal dependence of the spin-change rate of silver (Ag) trapped in dense He-3 is accounted for by the formation and spin change of (AgHe)-He-3 van der Waals molecules, thus providing indirect evidence for molecular formation in a buffer-gas trap. C1 [Brahms, N.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Brahms, N.; Tscherbul, T. V.; Dalgarno, A.; Doyle, J. M.] Harvard MIT Ctr Ultracold Atoms, Cambridge, MA 02138 USA. [Tscherbul, T. V.; Zhang, P.; Sadeghpour, H. R.; Dalgarno, A.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Klos, J.] Univ Maryland, Dept Chem & Biochem, College Pk, MD 20742 USA. [Doyle, J. M.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Walker, T. G.] Univ Wisconsin, Dept Phys, Madison, WI 53715 USA. RP Brahms, N (reprint author), Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. RI Tscherbul, Timur/K-3286-2014; Walker, Thad/N-5590-2014 OI Tscherbul, Timur/0000-0001-5689-040X; Walker, Thad/0000-0002-0996-3351 FU DOE Office of Basic Energy Science; NSF [PHY-0757157]; ITAMP at the Harvard/Smithsonian Center for Astrophysics; University of Wisconsin; Millard Alexander at UMD (NSF) [CHE-0848110] FX We acknowledge stimulating discussions with A.A. Buchachenko and Y.S. Au. We are grateful for grants from the DOE Office of Basic Energy Science and NSF to the Harvard-MIT CUA (NSF Grant No. PHY-0757157), ITAMP at the Harvard/Smithsonian Center for Astrophysics, the University of Wisconsin, and Millard Alexander at UMD (NSF Grant No. CHE-0848110). NR 35 TC 14 Z9 14 U1 0 U2 4 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 J9 PHYS REV LETT JI Phys. Rev. Lett. PD JUL 16 PY 2010 VL 105 IS 3 AR 033001 DI 10.1103/PhysRevLett.105.033001 PG 4 WC Physics, Multidisciplinary SC Physics GA 627AB UT WOS:000280008900006 PM 20867761 ER PT J AU Comita, LS Muller-Landau, HC Aguilar, S Hubbell, SP AF Comita, Liza S. Muller-Landau, Helene C. Aguilar, Salomon Hubbell, Stephen P. TI Asymmetric Density Dependence Shapes Species Abundances in a Tropical Tree Community SO SCIENCE LA English DT Article ID LOCAL NEIGHBORHOOD; NEOTROPICAL FOREST; SHADE TOLERANCE; DIVERSITY; SURVIVAL; COEXISTENCE; RECRUITMENT; PATHOGENS; SEEDLINGS; GROWTH AB The factors determining species commonness and rarity are poorly understood, particularly in highly diverse communities. Theory predicts that interactions with neighbors of the same (conspecific) and other (heterospecific) species can influence a species' relative abundance, but empirical tests are lacking. By using a hierarchical model of survival for more than 30,000 seedlings of 180 tropical tree species on Barro Colorado Island, Panama, we tested whether species' sensitivity to neighboring individuals relates to their relative abundance in the community. We found wide variation among species in the effect of conspecific, but not heterospecific, neighbors on survival, and we found a significant relationship between the strength of conspecific neighbor effects and species abundance. Specifically, rare species suffered more from the presence of conspecific neighbors than common species did, suggesting that conspecific density dependence shapes species abundances in diverse communities. C1 [Comita, Liza S.] Natl Ctr Ecol Anal & Synth, Santa Barbara, CA 93101 USA. [Comita, Liza S.; Muller-Landau, Helene C.] Univ Minnesota, Dept Ecol Evolut & Behav, St Paul, MN 55108 USA. [Muller-Landau, Helene C.; Aguilar, Salomon; Hubbell, Stephen P.] Smithsonian Trop Res Inst, Balboa Ancon, Panama. [Hubbell, Stephen P.] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90024 USA. RP Comita, LS (reprint author), Natl Ctr Ecol Anal & Synth, 735 State St,Suite 300, Santa Barbara, CA 93101 USA. EM comita@nceas.ucsb.edu OI Comita, Liza/0000-0002-9169-1331 FU Packard Fellowship for Science and Engineering; NSF [DEB-0075102, 0425651, 0710211, 0823728]; Andrew W. Mellon Foundation; HSBC FX We thank the dozens of field assistants who conducted the seedling and tree censuses; R. Perez for assistance with species identifications; S. Lao for help with data management; and S. Banerjee, S. M. Lee, M. Schofield, and A. Gelman for statistical advice. The study was financially supported by a Packard Fellowship for Science and Engineering (to H.C.M.), NSF (grants DEB-0075102, 0425651, 0710211, and 0823728 to S. P. H.), the Andrew W. Mellon Foundation, and the HSBC Climate Partnership, with logistical support from the Center of Tropical Forest Science, Smithsonian Tropical Research Institute, and University of Georgia. NR 32 TC 230 Z9 239 U1 15 U2 166 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD JUL 16 PY 2010 VL 329 IS 5989 BP 330 EP 332 DI 10.1126/science.1190772 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 625VW UT WOS:000279925900044 PM 20576853 ER PT J AU Schmidt, ME McCoy, TJ AF Schmidt, Mariek E. McCoy, Timothy J. TI The evolution of a heterogeneous Martian mantle: Clues from K, P, Ti, Cr, and Ni variations in Gusev basalts and shergottite meteorites SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE Mars igneous processes; shergottites; Gusev basalts; Mars mantle ID CHEMICAL-COMPOSITION; TERRESTRIAL PLANETS; FRACTIONAL CRYSTALLIZATION; ISOTOPIC SYSTEMATICS; SIDEROPHILE ELEMENTS; MAGMATIC PROCESSES; SNC METEORITES; TRACE-ELEMENT; RB-SR; MARS AB Martian basalts represent samples of the interior of the planet, and their composition reflects their source at the time of extraction as well as later igneous processes that affected them. To better understand the composition and evolution of Mars, we compare whole rock compositions of basaltic shergottitic meteorites and basaltic lavas examined by the Spirit Mars Exploration Rover in Gusev Crater. Concentrations range from K-poor (as low as 0.02 wt.% K2O) in the shergottites to K-rich (up to 1.2 wt.% K2O) in basalts from the Columbia Hills (CH) of Gusev Crater: the Adirondack basalts from the Gusev Plains have more intermediate concentrations of K2O (0.16 wt.% to below detection limit). The compositional dataset for the Gusev basalts is more limited than for the shergottites, but it includes the minor elements K. P, Ti, Cr, and Ni, whose behavior during mantle melting varies from very incompatible (prefers melt) to very compatible (remains in the residuum). The range in partitioning behavior of these elements provides leverage on interpreting igneous processes. Models are presented that demonstrate how concentrations of these elements in Gusev basaltic magmas would change by simple igneous processes (fractional crystallization, crustal contamination, and mantle partial melting). The Gusev basalts may be related by two-stage batch melting of a primitive (K-rich) mantle source to first, generate the K-rich, Columbia Hills basalts and second, the lower K Adirondack basalts, leaving behind a K-poor residuum. The mantle source for the Gusev basalts is separate from the more depleted (K-poorer) source region of the shergottites. This indicates that primitive. K-rich mantle persisted until the Early Hesperian during formation of the Columbia Hills basalts. We suggest that separate mantle reservoirs developed by inhomogeneous partial melting (at melt fractions greater than 0.05) to form the Martian crust in the first 1 Ga of the planet's history. (C) 2010 Elsevier B.V. All rights reserved. C1 [Schmidt, Mariek E.] Brock Univ, Dept Earth Sci, St Catharines, ON L2S 3A1, Canada. [McCoy, Timothy J.] Natl Museum Nat Hist, Dept Mineral Sci, Smithsonian Inst, Washington, DC 20560 USA. RP Schmidt, ME (reprint author), Brock Univ, Dept Earth Sci, St Catharines, ON L2S 3A1, Canada. EM mschmidt2@brocku.ca FU Mars Exploration Rover FX This work benefited from the Mars Meteorite Compendium (Meyer, http://curator.jsc.nasa.gov/antmet/mmc/index.cfm) and was supported by a Mars Exploration Rover participating scientist award to Tim McCoy. Careful and perceptive reviews by Kevin Righter and an anonymous reviewer greatly improved this manuscript. In addition, we acknowledge the engineers and scientists on the MER team for their contributions to the success of the mission. NR 90 TC 15 Z9 15 U1 2 U2 18 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0012-821X EI 1385-013X J9 EARTH PLANET SC LETT JI Earth Planet. Sci. Lett. PD JUL 15 PY 2010 VL 296 IS 1-2 BP 67 EP 77 DI 10.1016/j.epsl.2010.04.046 PG 11 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 625OW UT WOS:000279905800007 ER PT J AU Muller, A Schippers, S Phaneuf, RA Scully, SWJ Aguilar, A Cisneros, C Gharaibeh, MF Schlachter, AS McLaughlin, BM AF Mueller, A. Schippers, S. Phaneuf, R. A. Scully, S. W. J. Aguilar, A. Cisneros, C. Gharaibeh, M. F. Schlachter, A. S. McLaughlin, B. M. TI K-shell photoionization of ground-state Li-like boron ions [B2+]: experiment and theory SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Article ID DOUBLY-EXCITED RESONANCES; LASER-PRODUCED PLASMAS; SINGLE GAS COLLISIONS; R-MATRIX THEORY; HIGH-RESOLUTION; CROSS-SECTIONS; AUGER-SPECTRA; B STARS; AUTOIONIZATION; SPECTROSCOPY AB Absolute cross sections for the K-shell photoionization of ground-state Li-like boron [B2+(1s(2)2s S-2)] ions were measured by employing the ion-photon merged-beams technique at the Advanced Light Source synchrotron radiation facility. The energy ranges 197.5-200.5 eV, and 201.9-202.1 eV of the [1s(2s2p)P-3]P-2(o) and [1s(2s2p)P-1] P-2(o) resonances, respectively, were investigated using resolving powers of up to 17 600. The energy range of the experiments was extended to about 238.2 eV yielding energies of the most prominent [1s(2l nl')] Po-2 resonances with an absolute accuracy of the order of 130 ppm. The natural linewidths of the [1s(2s2p)P-3] Po-2 and [1s(2s2p)P-1] P-2(o) resonances were measured to be 4.8 +/- 0.6meV and 29.7 +/- 2.5meV, respectively, which compare favourably with theoretical results of 4.40 meV and 30.53 meV determined using an intermediate-coupling R-matrix method. C1 [Scully, S. W. J.; McLaughlin, B. M.] Queens Univ Belfast, Sch Math & Phys, CTAMOP, Belfast BT7 1NN, Antrim, North Ireland. [Mueller, A.; Schippers, S.] Univ Giessen, Inst Atom & Mol Phys, D-35392 Giessen, Germany. [Phaneuf, R. A.; Scully, S. W. J.; Aguilar, A.; Gharaibeh, M. F.] Univ Nevada, Dept Phys, Reno, NV 89557 USA. [Aguilar, A.; Schlachter, A. S.] Univ Calif Berkeley, Lawrence Berkeley Lab, Adv Light Source, Berkeley, CA 94720 USA. [Cisneros, C.] Univ Nacl Autonoma Mexico, Ctr Ciencias Fis, Cuernavaca 62131, Morelos, Mexico. [McLaughlin, B. M.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RP McLaughlin, BM (reprint author), Queens Univ Belfast, Sch Math & Phys, CTAMOP, David Bates Bldg,7 Coll Pk, Belfast BT7 1NN, Antrim, North Ireland. EM b.mclaughlin@qub.ac.uk RI Muller, Alfred/A-3548-2009; Schippers, Stefan/A-7786-2008 OI Muller, Alfred/0000-0002-0030-6929; Schippers, Stefan/0000-0002-6166-7138 FU Deutsche Forschungsgemeinschaft [Mu 1068/10]; US Department of Energy ( DOE) [DE-AC03-76SF-00098, DE-FG02-03ER15424]; US National Science Foundation FX We acknowledge support by Deutsche Forschungsgemeinschaft under project number Mu 1068/10 and through NATO Collaborative Linkage grant 976362 as well as by the US Department of Energy ( DOE) under contract DE-AC03-76SF-00098 and grant DE-FG02-03ER15424. BMM acknowledges support by the US National Science Foundation through a grant to ITAMP at the Harvard-Smithsonian Center for Astrophysics. The computational work was carried out at the National Energy Research Scientific Computing Center in Oakland, CA, USA, and on the Tera-grid at the National Institute for Computational Science (NICS) in TN, USA, which is supported in part by the US National Science Foundation. NR 46 TC 21 Z9 21 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0953-4075 J9 J PHYS B-AT MOL OPT JI J. Phys. B-At. Mol. Opt. Phys. PD JUL 14 PY 2010 VL 43 IS 13 AR 135602 DI 10.1088/0953-4075/43/13/135602 PG 11 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 613TI UT WOS:000279003500030 ER PT J AU Hunt, ME Scherrer, MP Ferrari, FD Matz, MV AF Hunt, Marguerite E. Scherrer, Michael P. Ferrari, Frank D. Matz, Mikhail V. TI Very Bright Green Fluorescent Proteins from the Pontellid Copepod Pontella mimocerami SO PLOS ONE LA English DT Article ID CORAL; REPORTER; RED; GFP; AMPHIOXUS; DIVERSITY; EVOLUTION; MUTANTS; EMBRYOS; MARKER AB Background: Fluorescent proteins (FP) homologous to the green fluorescent protein (GFP) from the jellyfish Aequorea victoria have revolutionized biomedical research due to their usefulness as genetically encoded fluorescent labels. Fluorescent proteins from copepods are particularly promising due to their high brightness and rapid fluorescence development. Results: Here we report two novel FPs from Pontella mimocerami (Copepoda, Calanoida, Pontellidae), which were identified via fluorescence screening of a bacterial cDNA expression library prepared from the whole-body total RNA of the animal. The proteins are very similar in sequence and spectroscopic properties. They possess high molar extinction coefficients (79,000 M(-1) cm(-)) and quantum yields (0.92), which make them more than two-fold brighter than the most common FP marker, EGFP. Both proteins form oligomers, which we were able to counteract to some extent by mutagenesis of the N-terminal region; however, this particular modification resulted in substantial drop in brightness. Conclusions: The spectroscopic characteristics of the two P. mimocerami proteins place them among the brightest green FPs ever described. These proteins may therefore become valuable additions to the in vivo imaging toolkit. C1 [Hunt, Marguerite E.; Scherrer, Michael P.] Univ Texas Austin, Inst Cellular & Mol Biol, Austin, TX 78712 USA. [Ferrari, Frank D.] Smithsonian Inst, Dept Invertebrate Zool, Natl Museum Nat Hist, Suitland, MD USA. [Matz, Mikhail V.] Univ Texas Austin, Sect Integrat Biol, Austin, TX 78712 USA. RP Hunt, ME (reprint author), Univ Texas Austin, Inst Cellular & Mol Biol, Austin, TX 78712 USA. EM matz@mail.utexas.edu OI Matz, Mikhail/0000-0001-5453-9819 FU National Institutes of Health [R01 GM078247]; Ocean Exploration program of the National Oceanic and Atmospheric Administration FX This work was supported by the Ocean Exploration program of the National Oceanic and Atmospheric Administration ("Operation Deep Scope 2007''), and the National Institutes of Health grant R01 GM078247 to M. V. M. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 35 TC 10 Z9 10 U1 1 U2 14 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 185 BERRY ST, STE 1300, SAN FRANCISCO, CA 94107 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD JUL 14 PY 2010 VL 5 IS 7 AR e11517 DI 10.1371/journal.pone.0011517 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 625HA UT WOS:000279884900005 PM 20644720 ER PT J AU Hill, EM Davis, JL Tamisiea, ME Lidberg, M AF Hill, Emma M. Davis, James L. Tamisiea, Mark E. Lidberg, Martin TI Combination of geodetic observations and models for glacial isostatic adjustment fields in Fennoscandia SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH LA English DT Article ID POSTGLACIAL SEA-LEVEL; ICE-AGE EARTH; FORMULATION; EQUATION; RECORDS; SURFACE; GRACE AB We demonstrate a new technique for using geodetic data to update a priori predictions for Glacial Isostatic Adjustment (GIA) in the Fennoscandia region. Global Positioning System (GPS), tide gauge, and Gravity Recovery and Climate Experiment (GRACE) gravity rates are assimilated into our model. The technique allows us to investigate the individual contributions from these data sets to the output GIA model in a self-consistent manner. Another benefit of the technique is that we are able to estimate uncertainties for the output model. These are reduced with each data set assimilated. Any uncertainties in the GPS reference frame are absorbed by reference frame adjustments that are estimated as part of the assimilation. Our updated model shows a spatial pattern and magnitude of peak uplift that is consistent with previous models, but our location of peak uplift is slightly to the east of many of these. We also simultaneously estimate a spatially averaged rate of local sea level rise. This regional rate (similar to 1.5 mm/yr) is consistent for all solutions, regardless of which data sets are assimilated or the magnitude of a priori GPS reference frame constraints. However, this is only the case if a uniform regional gravity rate, probably representing errors in, or unmodeled contributions to, the low-degree harmonic terms from GRACE, is also estimated for the assimilated GRACE data. Our estimated sea level rate is consistent with estimates obtained using a more traditional approach of direct "correction" using collocated GPS and tide gauge sites. C1 [Hill, Emma M.; Davis, James L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Tamisiea, Mark E.] Natl Oceanog Ctr, Liverpool L3 5DA, Merseyside, England. [Lidberg, Martin] Chalmers, Onsala Space Observ, S-41296 Gothenburg, Sweden. RP Hill, EM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 42, Cambridge, MA 02138 USA. EM ehill@cfa.harvard.edu; jdavis@cfa.harvard.edu; mtam@pol.ac.uk; martin.lidberg@lm.se RI Hill, Emma/B-7037-2011; Davis, James/D-8766-2013 OI Hill, Emma/0000-0003-0231-5818; Davis, James/0000-0003-3057-477X FU NASA [NNX08AJ79G, NNX07AM77G]; Natural Environment Research Council FX This work was supported by NASA grants NNX08AJ79G and NNX07AM77G (EMH and JLD), and by the Natural Environment Research Council's Oceans 2025 program (MET). We thank R. Hass for useful discussions regarding least squares collocation, and are grateful to K. Fleming and R. Sabadini for their insightful reviews. This work also benefitted from discussions with members of the Stable North America Reference Frame (SNARF) Working Group. Some figures were generated using the Generic Mapping Tools [Wessel and Smith, 1998]. NR 43 TC 22 Z9 22 U1 2 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SOL EA JI J. Geophys. Res.-Solid Earth PD JUL 13 PY 2010 VL 115 AR B07403 DI 10.1029/2009JB006967 PG 12 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 627OH UT WOS:000280048700005 ER PT J AU Zhao, L Duan, WH Yelin, SF AF Zhao, L. Duan, Wenhui Yelin, S. F. TI All-optical beam control with high speed using image-induced blazed gratings in coherent media SO PHYSICAL REVIEW A LA English DT Article ID ELECTROMAGNETICALLY INDUCED TRANSPARENCY; LIGHT; DESORPTION; PARTICLE; PULSES; ATOMS; STEP AB Based on the theory of electromagnetically induced transparency, we study the formation of all-optical blazed transmission gratings in a coherently driven three-level atomic system using intensity-modulated images in coupling fields. Also, we analyze the feasibility of high-speed (megahertz) modulation for the induced gratings by means of image-bearing flat-top pulse trains. Consequently, continuous-wave probe fields can be efficiently and rapidly deflected in free space. When more sophisticated images are adopted, our scheme can provide further possibilities of all-optical beam splitting and fanning. C1 [Zhao, L.; Duan, Wenhui] Tsinghua Univ, Dept Phys, Beijing 100084, Peoples R China. [Yelin, S. F.] Univ Connecticut, Dept Phys, Storrs, CT 06269 USA. [Yelin, S. F.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RP Zhao, L (reprint author), Tsinghua Univ, Dept Phys, Beijing 100084, Peoples R China. EM zhaol@phys.tsinghua.edu.cn RI Duan, Wenhui /H-4992-2011 OI Duan, Wenhui /0000-0001-9685-2547 FU China Postdoctoral Science Foundation; Ministry of Science and Technology of China [2006CB0L0601]; National Natural Science Foundation of China FX This work was supported by China Postdoctoral Science Foundation, the Ministry of Science and Technology of China (Grant No. 2006CB0L0601), and the National Natural Science Foundation of China. L.Z. thanks R. Zhou and F. Peng for helpful discussions. NR 42 TC 18 Z9 18 U1 1 U2 6 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD JUL 12 PY 2010 VL 82 IS 1 AR 013809 DI 10.1103/PhysRevA.82.013809 PG 8 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 623VQ UT WOS:000279774000015 ER PT J AU Rea, N Torres, DF van der Klis, M Jonker, PG Mendez, M Sierpowska-Bartosik, A AF Rea, N. Torres, D. F. van der Klis, M. Jonker, P. G. Mendez, M. Sierpowska-Bartosik, A. TI Deep Chandra observations of TeV binaries - I. LS I+61 degrees 303 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: individual: LS I+61 degrees 303; X-rays: binaries ID GAMMA-RAY BINARY; 2004 PERIASTRON PASSAGE; XMM-NEWTON OBSERVATIONS; X-RAY; I+61 303; PSR B1259-63; ORBITAL MODULATION; BLACK-HOLE; RADIO; LS-5039 AB We report on a 95 ks Chandra observation of the TeV emitting high-mass X-ray binary LS I +61 degrees 303, using the ACIS-S camera in continuous clocking mode to search for a possible X-ray pulsar in this system. The observation was performed while the compact object was passing from phase 0.94 to 0.98 in its orbit around the Be companion star (hence close to the apastron passage). We did not find any periodic or quasi-periodic signal (at this orbital phase) in a frequency range of 0.005-175 Hz. We derived an average pulsed fraction (PF) 3 Sigma upper limit for the presence of a periodic signal of less than or similar to 10 per cent (although this limit is strongly dependent on the frequency and the energy band), the deepest limit ever reached for this object. Furthermore, the source appears highly variable in flux and spectrum even in this very small orbital phase range, in particular we detect two flares, lasting thousands of seconds, with a very hard X-ray spectrum with respect to the average source spectral distribution. The X-ray PF limits we derived are lower than the PF of any isolated rotational-powered pulsar, in particular having a TeV counterpart. In this scenario, most of the X-ray emission of LS I +61 degrees 303 should necessarily come from the interwind or innerpulsar wind zone shock rather than from the magnetosphere of the putative pulsar. On the other hand, very low X-ray PFs are not unseen in accreting neutron star systems, although we cannot at all exclude the black hole nature of the hosted compact object, a pulsar with a beam pointing away from our line of sight or spinning faster than similar to 5.6 ms, nor that pulsations might have a transient appearance in only a small fraction of the orbit. Furthermore, we did not find evidence for the previously suggested extended X-ray emission. C1 [Rea, N.; Torres, D. F.] Inst Ciencies Espai ICE IEEC CSIC, Fac Ciencies, Barcelona 08193, Spain. [Torres, D. F.] ICREA, Barcelona, Spain. [van der Klis, M.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands. [Jonker, P. G.] SRON, Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. [Jonker, P. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Mendez, M.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Sierpowska-Bartosik, A.] Univ Lodz, Dept Astrophys, PL-90236 Lodz, Poland. RP Rea, N (reprint author), Inst Ciencies Espai ICE IEEC CSIC, Fac Ciencies, Campus UAB,Torre C5 Parell,2A Planta, Barcelona 08193, Spain. EM rea@ieec.uab.es RI Mendez, Mariano/C-8011-2012; Rea, Nanda/I-2853-2015; Torres, Diego/O-9422-2016 OI Mendez, Mariano/0000-0003-2187-2708; Rea, Nanda/0000-0003-2177-6388; Torres, Diego/0000-0002-1522-9065 FU Ramon y Cajal Research; [AYA2009-07391]; [SGR2009-811] FX This research has made use of data from the Chandra X-ray Observatory and software provided by the Chandra X-ray Center. NR is supported by a Ramon y Cajal Research Fellowship to CSIC, and thanks G. L. Israel for useful discussion, advices concerning the timing analysis and for allowing the use of his DPS software. We thank the anonymous referee for his/her very useful suggestions and V. Bosch-Ramon and M. Ribo for comments. This work has been supported by grants AYA2009-07391 and SGR2009-811. NR 59 TC 27 Z9 27 U1 0 U2 1 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUL 11 PY 2010 VL 405 IS 4 BP 2206 EP 2214 DI 10.1111/j.1365-2966.2010.16642.x PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 619SP UT WOS:000279450900006 ER PT J AU Harker, G Zaroubi, S Bernardi, G Brentjens, MA de Bruyn, AG Ciardi, B Jelic, V Koopmans, LVE Labropoulos, P Mellema, G Offringa, A Pandey, VN Pawlik, AH Schaye, J Thomas, RM Yatawatta, S AF Harker, Geraint Zaroubi, Saleem Bernardi, Gianni Brentjens, Michiel A. de Bruyn, A. G. Ciardi, Benedetta Jelic, Vibor Koopmans, Leon V. E. Labropoulos, Panagiotis Mellema, Garrelt Offringa, Andre Pandey, V. N. Pawlik, Andreas H. Schaye, Joop Thomas, Rajat M. Yatawatta, Sarod TI Power spectrum extraction for redshifted 21-cm Epoch of Reionization experiments: the LOFAR case SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE cosmology: theory; diffuse radiation; methods: statistical; radio lines: general ID 21 CENTIMETER FLUCTUATIONS; INTERGALACTIC MEDIUM; COSMIC REIONIZATION; 1ST STARS; FOREGROUNDS; HYDROGEN; LINE; GAS; SIMULATIONS; CONSTRAINTS AB One of the aims of the Low Frequency Array (LOFAR) Epoch of Reionization (EoR) project is to measure the power spectrum of variations in the intensity of redshifted 21-cm radiation from the EoR. The sensitivity with which this power spectrum can be estimated depends on the level of thermal noise and sample variance, and also on the systematic errors arising from the extraction process, in particular from the subtraction of foreground contamination. We model the extraction process using realistic simulations of the cosmological signal, the foregrounds and noise, and so estimate the sensitivity of the LOFAR EoR experiment to the redshifted 21-cm power spectrum. Detection of emission from the EoR should be possible within 360 h of observation with a single station beam. Integrating for longer, and synthesizing multiple station beams within the primary (tile) beam, then enables us to extract progressively more accurate estimates of the power at a greater range of scales and redshifts. We discuss different observational strategies which compromise between depth of observation, sky coverage and frequency coverage. A plan in which lower frequencies receive a larger fraction of the time appears to be promising. We also study the nature of the bias which foreground fitting errors induce on the inferred power spectrum and discuss how to reduce and correct for this bias. The angular and line-of-sight power spectra have different merits in this respect, and we suggest considering them separately in the analysis of LOFAR data. C1 [Harker, Geraint] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Harker, Geraint] NASA, Ames Res Ctr, NASA Lunar Sci Inst, Moffett Field, CA 94035 USA. [Zaroubi, Saleem; Brentjens, Michiel A.; de Bruyn, A. G.; Jelic, Vibor; Koopmans, Leon V. E.; Labropoulos, Panagiotis; Offringa, Andre; Pandey, V. N.; Yatawatta, Sarod] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Bernardi, Gianni] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [de Bruyn, A. G.] ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Ciardi, Benedetta] Max Planck Inst Astrophys, D-85748 Garching, Germany. [Mellema, Garrelt] Stockholm Univ, AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden. [Mellema, Garrelt] Stockholm Univ, AlbaNova, Dept Astron, SE-10691 Stockholm, Sweden. [Pawlik, Andreas H.; Schaye, Joop] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Pawlik, Andreas H.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Thomas, Rajat M.] Univ Tokyo, Inst Math & Phys Universe IPMU, Chiba 2778582, Japan. RP Harker, G (reprint author), Univ Colorado, Ctr Astrophys & Space Astron, 389 UCB, Boulder, CO 80309 USA. EM geraint.harker@colorado.edu RI Jelic, Vibor/B-2938-2014; Thomas, Rajat/B-7105-2014; Mellema, Garrelt/K-4962-2014; Harker, Geraint/C-4885-2012; Ciardi, Benedetta/N-7625-2015; Yatawatta, Sarod/E-6037-2013 OI Schaye, Joop/0000-0002-0668-5560; Jelic, Vibor/0000-0002-6034-8610; Thomas, Rajat/0000-0002-5362-4816; Mellema, Garrelt/0000-0002-2512-6748; Harker, Geraint/0000-0002-7894-4082; Yatawatta, Sarod/0000-0001-5619-4017 FU Netherlands Organisation for Scientific Research (NWO); NASA Lunar Science Institute [NNA09DB30A]; European Union; European Regional Development Fund; 'Samenwerkingsverband Noord-Nederland', EZ/KOMPAS FX For the majority of the period during which this work was undertaken, GH was supported by a grant from the Netherlands Organisation for Scientific Research (NWO), and for the latter part of this period by the LUNAR consortium (http://lunar.colorado.edu) which, headquartered at the University of Colorado, is funded by the NASA Lunar Science Institute (via Cooperative Agreement NNA09DB30A) to investigate concepts for astrophysical observatories on the Moon. As LOFAR members, the authors are partially funded by the European Union, European Regional Development Fund and 'Samenwerkingsverband Noord-Nederland', EZ/KOMPAS. The dark matter simulation was performed on Huygens, the Dutch national supercomputer. We thank the referee, J. Bowman, for suggesting the cross-correlation technique of Section 3.3.3 and for improving the clarity of the presentation. NR 42 TC 81 Z9 81 U1 0 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUL 11 PY 2010 VL 405 IS 4 BP 2492 EP 2504 DI 10.1111/j.1365-2966.2010.16628.x PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 619SP UT WOS:000279450900030 ER PT J AU Nardini, E Risaliti, G Watabe, Y Salvati, M Sani, E AF Nardini, E. Risaliti, G. Watabe, Y. Salvati, M. Sani, E. TI The role of nuclear activity as the power source of ultraluminous infrared galaxies SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; galaxies: starburst; infrared: galaxies ID SPITZER-SPACE-TELESCOPE; PALOMAR-GREEN QUASARS; BAND IMAGING SURVEY; MIDINFRARED SPECTROSCOPY; MU-M; OPTICAL SPECTROSCOPY; IRAS GALAXIES; GALACTIC NUCLEI; HIGH-REDSHIFT; BLACK-HOLES AB We present the results of a 5-8 mu m spectral analysis performed on the largest sample of local ultraluminous infrared galaxies (ULIRGs) selected so far, consisting of 164 objects up to a redshift of similar to 0.35. The unprecedented sensitivity of the Infrared Spectrograph onboard Spitzer allowed us to develop an effective diagnostic method to quantify the active galactic nucleus (AGN) and starburst (SB) contribution to this class of objects. The large AGN over SB brightness ratio at 5-8 mu m and the sharp difference between the spectral properties of AGN and SB galaxies in this wavelength range make it possible to detect even faint or obscured nuclear activity, and disentangle its emission from that of star formation. By defining a simple model we are also able to estimate the intrinsic bolometric corrections for both the AGN and SB components, and obtain the relative AGN/SB contribution to the total luminosity of each source. Our main results are the following. The AGN detection rate among local ULIRGs amounts up to 70 per cent, with 113/164 convincing detections within our sample, while the global AGN/SB power balance is similar to 1/3. A general agreement is found with optical classification; however, among the objects with no spectral signatures of nuclear activity, our IR diagnostics find a subclass of elusive, highly obscured AGN. We analyse the correlation between nuclear activity and IR luminosity, recovering the well-known trend of growing AGN significance as a function of the overall energy output of the system: the sources exclusively powered by star formation are mainly found at L-IR < 1012.3 L-circle dot, while the average AGN contribution rises from similar to 10 to similar to 60 per cent across the ULIRG luminosity range. From a morphological point of view, we confirm that the AGN content is larger in compact systems, but the link between activity and evolutionary stage is rather loose. By analysing a control sample of IR-luminous galaxies around z similar to 1, we find evidence for only minor changes with redshift of the large-scale spectral properties of the AGN and SB components. This underlines the potential of our method as a straightforward and quantitative AGN/SB diagnostic tool for ULIRG-like systems at high redshift as well, and hints to possible photometric variants for fainter sources. C1 [Nardini, E.; Sani, E.] Univ Florence, Dipartimento Fis & Astron, Sez Astron, I-50125 Florence, Italy. [Risaliti, G.; Watabe, Y.; Salvati, M.] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. [Risaliti, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Nardini, E (reprint author), Univ Florence, Dipartimento Fis & Astron, Sez Astron, Lgo E Fermi 2, I-50125 Florence, Italy. EM nardini@arcetri.astro.it OI Risaliti, Guido/0000-0002-3556-977X FU NASA [NNX09AT10G, ASI-INAF I/088/06/0] FX We are grateful to the anonymous referee for the constructive comments and suggestions. This work has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. We acknowledge financial support from NASA grant NNX09AT10G and ASI-INAF I/088/06/0 contract. NR 92 TC 54 Z9 54 U1 0 U2 3 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUL 11 PY 2010 VL 405 IS 4 BP 2505 EP 2520 DI 10.1111/j.1365-2966.2010.16618.x PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 619SP UT WOS:000279450900031 ER PT J AU Villegas, D Jordan, A Peng, EW Blakeslee, JP Cote, P Ferrarese, L Kissler-Patig, M Mei, S Infante, L Tonry, JL West, MJ AF Villegas, Daniela Jordan, Andres Peng, Eric W. Blakeslee, John P. Cote, Patrick Ferrarese, Laura Kissler-Patig, Markus Mei, Simona Infante, Leopoldo Tonry, John L. West, Michael J. TI THE ACS FORNAX CLUSTER SURVEY. VIII. THE LUMINOSITY FUNCTION OF GLOBULAR CLUSTERS IN VIRGO AND FORNAX EARLY-TYPE GALAXIES AND ITS USE AS A DISTANCE INDICATOR SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: elliptical and lenticular, cD; galaxies: star clusters: general; globular clusters: general ID DATA REDUCTION PROCEDURES; DWARF ELLIPTIC GALAXIES; TELESCOPE KEY PROJECT; MEASURING EXTRAGALACTIC DISTANCES; INITIAL MASS FUNCTION; HUBBLE CONSTANT; STAR-CLUSTERS; DYNAMICAL EVOLUTION; PLANETARY-NEBULAE; FUNDAMENTAL PLANE AB We use a highly homogeneous set of data from 132 early-type galaxies in the Virgo and Fornax clusters in order to study the properties of the globular cluster luminosity function (GCLF). The globular cluster system of each galaxy was studied using a maximum likelihood approach to model the intrinsic GCLF after accounting for contamination and completeness effects. The results presented here update our Virgo measurements and confirm our previous results showing a tight correlation between the dispersion of the GCLF and the absolute magnitude of the parent galaxy. Regarding the use of the GCLF as a standard candle, we have found that the relative distance modulus between the Virgo and Fornax clusters is systematically lower than the one derived by other distance estimators, and in particular, it is 0.22 mag lower than the value derived from surface brightness fluctuation measurements performed on the same data. From numerical simulations aimed at reproducing the observed dispersion of the value of the turnover magnitude in each galaxy cluster we estimate an intrinsic dispersion on this parameter of 0.21 mag and 0.15 mag for Virgo and Fornax, respectively. All in all, our study shows that the GCLF properties vary systematically with galaxy mass showing no evidence for a dichotomy between giant and dwarf early-type galaxies. These properties may be influenced by the cluster environment as suggested by cosmological simulations. C1 [Villegas, Daniela; Kissler-Patig, Markus] European So Observ, D-85748 Garching, Germany. [Jordan, Andres; Infante, Leopoldo] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 7820436, Chile. [Jordan, Andres] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Peng, Eric W.] Peking Univ, Dept Astron, Beijing 100871, Peoples R China. [Blakeslee, John P.; Cote, Patrick; Ferrarese, Laura] Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Mei, Simona] Univ Paris Denis Diderot, F-75205 Paris 13, France. [Mei, Simona] Observ Paris, GEPI, Sect Meudon, F-92195 Meudon, France. [Tonry, John L.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [West, Michael J.] European So Observ, Santiago 19001, Chile. RP Villegas, D (reprint author), European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. OI Jordan, Andres/0000-0002-5389-3944; Blakeslee, John/0000-0002-5213-3548 FU Space Telescope Science Institute [GO-9401, GO-10217]; NASA [NAS5-26555]; Chilean Center of Excellence in Astrophysics and Associated Technologies [PFB 06]; Chilean Center for Astrophysics FONDAP [15010003]; MIDEPLAN's Programa Inicativa Cientifica Milenio [P07-021-F]; National Aeronautics and Space Administration FX Support for programs GO-9401 and GO-10217 was provided through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. A.J. and L.I. acknowledge support from the Chilean Center of Excellence in Astrophysics and Associated Technologies (PFB 06) and from the Chilean Center for Astrophysics FONDAP 15010003. Additional support for A.J. is provided by MIDEPLAN's Programa Inicativa Cientifica Milenio through grant P07-021-F. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 81 TC 56 Z9 56 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2010 VL 717 IS 2 BP 603 EP 616 DI 10.1088/0004-637X/717/2/603 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 635JG UT WOS:000280650800001 ER PT J AU Quanz, SP Beuther, H Steinacker, J Linz, H Birkmann, SM Krause, O Henning, T Zhang, QZ AF Quanz, Sascha P. Beuther, Henrik Steinacker, Juergen Linz, Hendrik Birkmann, Stephan M. Krause, Oliver Henning, Thomas Zhang, Qizhou TI A LARGE, MASSIVE, ROTATING DISK AROUND AN ISOLATED YOUNG STELLAR OBJECT SO ASTROPHYSICAL JOURNAL LA English DT Article DE protoplanetary disks; stars: formation; stars: pre-main sequence ID STAR-FORMATION; CIRCUMSTELLAR DISKS; PROTOPLANETARY DISKS; PHYSICAL CONDITIONS; BIPOLAR OUTFLOW; IRAS 18059-3211; DARK CLOUDS; T-TAURI; DUST; ACCRETION AB We present multi-wavelength observations and a radiative transfer model of a newly discovered massive circumstellar disk of gas and dust which is one of the largest disks known today. Seen almost edge-on, the disk is resolved in high-resolution near-infrared (NIR) images and appears as a dark lane of high opacity intersecting a bipolar reflection nebula. Based on molecular line observations, we estimate the distance to the object to be 3.5 kpc. This leads to a size for the dark lane of similar to 10,500 AU but due to shadowing effects the true disk size could be smaller. In Spitzer/IRAC 3.6 mu m images, the elongated shape of the bipolar reflection nebula is still preserved and the bulk of the flux seems to come from disk regions that can be detected due to the slight inclination of the disk. At longer IRAC wavelengths, the flux is mainly coming from the central regions penetrating directly through the dust lane. Interferometric observations of the dust continuum emission at millimeter wavelengths with the Submillimeter Array confirm this finding as the peak of the unresolved millimeter-emission coincides perfectly with the peak of the Spitzer/IRAC 5.8 mu m flux and the center of the dark lane seen in the NIR images. Simultaneously acquired CO data reveal a molecular outflow along the northern part of the reflection nebula which seems to be the outflow cavity. An elongated gaseous disk component is also detected and shows signs of rotation. The emission is perpendicular to the molecular outflow and thus parallel to but even more extended than the dark lane in the NIR images. Based on the dust continuum and the CO observations, we estimate a disk mass of up to a few solar masses depending on the underlying assumptions. Whether the disk-like structure is an actual accretion disk or rather a larger-scale flattened envelope or pseudodisk is difficult to discriminate with the current data set. The existence of HCO(+)/H(13)CO(+) emission proves the presence of dense gas in the disk and the molecules' abundances are similar to those found in other circumstellar disks. We furthermore detected C(2)H toward the objects and discuss this finding in the context of star formation. Finally, we have performed radiative transfer modeling of the K-band scattered light image varying a disk plus outflow two-dimensional density profile and the stellar properties. The model approximately reproduces extent and location of the dark lane, and the basic appearance of the outflow. We discuss our findings in the context of circumstellar disks across all mass regimes and conclude that our discovery is an ideal laboratory to study the early phases in the evolution of massive circumstellar disks surrounding young stellar objects. C1 [Quanz, Sascha P.] ETH, Inst Astron, CH-8093 Zurich, Switzerland. [Quanz, Sascha P.; Beuther, Henrik; Steinacker, Juergen; Linz, Hendrik; Krause, Oliver; Henning, Thomas] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Steinacker, Juergen] Observ Paris, LERMA, F-75014 Paris, France. [Birkmann, Stephan M.] ESA, Estec, NL-2200 AG Noordwijk, Netherlands. [Zhang, Qizhou] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Quanz, SP (reprint author), ETH, Inst Astron, Wolfgang Pauli Str 27, CH-8093 Zurich, Switzerland. EM quanz@astro.phys.ethz.ch OI Zhang, Qizhou/0000-0003-2384-6589 FU NASA FX Based on observations made at the Calar Alto Observatory. This work is based in part on data collected at Subaru Telescope, which is operated by the National Astronomical Observatory of Japan, and on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. NR 83 TC 8 Z9 8 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2010 VL 717 IS 2 BP 693 EP 707 DI 10.1088/0004-637X/717/2/693 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 635JG UT WOS:000280650800009 ER PT J AU Leipski, C Haas, M Willner, SP Ashby, MLN Wilkes, BJ Fazio, GG Antonucci, R Barthel, P Chini, R Siebenmorgen, R Ogle, P Heymann, F AF Leipski, C. Haas, M. Willner, S. P. Ashby, M. L. N. Wilkes, B. J. Fazio, G. G. Antonucci, R. Barthel, P. Chini, R. Siebenmorgen, R. Ogle, P. Heymann, F. TI MID-INFRARED SPECTROSCOPY OF HIGH-REDSHIFT 3CRR SOURCES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: high-redshift; infrared: galaxies ID ACTIVE GALACTIC NUCLEI; SPECTRAL ENERGY-DISTRIBUTIONS; INTERSTELLAR EXTINCTION LAW; POWERFUL RADIO GALAXIES; SPITZER-SPACE-TELESCOPE; 8.0 MU-M; UNIFIED SCHEMES; KECK SPECTROPOLARIMETRY; INFRARED OBSERVATIONS; SILICATE FEATURES AB Using the Spitzer Space Telescope, we have obtained rest-frame 9-16 mu m spectra of 11 quasars and 9 radio galaxies from the 3CRR catalog at redshifts 1.0 < z < 1.4. This complete flux-limited 178 MHz selected sample is unbiased with respect to orientation and therefore suited to studying orientation-dependent effects in the most powerful active galactic nuclei (AGNs). The mean radio-galaxy spectrum shows a clear silicate absorption feature (tau(9.7 mu m) = 1.1) whereas the mean quasar spectrum shows silicates in emission. The mean radio-galaxy spectrum matches a dust-absorbed mean quasar spectrum in both shape and overall flux level. The data for individual objects conform to these results. The trend of the silicate depth to increase with decreasing core fraction of the radio source further supports that for this sample orientation is the main driver for the difference between radio galaxies and quasars, as predicted by AGN unification. However, comparing our high-z sample with lower redshift 3CRR objects reveals that the absorption of the high-z radio galaxy MIR continuum is lower than expected from a scaled-up version of lower luminosity sources, and we discuss some effects that may explain these trends. C1 [Leipski, C.; Antonucci, R.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Haas, M.; Chini, R.; Heymann, F.] Ruhr Univ Bochum, Astron Inst, D-44801 Bochum, Germany. [Willner, S. P.; Ashby, M. L. N.; Wilkes, B. J.; Fazio, G. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Barthel, P.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Siebenmorgen, R.; Heymann, F.] European So Observ, D-85748 Garching, Germany. [Ogle, P.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. RP Leipski, C (reprint author), Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. EM leipski@physics.ucsb.edu OI Wilkes, Belinda/0000-0003-1809-2364 FU NASA, JPL/Caltech; National Aeronautics and Space Administration FX This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. 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. M. H. is supported by Nordrhein-Westfalische Akademie der Wissenschaften und der Kunste. NR 73 TC 26 Z9 26 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2010 VL 717 IS 2 BP 766 EP 775 DI 10.1088/0004-637X/717/2/766 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 635JG UT WOS:000280650800013 ER PT J AU Dobler, G Finkbeiner, DP Cholis, I Slatyer, T Weiner, N AF Dobler, Gregory Finkbeiner, Douglas P. Cholis, Ilias Slatyer, Tracy Weiner, Neal TI THE FERMI HAZE: A GAMMA-RAY COUNTERPART TO THE MICROWAVE HAZE SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays: general; gamma rays: ISM ID LUMINOSITY FUNCTION; SOURCE LIST; RADIATION; EMISSION; BINARIES; GALAXY; INDICATOR; SKY AB The FermiGamma-ray Space Telescope reveals a diffuse inverse Compton (IC) signal in the inner Galaxy with a similar spatial morphology to the microwave haze observed by WMAP, supporting the synchrotron interpretation of the microwave signal. Using spatial templates, we regress out pi(0) gammas, as well as IC and bremsstrahlung components associated with known soft-synchrotron counterparts. We find a significant gamma-ray excess toward the Galactic center with a spectrum that is significantly harder than other sky components and is most consistent with IC from a hard population of electrons. The morphology and spectrum are consistent with it being the IC counterpart to the electrons which generate the microwave haze seen at WMAP frequencies. In addition, the implied electron spectrum is hard; electrons accelerated in supernova shocks in the disk which then diffuse a few kpc to the haze region would have a softer spectrum. We describe the full-sky Fermi maps used in this analysis and make them available for download. C1 [Dobler, Gregory; Finkbeiner, Douglas P.; Slatyer, Tracy] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. [Dobler, Gregory] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA. [Finkbeiner, Douglas P.; Slatyer, Tracy] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Cholis, Ilias; Weiner, Neal] NYU, Dept Phys, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. RP Dobler, G (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St,MS 51, Cambridge, MA 02138 USA. EM dobler@kitp.ucsb.edu NR 40 TC 129 Z9 129 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2010 VL 717 IS 2 BP 825 EP 842 DI 10.1088/0004-637X/717/2/825 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 635JG UT WOS:000280650800018 ER PT J AU ZuHone, JA Markevitch, M Johnson, RE AF ZuHone, J. A. Markevitch, M. Johnson, R. E. TI STIRRING UP THE POT: CAN COOLING FLOWS IN GALAXY CLUSTERS BE QUENCHED BY GAS SLOSHING? SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: general; galaxies: clusters: intracluster medium; methods: numerical; X-rays: galaxies: clusters ID X-RAY SPECTROSCOPY; DARK-MATTER HALOS; THERMAL CONDUCTION; CHANDRA OBSERVATION; HIGH-RESOLUTION; PERSEUS CLUSTER; COLD FRONTS; MERGERS; CORES; TEMPERATURE AB X-ray observations of clusters of galaxies reveal the presence of edges in surface brightness and temperature, known as "cold fronts." In relaxed clusters with cool cores, these commonly observed edges have been interpreted as evidence for the "sloshing" of the core gas in the cluster's gravitational potential. Such sloshing may provide a source of heat to the cluster core by mixing hot gas from the cluster outskirts with the cool-core gas. Using high-resolution N-body/Eulerian hydrodynamic simulations, we model gas sloshing in galaxy clusters initiated by mergers with subclusters. The simulations include merger scenarios with gas-filled and gasless subclusters. The effect of changing the viscosity of the intracluster medium is also explored, but heat conduction is assumed to be negligible. We find that sloshing can facilitate heat inflow to the cluster core, provided that there is a strong enough disturbance. Additionally, sloshing redistributes the gas in the cluster core, causing the gas to expand and decreasing the efficiency of radiative cooling. In adiabatic simulations, we find that sloshing can raise the entropy floor of the cluster core by nearly an order of magnitude in the strongest cases. If the ICM is viscous, the mixing of gases with different entropies is decreased and consequently the heat flux to the core is diminished. In simulations where radiative cooling is included, we find that although eventually a cooling flow develops, sloshing can prevent the significant buildup of cool gas in the core for times on the order of a Gyr for small disturbances and a few Gyr for large ones. If repeated encounters with merging subclusters sustain the sloshing of the central core gas, as is observed, this process can provide a relatively steady source of heat to the core, which can help prevent a significant cooling flow. C1 [ZuHone, J. A.; Markevitch, M.; Johnson, R. E.] Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Johnson, R. E.] Dartmouth Coll, Wilder Lab, Dept Phys & Astron, Hanover, NH 03755 USA. RP ZuHone, JA (reprint author), Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. NR 66 TC 85 Z9 85 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2010 VL 717 IS 2 BP 908 EP 928 DI 10.1088/0004-637X/717/2/908 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 635JG UT WOS:000280650800025 ER PT J AU Ruiter, AJ Belczynski, K Benacquista, M Larson, SL Williams, G AF Ruiter, Ashley J. Belczynski, Krzysztof Benacquista, Matthew Larson, Shane L. Williams, Gabriel TI THE LISA GRAVITATIONAL WAVE FOREGROUND: A STUDY OF DOUBLE WHITE DWARFS SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; gravitation; gravitational waves; stars: evolution; white dwarfs ID INTERFEROMETER-SPACE-ANTENNA; CANUM-VENATICORUM BINARIES; AM CVN STARS; COMMON ENVELOPE EVOLUTION; DIGITAL SKY SURVEY; X-RAY SOURCES; POPULATION SYNTHESIS; GALACTIC BINARIES; DETACHED SYSTEMS; COMPACT OBJECTS AB Double white dwarfs (WDs) are expected to be a source of confusion-limited noise for the future gravitational wave observatory LISA. In a specific frequency range, this "foreground noise" is predicted to rise above the instrumental noise and hinder the detection of other types of signals, e. g., gravitational waves arising from stellar-mass objects inspiraling intomassive black holes. Inmany previous studies, only detached populations of compact object binaries have been considered in estimating the LISA gravitational wave foreground signal. Here, we investigate the influence of compact object detached and Roche-Lobe overflow (RLOF) Galactic binaries on the shape and strength of the LISA signal. Since > 99% of remnant binaries that have orbital periods within the LISA sensitivity range are WD binaries, we consider only these binaries when calculating the LISA signal. We find that the contribution of RLOF binaries to the foreground noise is negligible at low frequencies, but becomes significant at higher frequencies, pushing the frequency at which the foreground noise drops below the instrumental noise to > 6 mHz. We find that it is important to consider the population of mass-transferring binaries in order to obtain an accurate assessment of the foreground noise on the LISA data stream. However, we estimate that there still exists a sizeable number (similar to 11,300) of Galactic double WD binaries that will have a signal-to-noise ratio > 5, and thus will be potentially resolvable with LISA. We present the LISA gravitational wave signal from the Galactic population of WD binaries, show the most important formation channels contributing to the LISA disk and bulge populations, and discuss the implications of these new findings. C1 [Ruiter, Ashley J.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Ruiter, Ashley J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ruiter, Ashley J.] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA. [Belczynski, Krzysztof] Los Alamos Natl Lab, CCS 2, ISR Grp 1, Los Alamos, NM 87545 USA. [Belczynski, Krzysztof] Univ Warsaw, Astron Observ, PL-00478 Warsaw, Poland. [Benacquista, Matthew; Williams, Gabriel] Univ Texas Brownsville, Ctr Gravitat Wave Astron, Brownsville, TX 78520 USA. [Larson, Shane L.] Utah State Univ, Dept Phys, Logan, UT 84322 USA. [Williams, Gabriel] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA. RP Ruiter, AJ (reprint author), Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85741 Garching, Germany. EM ajr@mpa-garching.mpg.de; kbelczyn@nmsu.edu; benacquista@phys.utb.edu; s.larson@usu.edu; gabriel.j.williams@gmail.com RI Larson, Shane/E-8576-2010 FU NASA [NNG05G106G, NNG04GD52G, NNG05GF71G]; KBN [1 P03D 022 28, PBZ-KBN-054/P03/2001]; Center for Gravitational Wave Astronomy; NSF [PHY 01-4375] FX We thank Gijs Nelemans for very useful discussion on this project, which greatly improved this work, and for providing data for Nelemans et al. (2001b) and Nelemans et al. (2004). K.B., M.B., and S.L.L. acknowledge the hospitality of the Aspen Center for Physics. M. B. and S.L.L. were supported at the Aspen Center by NASA Award Number NNG05G106G. M.B. is also supported by NASA APRA grant Number NNG04GD52G. K.B. and A.J.R. acknowledge support through KBN Grants 1 P03D 022 28 and PBZ-KBN-054/P03/2001, and the hospitality of the Center for Gravitational Wave Astronomy (UTB). S.L.L. also acknowledges support from the Center for Gravitational Wave Physics, funded by the NSF under cooperative agreement PHY 01-4375, and from NASA award NNG05GF71G. A.J.R. acknowledges the support of Sigma Xi and the hospitality of the Nicolaus Copernicus Astronomical Center. The majority of A.J.R.'s calculations for this work were carried out at New Mexico State University and the Harvard-Smithsonian Center for Astrophysics. The authors also thank Sam Finn for directing us to the KDE package for Matlab, which was used to generate the PDFs of the various channels, and Joe Romano for providing a routine for generating the LISA noise. Finally, we thank the referee Gijs Nelemans and the anonymous referee for highly insightful questions and comments. StarTrack simulations were performed at the Copernicus Center in Warsaw, Poland. NR 88 TC 34 Z9 34 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2010 VL 717 IS 2 BP 1006 EP 1021 DI 10.1088/0004-637X/717/2/1006 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 635JG UT WOS:000280650800033 ER PT J AU Park, SQ Barmby, P Willner, SP Ashby, MLN Fazio, GG Georgakakis, A Ivison, RJ Konidaris, NP Miyazaki, S Nandra, K Rosario, DJ AF Park, S. Q. Barmby, P. Willner, S. P. Ashby, M. L. N. Fazio, G. G. Georgakakis, A. Ivison, R. J. Konidaris, N. P. Miyazaki, S. Nandra, K. Rosario, D. J. TI AEGIS: A MULTIWAVELENGTH STUDY OF SPITZER POWER-LAW GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; infrared: galaxies; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; EXTENDED GROTH STRIP; DEEP FIELD-NORTH; SPECTRAL ENERGY-DISTRIBUTIONS; DIGITAL SKY SURVEY; X-RAY-SPECTRA; SUPERMASSIVE BLACK-HOLES; DUST-OBSCURED GALAXIES; STAR-FORMING GALAXIES; SEYFERT-GALAXIES AB This paper analyzes a sample of 489 Spitzer/Infrared Array Camera (IRAC) sources in the Extended Groth Strip (EGS), whose spectral energy distributions fit a red power law (PL) from 3.6 to 8.0 mu m. The median redshift for sources with known redshifts is < z > = 1.6. Though all or nearly all of the sample galaxies are likely to be active galactic nuclei (AGNs), only 33% were detected in the EGS X-ray survey (AEGIS-X) using 200 ks Chandra observations. The detected sources are X-ray luminous with L(X) > 10(43) erg s(-1) and moderately to heavily obscured with N(H) > 10(22) cm(-2). Stacking the X-ray-undetected sample members yields a statistically significant X-ray signal, suggesting that they are on average more distant or more obscured than sources with X-ray detections. The ratio of X-ray to mid-infrared fluxes suggests that a substantial fraction of the sources undetected in X-rays are obscured at the Compton-thick level, in contrast to the X-ray-detected sources, all of which appear to be Compton thin. For the X-ray-detected PL sources with redshifts, an Xray luminosity L(X) similar to 10(44) erg s(-1) marks a transition between low-luminosity, blue sources dominated by the host galaxy to high-luminosity, red PL sources dominated by nuclear activity. X-ray-to-optical ratios, infrared variability, and 24 mu m properties of the sample are consistent with the identification of infrared PL sources as active nuclei, but a rough estimate is that only 22% of AGNs are selected by the PL criteria. Comparison of the PL selection technique and various IRAC color criteria for identifying AGNs confirms that high-redshift samples selected via simple IRAC colors may be heavily contaminated by starlight-dominated objects. C1 [Park, S. Q.; Barmby, P.; Willner, S. P.; Ashby, M. L. N.; Fazio, G. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Barmby, P.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [Georgakakis, A.] Natl Observ Athens, Athens 15236, Greece. [Ivison, R. J.] Royal Observ, Sci & Technol Facil Council, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Ivison, R. J.] Univ Edinburgh, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Konidaris, N. P.; Rosario, D. J.] Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA. [Miyazaki, S.] Natl Astron Observ Japan, Tokyo 1818588, Japan. [Nandra, K.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England. RP Park, SQ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM spark@cfa.harvard.edu RI Georgakakis, Antonis/K-4457-2013; Barmby, Pauline/I-7194-2016; Ivison, R./G-4450-2011; OI Barmby, Pauline/0000-0003-2767-0090; Ivison, R./0000-0001-5118-1313; Georgakakis, Antonis/0000-0002-3514-2442 FU NASA FX We thank Mark Dickinson for supplying FIDEL data in advance of publication, and Alison Coil and Christopher Willmer for advice concerning the spectroscopic data. This study has made use of data from AEGIS, a multiwavelength sky survey conducted with Chandra, GALEX, Hubble, Spitzer, Keck, Palomar, CFHT, MMT, Subaru, VLA, and other telescopes and supported in part by the NSF and NASA. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA. This work is based in part on data collected at Subaru telescope, which is operated by the National Astronomical Observatory of Japan and on observations obtained with MegaPrime/MegaCam, a joint project of Canada-France-Hawaii Telescope (CFHT) and CEA/DAPNIA, at the CFHT which is operated by the National Research Council (NRC) of Canada, the Institut National des Sciences de l'Univers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawaii. This work is based in part on data products produced at TERAPIX and the Canadian Astronomy Data Centre as part of the CFHT Legacy Survey, a collaborative project of NRC and CNRS. The observations reported here were obtained in part at the MMT Observatory, a facility operated jointly by the Smithsonian Institution and the University of Arizona. P.B acknowledges research support from the Natural Sciences and Engineering Research Council of Canada. NR 105 TC 22 Z9 22 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2010 VL 717 IS 2 BP 1181 EP 1201 DI 10.1088/0004-637X/717/2/1181 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 635JG UT WOS:000280650800045 ER PT J AU Tang, YW Ho, PTP Koch, PM Rao, R AF Tang, Ya-Wen Ho, Paul T. P. Koch, Patrick M. Rao, Ramprasad TI HIGH-ANGULAR RESOLUTION DUST POLARIZATION MEASUREMENTS: SHAPED B-FIELD LINES IN THE MASSIVE STAR-FORMING REGION ORION BN/KL SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual objects (Orion BN/KL, M42); ISM: magnetic fields; polarization; stars: formation ID MAGNETIC-FIELD; SUBMILLIMETER ARRAY; MOLECULAR CLOUDS; SOURCE I; KL; OMC-1; EMISSION; OUTFLOW; NEBULA; KINEMATICS AB We present observational results of the thermal dust continuum emission and its linear polarization in one of the nearest massive star-forming sites Orion BN/KL in Orion Molecular Cloud-1. The observations were carried out with the Submillimeter Array. With an angular resolution of 1 '' (similar to 2 mpc; 480 AU), we have detected and resolved the densest cores near the BN/KL region. At a wavelength of similar to 870 mu m, the polarized dust emission can be used to trace the structure of the magnetic field in this star-forming core. The dust continuum appears to arise from a V-shaped region, with a cavity nearly coincident with the center of the explosive outflows observed on larger scales. The position angles (P.A.s) of the observed polarization vary significantly by a total of about 90 degrees but smoothly, i.e., curl-like, across the dust ridges. Such a polarization pattern can be explained with dust grains being magnetically aligned instead of mechanically with outflows, since the latter mechanism would cause the P.A.s to be parallel to the direction of the outflow, i.e., radial-like. The magnetic field projected in the plane of sky is therefore derived by rotating the P.A.s of the polarization by 90 degrees. We find an azimuthally symmetric structure in the overall magnetic field morphology, with the field directions pointing toward 2 ''.5 west to the center of the explosive outflows. We also find a preferred symmetry plane at a P.A. of 36 degrees, which is perpendicular to the mean magnetic field direction (120 degrees) of the 0.5 pc dust ridge. Two possible interpretations of the origin of the observedmagnetic field structure are discussed. C1 [Tang, Ya-Wen; Ho, Paul T. P.; Koch, Patrick M.; Rao, Ramprasad] Acad Sinica, Inst Astron & Astrophys, Taipei, Taiwan. [Ho, Paul T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Tang, YW (reprint author), Acad Sinica, Inst Astron & Astrophys, Taipei, Taiwan. EM ywtang@asiaa.sinica.edu.tw OI Tang, Ya-Wen/0000-0002-0675-276X FU NSC [NSC97-2112-M-001-007-MY3, NSC98-2119-M-001-024-MY4] FX The authors acknowledge the anonymous referee for the helpful comments, which have improved the presentation of the paper. Y.-W.T. is grateful to Josep M. Girart and Mike Cai for the interesting discussions. Y.-W.T. and P.T.P.H. are supported by NSC grants NSC97-2112-M-001-007-MY3 and NSC98-2119-M-001-024-MY4. NR 50 TC 29 Z9 29 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2010 VL 717 IS 2 BP 1262 EP 1273 DI 10.1088/0004-637X/717/2/1262 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 635JG UT WOS:000280650800052 ER PT J AU Hartman, JD AF Hartman, J. D. TI CORRELATION BETWEEN STELLAR ACTIVITY AND THE SURFACE GRAVITY OF HOT JUPITERS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE methods: statistical; planetary systems; stars: activity ID TRANSITING EXTRASOLAR PLANETS; LOWER MAIN-SEQUENCE; LOW-DENSITY PLANET; GIANT PLANETS; LIGHT-CURVE; MAGNETIC ACTIVITY; ECCENTRIC ORBIT; KEPLER FIELD; SHORT-TERM; K DWARF AB Recently, Knutson et al. have demonstrated a correlation between the presence of temperature inversions in the atmospheres of hot Jupiters and the chromospheric activity levels of the host stars. Here, we show that there is also a correlation, with greater than 99.5% confidence, between the surface gravity of hot Jupiters and the activity levels of the host stars, such that high surface gravity planets tend be found around high-activity stars. We also find a less significant positive correlation between planet mass and chromospheric activity, but no significant correlation is seen between planet radius and chromospheric activity. We consider the possibility that this may be due to an observational bias against detecting lower mass planets around higher activity stars, but conclude that this bias is only likely to affect the detection of planets much smaller than those considered here. Finally, we speculate on physical origins for the correlation-including the possibility that the effect of stellar insolation on planetary radii has been significantly underestimated, that strong UV flux evaporates planetary atmospheres, or that high-mass hot Jupiters induce activity in their host stars-but do not find any of these hypotheses to be particularly compelling. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Hartman, JD (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jhartman@cfa.harvard.edu OI Hartman, Joel/0000-0001-8732-6166 FU NASA [NNG04GN74G, NNX08AF23G]; SAO IRD FX I am greatly indebted to H. Knutson, A. Howard, and H. Isaacson for publishing the log R'HK values on which this study is based. I also thank R. Noyes, G. Bakos, and H. Knutson for helpful discussions and comments on this Letter, A. Howard for helpful comments, in particular for pointing out the need to correct for the number of independent trials in determining the FAP, and J. Fortney for helpful comments, in particular for suggesting that planetary evaporation could explain the apparent correlation. Finally, I thank the anonymous referee for a careful review of this Letter and for several helpful comments. Support for this work is through the HATNet project, via NASA grants NNG04GN74G, NNX08AF23G and SAO IR&D grants. NR 48 TC 26 Z9 26 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUL 10 PY 2010 VL 717 IS 2 BP L138 EP L142 DI 10.1088/2041-8205/717/2/L138 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 619LC UT WOS:000279430700013 ER PT J AU Hui, YW Schultz, DR Kharchenko, VA Bhardwaj, A Branduardi-Raymont, G Stancil, PC Cravens, TE Lisse, CM Dalgarno, A AF Hui, Yawei Schultz, David R. Kharchenko, Vasili A. Bhardwaj, Anil Branduardi-Raymont, Graziella Stancil, Phillip C. Cravens, Thomas E. Lisse, Carey M. Dalgarno, Alexander TI Comparative analysis and variability of the Jovian X-ray spectra detected by the Chandra and XMM-Newton observatories SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID EMISSION; JUPITER; OXYGEN; IONS; PRECIPITATION; TRANSITIONS; ATMOSPHERE; COMETS; AURORA; E1 AB Expanding upon recent work, a more comprehensive spectral model based on charge exchange induced X-ray emission by ions precipitating into the Jovian atmosphere is used to provide new understanding of the polar auroras. In conjunction with the Xspec spectral fitting software, the model is applied to analyze observations from both Chandra and XMM-Newton by systematically varying the initial precipitating ion parameters to obtain the best fit model for the observed spectra. In addition to the oxygen and sulfur ions considered previously, carbon is included to discriminate between solar wind and Jovian magnetospheric ion origins, enabled by the use of extensive databases of both atomic collision cross sections and radiative transitions. On the basis of fits to all the Chandra observations, we find that carbon contributes negligibly to the observed polar X-ray emission suggesting that the highly accelerated precipitating ions are of magnetospheric origin. Most of the XMM-Newton fits also favor this conclusion with one exception that implies a possible carbon contribution. Comparison among all the spectra from these two observatories in light of the inferred initial energies and relative abundances of precipitating ions from the modeling show that they are significantly variable in time (observation date) and space (north and south polar X-ray auroras). C1 [Hui, Yawei; Schultz, David R.] Oak Ridge Natl Lab, Div Phys, Oak Ridge, TN 37831 USA. [Kharchenko, Vasili A.] Univ Connecticut, Dept Phys, Storrs, CT 06269 USA. [Bhardwaj, Anil] Vikram Sarabhai Space Ctr, Space Phys Lab, Trivandrum 695022, Kerala, India. [Branduardi-Raymont, Graziella] Univ Coll London, Mullard Space Sci Lab, Surrey RH5 6NT, England. [Stancil, Phillip C.] Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA. [Stancil, Phillip C.] Univ Georgia, Ctr Simulat Phys, Athens, GA 30602 USA. [Cravens, Thomas E.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA. [Lisse, Carey M.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Dalgarno, Alexander] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Hui, YW (reprint author), Oak Ridge Natl Lab, Div Phys, Bldg 6010, Oak Ridge, TN 37831 USA. EM huiy@ornl.gov; schultzd@ornl.gov; kharchenko@phys.uconn.edu; gbr@mssl.ucl.ac.uk; stancil@physast.uga.edu; cravens@ku.edu; carey.lisse@jhuapl.edu; adalgarno@cfa.harvard.edu RI Lisse, Carey/B-7772-2016; OI Lisse, Carey/0000-0002-9548-1526; Bhardwaj, Anil/0000-0003-1693-453X FU NASA [NNH07AF12I] FX This work has been supported by NASA Planetary Atmospheres Program grant NNH07AF12I. We are grateful to the Chandra Helpdesk staff, particularly Elizabeth Galle, for assistance with processing the raw observations files. We also acknowledge Glenn E. Allen who coded the new Chandra data reduction algorithms. NR 33 TC 15 Z9 15 U1 1 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD JUL 8 PY 2010 VL 115 AR A07102 DI 10.1029/2009JA014854 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 624NQ UT WOS:000279826200003 ER PT J AU Kitahara, MV Cairns, SD Stolarski, J Blair, D Miller, DJ AF Kitahara, Marcelo V. Cairns, Stephen D. Stolarski, Jaroslaw Blair, David Miller, David J. TI A Comprehensive Phylogenetic Analysis of the Scleractinia (Cnidaria, Anthozoa) Based on Mitochondrial CO1 Sequence Data SO PLOS ONE LA English DT Article ID PHYLUM CNIDARIA; EVOLUTIONARY RELATIONSHIPS; CORALS; SYSTEMATICS; CLASSIFICATION; HEXACORALLIA; INFERENCE; ATLANTIC; PACIFIC; BIOLOGY AB Background: Classical morphological taxonomy places the approximately 1400 recognized species of Scleractinia (hard corals) into 27 families, but many aspects of coral evolution remain unclear despite the application of molecular phylogenetic methods. In part, this may be a consequence of such studies focusing on the reef-building (shallow water and zooxanthellate) Scleractinia, and largely ignoring the large number of deep-sea species. To better understand broad patterns of coral evolution, we generated molecular data for a broad and representative range of deep sea scleractinians collected off New Caledonia and Australia during the last decade, and conducted the most comprehensive molecular phylogenetic analysis to date of the order Scleractinia. Methodology: Partial (595 bp) sequences of the mitochondrial cytochrome oxidase subunit 1 (CO1) gene were determined for 65 deep-sea (azooxanthellate) scleractinians and 11 shallow-water species. These new data were aligned with 158 published sequences, generating a 234 taxon dataset representing 25 of the 27 currently recognized scleractinian families. Principal Findings/Conclusions: There was a striking discrepancy between the taxonomic validity of coral families consisting predominantly of deep-sea or shallow-water species. Most families composed predominantly of deep-sea azooxanthellate species were monophyletic in both maximum likelihood and Bayesian analyses but, by contrast (and consistent with previous studies), most families composed predominantly of shallow-water zooxanthellate taxa were polyphyletic, although Acroporidae, Poritidae, Pocilloporidae, and Fungiidae were exceptions to this general pattern. One factor contributing to this inconsistency may be the greater environmental stability of deep-sea environments, effectively removing taxonomic "noise'' contributed by phenotypic plasticity. Our phylogenetic analyses imply that the most basal extant scleractinians are azooxanthellate solitary corals from deep-water, their divergence predating that of the robust and complex corals. Deep-sea corals are likely to be critical to understanding anthozoan evolution and the origins of the Scleractinia. C1 [Kitahara, Marcelo V.; Miller, David J.] James Cook Univ, ARC Ctr Excellence Coral Reefs Studies, Townsville, Qld 4811, Australia. [Kitahara, Marcelo V.; Miller, David J.] James Cook Univ, Coral Genom Grp, Townsville, Qld 4811, Australia. [Cairns, Stephen D.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. [Stolarski, Jaroslaw] Polish Acad Sci, Inst Paleobiol, Warsaw, Poland. [Blair, David] James Cook Univ, Sch Marine & Trop Biol, Townsville, Qld 4811, Australia. RP Kitahara, MV (reprint author), James Cook Univ, ARC Ctr Excellence Coral Reefs Studies, Townsville, Qld 4811, Australia. EM mvkitahara@yahoo.com.br RI Kitahara, Marcelo/D-5560-2011; Blair, David/G-6052-2011; Manager, MEEL/C-4732-2015 OI Blair, David/0000-0002-4658-3251; FU Australian Research Council (through the Centre of Excellence for Coral Reef Studies); Brazilian Coordination for the Improvement of Higher Education Personnel (CAPES); Fisheries Research and Development Corporation (FRDC); Australian Government Department of Environment, Water, Heritage and the Arts; Australian CSIRO (Commonwealth Scientific and Industrial Research Organization) Wealth [SS102005, SS022007] FX This study was supported through funding from the Australian Research Council (through the Centre of Excellence for Coral Reef Studies) grants to DJM. MVK is a recipient of a PhD scholarship from the Brazilian Coordination for the Improvement of Higher Education Personnel (CAPES). The Australian specimens examined in the present study were collected with funding from the Fisheries Research and Development Corporation (FRDC) and Environment Australia (now the Australian Government Department of Environment, Water, Heritage and the Arts); the 2005/2007 cruises (SS102005 and SS022007) were funded by the Australian CSIRO (Commonwealth Scientific and Industrial Research Organization) Wealth from Oceans Flagship with the assistance of the Australian Government Department of the Environment, Water, Heritage and the Arts; and the NORFANZ cruise was a collaboration between Australia's National Oceans Office (now the Australian Government Department of Environment, Water, Heritage and the Arts), Australia's CSIRO Marine and Atmospheric Research, New Zealand's Ministry of Fisheries and New Zealand's National Institute of Water and Atmospheric Sciences. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 69 TC 84 Z9 86 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 JUL 8 PY 2010 VL 5 IS 7 AR e11490 DI 10.1371/journal.pone.0011490 PG 9 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 622CS UT WOS:000279637100015 PM 20628613 ER PT J AU Tamisiea, ME Hill, EM Ponte, RM Davis, JL Velicogna, I Vinogradova, NT AF Tamisiea, M. E. Hill, E. M. Ponte, R. M. Davis, J. L. Velicogna, I. Vinogradova, N. T. TI Impact of self-attraction and loading on the annual cycle in sea level SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article ID SATELLITE ALTIMETRY; ICE SHEETS; MASS; WATER; EQUILIBRIUM; VARIABILITY; PRESSURE; DYNAMICS; MODELS; OCEAN AB The annual exchange of water between the continents and oceans is observed by GPS, gravimetry, and altimetry. However, the global average amplitude of this annual cycle (observed amplitude of similar to 8 mm) is not representative of the effects that would be observed at individual tide gauges or at ocean bottom pressure recorders because of self-attraction and loading effects (SAL). In this paper, we examine the spatial variation of sea level change caused by the three main components that load the Earth and contribute to the water cycle: hydrology (including snow), the atmosphere, and the dynamic ocean. The SAL effects cause annual amplitudes at tide gauges (modeled here with a global average of similar to 9 mm) to vary from less than 2 mm to more than 18 mm. We find a variance reduction (global average of 3 to 4%) after removing the modeled time series from a global set of tide gauges. We conclude that SAL effects are significant in places (e. g., the south central Pacific and coastal regions in Southeast Asia and west central Africa) and should be considered when interpreting these data sets and using them to constrain ocean circulation models. C1 [Tamisiea, M. E.] Natl Oceanog Ctr, Liverpool L3 5DA, Merseyside, England. [Hill, E. M.; Davis, J. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ponte, R. M.; Vinogradova, N. T.] Atmospher & Environm Res Inc, Lexington, MA 02421 USA. [Velicogna, I.] Univ Calif Irvine, Sch Phys Sci, Irvine, CA 92697 USA. RP Tamisiea, ME (reprint author), Natl Oceanog Ctr, Joseph Proudman Bldg,6 Brownlow St, Liverpool L3 5DA, Merseyside, England. EM mtam@pol.ac.uk RI Hill, Emma/B-7037-2011; Davis, James/D-8766-2013 OI Hill, Emma/0000-0003-0231-5818; Davis, James/0000-0003-3057-477X FU Natural Environment Research Council; NASA [NNX08AJ79G, NNX07AM77G] FX This study was funded by Natural Environment Research Council's Oceans 2025 program (MET), NASA grants NNX08AJ79G (EMH, JLD) and NNX07AM77G (EMH, RMP, JLD, NTV), NASA's Cryospheric Science Program, Solid Earth and Natural Hazards Program, Terrestrial Hydrology Program and the NSF Office of Polar Programs (IV). We would like to thank Chris Hughes for discussions and Erik Ivins and an anonymous reviewer for useful suggestions. The GLDAS/Noah data used in this study were acquired as part of the mission of NASA's Earth Science Division and archived and distributed by the Goddard Earth Sciences (GES) Data and Information Services Center (DISC). NCEP Reanalysis derived data were provided by the NOAA-ESRL PSD, Boulder, Colorado, USA, from their Web site at http://www.esrl.noaa.gov/psd/. NR 47 TC 28 Z9 29 U1 2 U2 9 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-OCEANS JI J. Geophys. Res.-Oceans PD JUL 7 PY 2010 VL 115 AR C07004 DI 10.1029/2009JC005687 PG 15 WC Oceanography SC Oceanography GA 624NG UT WOS:000279825200001 ER PT J AU Larjavaara, M AF Larjavaara, Markku TI Maintenance cost, toppling risk and size of trees in a self-thinning stand SO JOURNAL OF THEORETICAL BIOLOGY LA English DT Article DE Allometric; Allometry; Biomass; Self-thinning law; Wind drag ID PINE; CONSTRAINTS; DENSITY; STEM; HEIGHT; GROWTH; MODEL AB Wind routinely topples trees during storms, and the likelihood that a tree is toppled depends critically on its allometry. Yet none of the existing theories to explain tree allometry consider wind drag on tree canopies. Since leaf area index in crowded, self-thinning stands is independent of stand density, the drag force per unit land can also be assumed to be independent of stand density, with only canopy height influencing the total toppling moment. Tree stem dimensions and the self-thinning biomass can then be computed by further assuming that the risk of toppling over and stem maintenance per unit land area are independent of stand density, and that stem maintenance cost is a linear function of stem surface area and sapwood volume. These assumptions provide a novel way to understand tree allometry and lead to a self-thinning line relating tree biomass and stand density with a power between -3/2 and -2/3 depending on the ratio of maintenance of sapwood and stem surface. (C) 2010 Elsevier Ltd. All rights reserved. C1 [Larjavaara, Markku] Smithsonian Trop Res Inst, CTFS Global Forest Carbon Res Initiat, Panama City, Panama. [Larjavaara, Markku] Univ Helsinki, Dept Forest Sci, FIN-00014 Helsinki, Finland. RP Larjavaara, M (reprint author), Smithsonian Trop Res Inst, CTFS Global Forest Carbon Res Initiat, Apartado Postal 0843-03092, Panama City, Panama. EM larjavaaram@si.edu OI Larjavaara, Markku/0000-0002-3484-889X FU HSBC FX I want to thank David A. King, Helene C. Muller-Landau, Annikki Makela, Juho Pennanen and anonymous reviewers for valuable comments, my wife Katja Sidoroff for general support during the 32 months from writing the first draft to an accepted paper and HSBC Climate Partnership for funding. NR 28 TC 10 Z9 10 U1 0 U2 12 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0022-5193 J9 J THEOR BIOL JI J. Theor. Biol. PD JUL 7 PY 2010 VL 265 IS 1 BP 63 EP 67 DI 10.1016/j.jtbi.2010.04.021 PG 5 WC Biology; Mathematical & Computational Biology SC Life Sciences & Biomedicine - Other Topics; Mathematical & Computational Biology GA 612UF UT WOS:000278928600006 PM 20417645 ER PT J AU Ticknor, C Rittenhouse, ST AF Ticknor, Christopher Rittenhouse, Seth T. TI Three Body Recombination of Ultracold Dipoles to Weakly Bound Dimers SO PHYSICAL REVIEW LETTERS LA English DT Article ID POLAR-MOLECULES; FERMI GASES; ATOMS; UNIVERSALITY; SCATTERING; SYSTEM; STATES AB We use universality in two-body dipolar physics to study three-body recombination. We present results for the universal structure of weakly bound two-dipole states that depend only on the s-wave scattering length ( a). We study threshold three-body recombination rates into weakly bound dimer states as a function of the scattering length. A Fermi golden rule analysis is used to estimate rates for different events mediated by the dipole-dipole interaction and a phenomenological contact interaction. The three-body recombination rate in the limit where a >> D contains terms which scale as a(4), a(2)D(2), and D(4), where D is the dipolar length. When a << D, the three-body recombination rate scales as D(4). C1 [Ticknor, Christopher; Rittenhouse, Seth T.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Ticknor, Christopher] Swinburne Univ Technol, ARC Ctr Excellence Quantum Atom Opt, Hawthorn, Vic 3122, Australia. [Ticknor, Christopher] Swinburne Univ Technol, Ctr Atom Opt & Ultrafast Spect, Hawthorn, Vic 3122, Australia. [Ticknor, Christopher] Los Alamos Natl Lab, Div Theoret, Los Alamos, NM 87545 USA. RP Ticknor, C (reprint author), Harvard Smithsonian Ctr Astrophys, ITAMP, 60 Garden St, Cambridge, MA 02138 USA. RI Rittenhouse, Seth/E-7688-2011; Ticknor, Christopher/B-8651-2014; OI Ticknor, Christopher/0000-0001-9972-4524 FU NSF through ITAMP at Harvard University; Smithsonian Astrophysical Observatory; Australian Research Council; U.S. DOE [DE-AC52-06NA25396] FX The authors thank H.R. Sadeghpour for numerous helpful discussions. Both authors gratefully acknowledge support from the NSF through ITAMP at Harvard University and Smithsonian Astrophysical Observatory. C.T. gratefully acknowledges partial support from the Australian Research Council and LANL, which is operated by Los Alamos National Security, LLC for the NNSA of the U.S. DOE under Contract No. DE-AC52-06NA25396. NR 28 TC 18 Z9 18 U1 0 U2 3 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 J9 PHYS REV LETT JI Phys. Rev. Lett. PD JUL 2 PY 2010 VL 105 IS 1 AR 013201 DI 10.1103/PhysRevLett.105.013201 PG 4 WC Physics, Multidisciplinary SC Physics GA 620FL UT WOS:000279484300001 PM 20867441 ER PT J AU Launius, RD AF Launius, Roger D. TI An unintended consequence of the IGY: Eisenhower, Sputnik, the Founding of NASA SO ACTA ASTRONAUTICA LA English DT Article DE Soviet union; Satellite; United states; Cold war crisis; Department of defense; National defense education act; Presidential science advisor; International geophysical year; IGY; NASA; National aeronautics and space act AB On October 4,1957, the Soviet Union launched the first Earth-circling artificial satellite and the United States responded by taking numerous actions aimed at "remediating" a Cold War crisis. This included the establishment of a separate civilian space agency charged with the conduct of an official program of scientific and technological space exploration, consolidation of Department of Defense space activities, the passage of the National Defense Education Act, the creation of a Presidential Science Advisor, and a host of lesser actions. The politics of these changes is fascinating, and has been interpreted as an appropriate political response to a unique crisis situation. Interest groups, all for differing reasons, prodded national leaders to undertake large-scale efforts, something the president thought unnecessarily expensive and once set in place impossible to dismantle. But was the Sputnik crisis truly a crisis in any real sense? Was it made into one by interest groups who used it for their own ends? This paper will trace briefly some of the major themes associated with the IGY and Sputnik and describe the political construction of the crisis as it emerged in 1957-1958. It will also discuss something about the transformation of federal science and technology that took place in response to this "crisis" and how it set in train a series of processes and policies that did not unravel until the end of the Cold War. Published by Elsevier Ltd. C1 [Launius, Roger D.] Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20013 USA. RP Launius, RD (reprint author), Smithsonian Inst, Natl Air & Space Museum, POB 37012,NASM Room 3556,MRC 311, Washington, DC 20013 USA. EM launiusr@si.edu OI Launius, Roger/0000-0003-1633-1253 NR 75 TC 0 Z9 0 U1 0 U2 5 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 J9 ACTA ASTRONAUT JI Acta Astronaut. PD JUL-AUG PY 2010 VL 67 IS 1-2 BP 254 EP 263 DI 10.1016/j.actaastro.2009.10.019 PG 10 WC Engineering, Aerospace SC Engineering GA 596LG UT WOS:000277685800023 ER PT J AU Hamilton, AJ Basset, Y Benke, KK Grimbacher, PS Miller, SE Novotny, V Samuelson, GA Stork, NE Weiblen, GD Yen, JDL AF Hamilton, Andrew J. Basset, Yves Benke, Kurt K. Grimbacher, Peter S. Miller, Scott E. Novotny, Vojtech Samuelson, G. Allan Stork, Nigel E. Weiblen, George D. Yen, Jian D. L. TI Quantifying Uncertainty in Estimation of Tropical Arthropod Species Richness SO AMERICAN NATURALIST LA English DT Article DE Coleoptera; host specificity; Latin hypercube sampling; global richness estimate; stochastic model; tropical rain forest insects ID HERBIVOROUS INSECTS; DIVERSITY; BIODIVERSITY; FOREST; INTEGRATION; PHYLOGENY; BEETLES AB There is a bewildering range of estimates for the number of arthropods on Earth. Several measures are based on extrapolation from species specialized to tropical rain forest, each using specific assumptions and justifications. These approaches have not provided any sound measure of uncertainty associated with richness estimates. We present two models that account for parameter uncertainty by replacing point estimates with probability distributions. The models predict medians of 3.7 million and 2.5 million tropical arthropod species globally, with 90% confidence intervals of [2.0, 7.4] million and [1.1, 5.4] million, respectively. Estimates of 30 million or greater are predicted to have <0.00001 probability. Sensitivity analyses identified uncertainty in the proportion of canopy arthropod species that are beetles as the most influential parameter, although uncertainties associated with three other parameters were also important. Using the median estimates suggests that in spite of 250 years of taxonomy and around 855,000 species of arthropods already described, approximately 70% await description. C1 [Hamilton, Andrew J.; Grimbacher, Peter S.; Stork, Nigel E.; Yen, Jian D. L.] Univ Melbourne, Dept Resource Management & Geog, Richmond, Vic 3121, Australia. [Basset, Yves] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Benke, Kurt K.] Dept Primary Ind, Parkville Ctr, Vic 3052, Australia. [Miller, Scott E.] Smithsonian Inst, Natl Museum Nat Hist & Natl Zool Pk, Washington, DC 20013 USA. [Novotny, Vojtech] Univ S Bohemia, Fac Sci, Ceske Budejovice 37005, Czech Republic. [Novotny, Vojtech] Acad Sci Czech Republic, Ctr Biol, Ceske Budejovice 37005, Czech Republic. [Samuelson, G. Allan] Bernice P Bishop Museum, Honolulu, HI 96817 USA. [Weiblen, George D.] Univ Minnesota, Dept Plant Biol, St Paul, MN 55108 USA. RP Hamilton, AJ (reprint author), Univ Melbourne, Dept Resource Management & Geog, Burnley Campus,500 Yarra Blvd, Richmond, Vic 3121, Australia. EM andrewjh@unimelb.edu.au RI Basset, Yves/B-6642-2014; Novotny, Vojtech/G-9434-2014; OI Novotny, Vojtech/0000-0001-7918-8023; Yen, Jian/0000-0001-7964-923X; Benke, Kurt/0000-0002-7812-3671; Miller, Scott/0000-0002-4138-1378 FU National Science Foundation; Christensen Fund; Grant Agency of the Czech Republic; Czech Academy of Sciences; Swedish Natural Science Research Council; Czech Ministry of Education; Otto Kinne Foundation; Darwin Initiative; International Centre of Insect Physiology and Ecology; Bishop Museum FX We thank B. Brook, A. Chao, and R. Colwell for providing insightful comments on earlier versions of this manuscript and N. Karavarsamis for advice on confidence interval estimation. The host specificity studies in New Guinea were supported by the National Science Foundation, Christensen Fund, Grant Agency of the Czech Republic, Czech Academy of Sciences, Swedish Natural Science Research Council, Czech Ministry of Education, Otto Kinne Foundation, Darwin Initiative, International Centre of Insect Physiology and Ecology, and Bishop Museum. Para-taxonomists in New Guinea are thanked for their assistance and are listed in Novotny et al. (2002). NR 35 TC 96 Z9 103 U1 7 U2 57 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0003-0147 EI 1537-5323 J9 AM NAT JI Am. Nat. PD JUL PY 2010 VL 176 IS 1 BP 90 EP 95 DI 10.1086/652998 PG 6 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA 605VN UT WOS:000278375200012 PM 20455708 ER PT J AU Hunt, G AF Hunt, Gene TI Evolution in Fossil Lineages: Paleontology and The Origin of Species SO AMERICAN NATURALIST LA English DT Article DE fossil record; Charles Darwin; modes of evolution; stasis; gradualism; diversity dependence ID PHANEROZOIC TAXONOMIC DIVERSITY; MOLECULAR PHYLOGENIES; THREESPINE STICKLEBACK; STABILIZING SELECTION; KINETIC-MODEL; RANDOM-WALKS; MORPHOLOGICAL EVOLUTION; PUNCTUATED EQUILIBRIUM; CLADE DIVERSIFICATION; PHENOTYPIC EVOLUTION AB Of all of the sources of evidence for evolution by natural selection, perhaps the most problematic for Darwin was the geological record of organic change. In response to the absence of species-level transformations in the fossil record, Darwin argued that the fossil record was too incomplete, too biased, and too poorly known to provide strong evidence against his theory. Here, this view of the fossil record is evaluated in light of 150 years of subsequent paleontological research. Although Darwin's assessment of the completeness and resolution of fossiliferous rocks was in several ways astute, today the fossil record is much better explored, documented, and understood than it was in 1859. In particular, a reasonably large set of studies tracing evolutionary trajectories within species can now be brought to bear on Darwin's expectation of gradual change driven by natural selection. An unusually high-resolution sequence of stickleback-bearing strata records the transformation of this lineage via natural selection. This adaptive trajectory is qualitatively consistent with Darwin's prediction, but it occurred much more rapidly than he would have guessed: almost all of the directional change was completed within 1,000 generations. In most geological sequences, this change would be too rapid to resolve. The accumulated fossil record at more typical paleontological scales (10(4)-10(6) years) reveals evolutionary changes that are rarely directional and net rates of change that are perhaps surprisingly slow, two findings that are in agreement with the punctuated-equilibrium model. Finally, Darwin's view of the broader history of life is reviewed briefly, with a focus on competition-mediated extinction and recent paleontological and phylogenetic attempts to assess diversity dependence in evolutionary dynamics. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. RP Hunt, G (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. EM hunte@si.edu RI Hunt, Gene/B-3783-2010 OI Hunt, Gene/0000-0001-6430-5020 NR 144 TC 10 Z9 10 U1 5 U2 56 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0003-0147 EI 1537-5323 J9 AM NAT JI Am. Nat. PD JUL PY 2010 VL 176 SU 1 BP S61 EP S76 DI 10.1086/657057 PG 16 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA 674KG UT WOS:000283740200005 PM 21043781 ER PT J AU Voigt-Heucke, SL Taborsky, M Dechmann, DKN AF Voigt-Heucke, Silke L. Taborsky, Michael Dechmann, Dina K. N. TI A dual function of echolocation: bats use echolocation calls to identify familiar and unfamiliar individuals SO ANIMAL BEHAVIOUR LA English DT Article DE Chiroptera; communication; eavesdropping; lesser bulldog bat; Noctilio albiventris; recognition; social behaviour ID SACCOPTERYX-BILINEATA CHIROPTERA; BOTTLE-NOSED DOLPHINS; LESSER BULLDOG BAT; BIG BROWN BATS; FORAGING BEHAVIOR; EPTESICUS-FUSCUS; TADARIDA-BRASILIENSIS; MYOTIS-LUCIFUGUS; NOCTILIO-ALBIVENTRIS; CONTAIN INFORMATION AB Bats use echolocation for orientation during foraging and navigation. However, it has been suggested that echolocation calls may also have a communicative function, for instance between roost members. In principle, this seems possible because echolocation calls are species specific and known to differ between the sexes, and between colonies and individuals for some species. We performed playback experiments with lesser bulldog bats, Noctilio albiventris, to which we presented calls of familiar/unfamiliar conspecifics, cohabitant/noncohabitant heterospecifics and ultrasonic white noise as a control. Bats reacted with a complex repertoire of social behaviours and the intensity of their response differed significantly between stimulus categories. Stronger reactions were shown towards echolocation calls of unfamiliar conspecifics than towards heterospecifics and white noise. To our knowledge, this is the first time that bats have been found to react to echolocation calls with a suite of social behaviours. Our results also provide the first experimental evidence for acoustical differentiation by bats between familiar and unfamiliar conspecifics, and of heterospecifics. Analysis of echolocation calls confirmed significant individual differences between echolocation calls. In addition, we found a nonsignificant trend towards group signatures in echolocation calls of N. albiventris. We suggest that echolocation calls used during orientation may also communicate species identity, group affiliation and individual identity. Our study highlights the communicative potential of sonar signals that have previously been categorized as cues in animal social systems. (C) 2010 The Association for the Study of Animal Behaviour. Published by Elsevier Ltd. All rights reserved. C1 [Voigt-Heucke, Silke L.] Free Univ Berlin, Dept Anim Behav, D-14195 Berlin, Germany. [Voigt-Heucke, Silke L.; Dechmann, Dina K. N.] Leibniz Inst Zoo & Wildlife Res, Leibniz, Germany. [Voigt-Heucke, Silke L.] Univ Vienna, Dept Behav Biol, A-1010 Vienna, Austria. [Taborsky, Michael] Univ Bern, Dept Behav Ecol, CH-3032 Hinterkappelen, Switzerland. [Dechmann, Dina K. N.] Univ Konstanz, Dept Biol, D-78457 Constance, Germany. [Dechmann, Dina K. N.] Smithsonian Trop Res Inst, Balboa, Panama. RP Voigt-Heucke, SL (reprint author), Free Univ Berlin, Dept Anim Behav, Takustr 6, D-14195 Berlin, Germany. EM voigt.heucke@googlemail.com RI Taborsky, Michael/F-8420-2013 OI Taborsky, Michael/0000-0002-1357-4316 FU German National Research Counci [DFG Vo 890/11] FX We thank Antje Kretzschmar, Felix Fornoff and Stefanie Ohler for help during the field work. Christian Voigt and Kamran Safi kindly provided insights and comments during the course of the project. Bjorn Siemers and Kamran Safi lent us some of the playback equipment. We thank the Smithsonian Research Institute and authorities and people of Panama. This work was funded by a grant from the German National Research Council to Christian C. Voigt and D.K.N.D. (DFG Vo 890/11). NR 81 TC 35 Z9 38 U1 4 U2 73 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0003-3472 J9 ANIM BEHAV JI Anim. Behav. PD JUL PY 2010 VL 80 IS 1 BP 59 EP 67 DI 10.1016/j.anbehav.2010.03.025 PG 9 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA 615RH UT WOS:000279153100009 ER PT J AU Inami, H Armus, L Surace, JA Mazzarella, JM Evans, AS Sanders, DB Howell, JH Petric, A Vavilkin, T Iwasawa, K Haan, S Murphy, EJ Stierwalt, S Appleton, PN Barnes, JE Bothun, G Bridge, CR Chan, B Charmandaris, V Frayer, DT Kewley, LJ Kim, DC Lord, S Madore, BF Marshall, JA Matsuhara, H Melbourne, JE Rich, J Schulz, B Spoon, HWW Sturm, E U, V Veilleux, S Xu, K AF Inami, H. Armus, L. Surace, J. A. Mazzarella, J. M. Evans, A. S. Sanders, D. B. Howell, J. H. Petric, A. Vavilkin, T. Iwasawa, K. Haan, S. Murphy, E. J. Stierwalt, S. Appleton, P. N. Barnes, J. E. Bothun, G. Bridge, C. R. Chan, B. Charmandaris, V. Frayer, D. T. Kewley, L. J. Kim, D. C. Lord, S. Madore, B. F. Marshall, J. A. Matsuhara, H. Melbourne, J. E. Rich, J. Schulz, B. Spoon, H. W. W. Sturm, E. U, V. Veilleux, S. Xu, K. TI THE BURIED STARBURST IN THE INTERACTING GALAXY II Zw 096 AS REVEALED BY THE SPITZER SPACE TELESCOPE SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies: individual (II Zw 096); galaxies: interactions; galaxies: starburst; galaxies: star clusters: general; infrared: galaxies ID ULTRALUMINOUS INFRARED GALAXIES; STAR-FORMING GALAXIES; SPECTRAL ENERGY-DISTRIBUTION; MU-M SPECTROSCOPY; ANTENNAE GALAXIES; IRS SPECTROSCOPY; CLUSTERS; SAMPLE; EVOLUTION; EMISSION AB An analysis of data from the Spitzer Space Telescope, Hubble Space Telescope, Chandra X-ray Observatory, and AKARI Infrared Astronomy Satellite is presented for the z = 0.036 merging galaxy system II Zw 096 (CGCG 448-020). Because II Zw 096 has an infrared luminosity of log(L-IR/L-circle dot) = 11.94, it is classified as a Luminous Infrared Galaxy (LIRG), and was observed as part of the Great Observatories All-sky LIRG Survey (GOALS). The Spitzer data suggest that 80% of the total infrared luminosity comes from an extremely compact, red source not associated with the nuclei of the merging galaxies. The Spitzer mid-infrared spectra indicate no high-ionization lines from a buried active galactic nucleus in this source. The strong detection of the 3.3 mu m and 6.2 mu m polycyclic aromatic hydrocarbon emission features in the AKARI and Spitzer spectra also implies that the energy source of II Zw 096 is a starburst. Based on Spitzer infrared imaging and AKARI near-infrared spectroscopy, the star formation rate is estimated to be 120 M-circle dot yr(-1) and >45 M-circle dot yr(-1), respectively. Finally, the high-resolution B-, I-, and H-band images show many star clusters in the interacting system. The colors of these clusters suggest at least two populations-one with an age of 1-5 Myr and one with an age of 20-500 Myr, reddened by 0-2 mag of visual extinction. The masses of these clusters span a range between 10(6) and 10(8) M-circle dot. This starburst source is reminiscent of the extranuclear starburst seen in NGC 4038/9 (the Antennae Galaxies) and Arp 299 but approximately an order of magnitude more luminous than the Antennae. The source is remarkable in that the off-nuclear infrared luminosity dominates the entire system. C1 [Inami, H.; Armus, L.; Surace, J. A.; Howell, J. H.; Petric, A.; Haan, S.; Murphy, E. J.; Stierwalt, S.; Marshall, J. A.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Inami, H.; Matsuhara, H.] Japan Aerosp Explorat Agcy, ISAS, Tokyo, Japan. [Inami, H.] Grad Univ Adv Studies, Dept Space & Astronaut Sci, Sokendai, Japan. [Mazzarella, J. M.; Howell, J. H.; Chan, B.; Lord, S.; Madore, B. F.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Evans, A. S.; Kim, D. C.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Sanders, D. B.; Barnes, J. E.; Kewley, L. J.; Rich, J.; U, V.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Vavilkin, T.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA. [Iwasawa, K.] ICREA, Barcelona, Spain. [Iwasawa, K.] Univ Barcelona, Barcelona, Spain. [Appleton, P. N.; Frayer, D. T.; Schulz, B.; Xu, K.] CALTECH, NASA Herschel Sci Ctr, Pasadena, CA 91125 USA. [Bothun, G.] Univ Oregon, Dept Phys, Eugene, OR 97402 USA. [Charmandaris, V.] Univ Crete, Dept Phys, GR-71003 Iraklion, Greece. [Charmandaris, V.] IESL Fdn Res & Technol Hellas, GR-71110 Iraklion, Greece. [Charmandaris, V.] Observ Paris, Chercheur Associe, F-75014 Paris, France. [Madore, B. F.] Carnegie Inst Sci, The Observatories, Pasadena, CA 91101 USA. [Spoon, H. W. W.] Cornell Univ, Dept Astron, Ithaca, NY 14953 USA. [Sturm, E.] MPE, D-85741 Garching, Germany. [U, V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Veilleux, S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Inami, H (reprint author), CALTECH, Spitzer Sci Ctr, MS 220-6, Pasadena, CA 91125 USA. EM inami@ipac.caltech.edu RI Charmandaris, Vassilis/A-7196-2008; OI Charmandaris, Vassilis/0000-0002-2688-1956; Rich, Jeffrey/0000-0002-5807-5078; Mazzarella, Joseph/0000-0002-8204-8619; Appleton, Philip/0000-0002-7607-8766 FU NASA [1407]; Spitzer Visiting Graduate Student Fellowship; Japan Society for the Promotion of Science (JSPS) [21-969] FX We thank J. Goldader and S. Satyapal for many helpful suggestions. The authors also thank an anonymous referee for suggestions which improved the manuscript. The Spitzer Space Telescope is operated by the Jet Propulsion Laboratory, California Institute of Technology, under NASA contract 1407. This research has made use of the NASA/IPAC Extragalactic Database (NED) and the Infrared Science Archive (IRSA) which are operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. Hanae Inami thanks the Spitzer Visiting Graduate Student Fellowship (from 2008 September to 2009 February) and Grant-in-Aid for Japan Society for the Promotion of Science (JSPS) Fellows (21-969) for supporting this work. NR 53 TC 23 Z9 23 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 JUL PY 2010 VL 140 IS 1 BP 63 EP 74 DI 10.1088/0004-6256/140/1/63 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 609XK UT WOS:000278691700006 ER PT J AU Seward, FD Williams, RM Chu, YH Gruendl, RA Dickel, JR AF Seward, F. D. Williams, R. M. Chu, Y. -H. Gruendl, R. A. Dickel, J. R. TI A CHANDRA OBSERVATION OF SNR 0540-697 SO ASTRONOMICAL JOURNAL LA English DT Article DE dust, extinction; H II regions; ISM: supernova remnants; Magellanic Clouds; techniques: image processing; X-rays: individual (SNR 0540-697) ID LARGE-MAGELLANIC-CLOUD; SUPERNOVA-REMNANTS; CATALOG; GHZ AB This paper describes a Chandra observation of SNR 0540-697 within the H II complex N159 in the Large Magellanic Cloud (LMC). Scattering from the nearby bright source LMC X-1, which obscures the western edge of the remnant, has been removed. Larger than previously believed, the 2'.0 x 2'.8 remnant is defined by optical filaments and two lobes of X-ray emission. A band of intervening material absorbs X-rays from the central part of the remnant. The N Lobe of the remnant is relatively bright and well defined, while emission from the S Lobe is much weaker. There is structure within the N Lobe but no clear X-ray emission from an outer shell indicating a shock in the interstellar medium. The X-ray spectrum is thermal with emission lines from Fe, Mg, and Si. The observed temperature and luminosity of the hot gas are 0.6 keV and 6 x 10(35) erg s(-1), respectively. These are consistent with characteristics expected for older remnants. There is also diffuse thermal X-ray emission north of N159 extending into N160, evidence for a larger remnant or bubble. C1 [Seward, F. D.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Williams, R. M.] Columbus State Univ, Dept Chem & Geol, Columbus, GA 31901 USA. [Chu, Y. -H.; Gruendl, R. A.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Dickel, J. R.] Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA. RP Seward, FD (reprint author), Smithsonian Astrophys Observ, MS4,60 Garden St, Cambridge, MA 02138 USA. FU NASA/CXC [G03-4096]; NASA LTSA [NNG05GC97G] FX Observations and analysis were supported by NASA/CXC Grant G03-4096. The authors are also grateful to Sean Points and R. Chris Smith for sharing images from the MCELS project. R. M. W. acknowledges support from NASA LTSA grant NNG05GC97G. NR 16 TC 6 Z9 6 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD JUL PY 2010 VL 140 IS 1 BP 177 EP 183 DI 10.1088/0004-6256/140/1/177 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 609XK UT WOS:000278691700015 ER PT J AU Winston, E Megeath, ST Wolk, SJ Spitzbart, B Gutermuth, R Allen, LE Hernandez, J Covey, K Muzerolle, J Hora, JL Myers, PC Fazio, GG AF Winston, E. Megeath, S. T. Wolk, S. J. Spitzbart, B. Gutermuth, R. Allen, L. E. Hernandez, J. Covey, K. Muzerolle, J. Hora, J. L. Myers, P. C. Fazio, G. G. TI THE PROPERTIES OF X-RAY LUMINOUS YOUNG STELLAR OBJECTS IN THE NGC 1333 AND SERPENS EMBEDDED CLUSTERS SO ASTRONOMICAL JOURNAL LA English DT Article DE circumstellar matter; infrared: stars; stars: pre-main sequence; X-rays: stars ID T-TAURI STARS; MAIN-SEQUENCE STARS; LOW-MASS STARS; POINT-SOURCE IDENTIFICATION; ORION ULTRADEEP PROJECT; SOLAR-TYPE STARS; CLOUD CORE; MOLECULAR CLOUD; FORMING REGION; XMM-NEWTON AB We present new Chandra X-ray data of the NGC 1333 embedded cluster and combine these data with existing Chandra data, Spitzer photometry, and ground-based spectroscopy of both the NGC 1333 and Serpens cloud core clusters to perform a detailed study of the X-ray properties of two of the nearest embedded clusters to the Sun. We first present new, deeper observations of NGC 1333 with Chandra ACIS-I and combine these with existing Spitzer observations of the region. In NGC 1333, a total of 95 cluster members are detected in X-rays of which 54 were previously identified in the Spitzer data. Of the Spitzer-identified sources, we detected 23% of the Class I protostars, 53% of the flat-spectrum sources, 52% of the Class II, and 50% of the transition disk young stellar objects (YSOs). Forty-one Class III members of the cluster are identified, bringing the total identified YSO population to 178. The X-ray luminosity functions (XLFs) of the NGC 1333 and Serpens clusters are compared to each other and the Orion Nebula Cluster (ONC). Based on a comparison of the XLFs of the Serpens and NGC 1333 clusters to the previously published ONC, we obtain a new distance for the Serpens cluster of 360(-13)(+22) pc. Using our previously published spectral types, effective temperatures, and bolometric luminosities, we analyze the dependence of the X-ray emission on the measured stellar properties. The X-ray luminosity was found to depend on the calculated bolometric luminosity as in previous studies of other clusters. We examine the dependence of L(X) on stellar surface area and effective temperature, and find that LX depends primarily on the stellar surface area. In the NGC 1333 cluster, the Class III sources have a somewhat higher X-ray luminosity for a given surface area. We also find evidence in NGC 1333 for a jump in the X-ray luminosity between spectral types of M0 and K7, we speculate that this may result from the presence of radiative zones in the K-stars. The gas column density versus extinction in the NGC 1333 parental molecular cloud was examined using the hydrogen column density determined from the X-ray absorption to the embedded stars and the K-band extinction measured to those stars. In NGC 1333, we find N(H) = 0.89 +/- 0.13 x 10(22)A(K), this is lower than expected of the standard interstellar medium but similar to that found previously in the Serpens cloud core. C1 [Winston, E.] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England. [Winston, E.; Wolk, S. J.; Spitzbart, B.; Covey, K.; Hora, J. L.; Myers, P. C.; Fazio, G. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Megeath, S. T.] Univ Toledo, Dept Phys & Astron, Ritter Observ, Toledo, OH 43606 USA. [Gutermuth, R.] Smith Coll, Five Colleges Astron Dept, Northampton, MA 01027 USA. [Gutermuth, R.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Allen, L. E.] Natl Opt Astron Observ, Tucson, AZ USA. [Hernandez, J.] Ctr Invest Astron, Merida 5101A, Venezuela. [Hernandez, J.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Muzerolle, J.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Winston, E (reprint author), Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England. EM ewinston@astro.ex.ac.uk OI Wolk, Scott/0000-0002-0826-9261; Hora, Joseph/0000-0002-5599-4650; Covey, Kevin/0000-0001-6914-7797 FU NASA [1256790, 960541] FX This work is based on observations made with the Chandra Telescope, under NASA contract NAS8-03060. This work is based on observations made with the Spitzer Space Telescope (PID 6, PID 174), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under NASA contract 1407. Support for this work was provided by NASA through contract 1256790 issued by JPL/Caltech. Support for the IRAC instrument was provided by NASA through contract 960541 issued by JPL. This work is based on observations taken with the Hectospec instrument on the MMT, a joint venture of the Smithsonian Institute and the University of Arizona. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. This research has made use of the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 81 TC 46 Z9 46 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD JUL PY 2010 VL 140 IS 1 BP 266 EP 292 DI 10.1088/0004-6256/140/1/266 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 609XK UT WOS:000278691700026 ER PT J AU Eales, SA Raymond, G Roseboom, IG Altieri, B Amblard, A Arumugam, V Auld, R Aussel, H Babbedge, T Blain, A Bock, J Boselli, A Brisbin, D Buat, V Burgarella, D Castro-Rodriguez, N Cava, A Chanial, P Clements, DL Conley, A Conversi, L Cooray, A Dowell, CD Dwek, E Dye, S Elbaz, D Farrah, D Fox, M Franceschini, A Gear, W Glenn, J Solares, EAG Griffin, M Harwit, M Hatziminaoglou, E Huang, J Ibar, E Isaak, K Ivison, RJ Lagache, G Levenson, L Lonsdale, CJ Lu, N Madden, S Maffei, B Mainetti, G Marchetti, L Morrison, GE Mortier, AMJ Nguyen, HT O'Halloran, B Oliver, SJ Omont, A Owen, FN Page, MJ Pannella, M Panuzzo, P Papageorgiou, A Pearson, CP Perez-Fournon, I Pohlen, M Rawlings, JI Rigopoulou, D Rizzo, D Rowan-Robinson, M Portal, MS Schulz, B Scott, D Seymour, N Shupe, DL Smith, AJ Stevens, JA Strazzullo, V Symeonidis, M Trichas, M Tugwell, KE Vaccari, M Valtchanov, I Vigroux, L Wang, L Ward, R Wright, G Xu, CK Zemcov, M AF Eales, S. A. Raymond, G. Roseboom, I. G. Altieri, B. Amblard, A. Arumugam, V. Auld, R. Aussel, H. Babbedge, T. Blain, A. Bock, J. Boselli, A. Brisbin, D. Buat, V. Burgarella, D. Castro-Rodriguez, N. Cava, A. Chanial, P. Clements, D. L. Conley, A. Conversi, L. Cooray, A. Dowell, C. D. Dwek, E. Dye, S. Elbaz, D. Farrah, D. Fox, M. Franceschini, A. Gear, W. Glenn, J. Solares, E. A. Gonzalez Griffin, M. Harwit, M. Hatziminaoglou, E. Huang, J. Ibar, E. Isaak, K. Ivison, R. J. Lagache, G. Levenson, L. Lonsdale, C. J. Lu, N. Madden, S. Maffei, B. Mainetti, G. Marchetti, L. Morrison, G. E. Mortier, A. M. J. Nguyen, H. T. O'Halloran, B. Oliver, S. J. Omont, A. Owen, F. N. Page, M. J. Pannella, M. Panuzzo, P. Papageorgiou, A. Pearson, C. P. Perez-Fournon, I. Pohlen, M. Rawlings, J. I. Rigopoulou, D. Rizzo, D. Rowan-Robinson, M. Sanchez Portal, M. Schulz, B. Scott, D. Seymour, N. Shupe, D. L. Smith, A. J. Stevens, J. A. Strazzullo, V. Symeonidis, M. Trichas, M. Tugwell, K. E. Vaccari, M. Valtchanov, I. Vigroux, L. Wang, L. Ward, R. Wright, G. Xu, C. K. Zemcov, M. TI First results from HerMES on the evolution of the submillimetre luminosity function SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: evoluton; galaxies: formation; galaxies: high-redshift; submillimeter: galaxies ID STAR-FORMING GALAXIES; REDSHIFT SURVEY; BLAST; UNIVERSE; DENSITY; HISTORY; FIELD AB We have carried out two extremely deep surveys with SPIRE, one of the two cameras on Herschel, at 250 mu m, close to the peak of the far-infrared background. We have used the results to investigate the evolution of the rest-frame 250-mu m luminosity function out to z = 2. We find evidence for strong evolution out to z similar or equal to 1 but evidence for at most weak evolution beyond this redshift. Our results suggest that a significant part of the stars and metals in the universe today were formed at z <= 1.4 in spiral galaxies. C1 [Eales, S. A.; Raymond, G.; Auld, R.; Dye, S.; Gear, W.; Griffin, M.; Isaak, K.; Papageorgiou, A.; Pohlen, M.] Cardiff Univ, Cardiff Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Roseboom, I. G.; Farrah, D.; Oliver, S. J.; Smith, A. J.; Wang, L.; Ward, R.] Univ Sussex, Ctr Astron, Dept Phys & Astron, Brighton BN1 9QH, E Sussex, England. [Altieri, B.; Conversi, L.; Sanchez Portal, M.; Valtchanov, I.] European Space Astron Ctr, Herschel Sci Ctr, Madrid 28691, Spain. [Amblard, A.; Cooray, A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Arumugam, V.; Ivison, R. J.] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Aussel, H.; Elbaz, D.; Madden, S.; Panuzzo, P.] Univ Paris Diderot, CE Saclay, Lab AIM Paris Saclay, CEA DSM Irfu CNRS, F-91191 Gif Sur Yvette, France. [Babbedge, T.; Chanial, P.; Clements, D. L.; Fox, M.; Mortier, A. M. J.; O'Halloran, B.; Rizzo, D.; Rowan-Robinson, M.; Trichas, M.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England. [Lu, N.; Schulz, B.; Shupe, D. L.; Xu, C. K.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Bock, J.; Dowell, C. D.; Levenson, L.; Nguyen, H. T.; Zemcov, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Boselli, A.; Buat, V.; Burgarella, D.] Univ Aix Marseille, CNRS, OAMP, Lab Astrophys Marseille, F-13388 Marseille 13, France. [Brisbin, D.] Cornell Univ, Ithaca, NY 14853 USA. [Castro-Rodriguez, N.; Cava, A.; Perez-Fournon, I.] IAC, Tenerife 38200, Spain. [Castro-Rodriguez, N.; Cava, A.; Perez-Fournon, I.] Univ La Laguna, Dept Astrofis, Tenerife 38205, Spain. [Conley, A.; Glenn, J.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Dwek, E.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. [Franceschini, A.; Mainetti, G.; Marchetti, L.; Vaccari, M.] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy. [Solares, E. A. Gonzalez] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Hatziminaoglou, E.] ESO, D-85748 Garching, Germany. [Huang, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ibar, E.; Ivison, R. J.; Wright, G.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Lagache, G.] Univ Paris 11, IAS, F-91405 Orsay, France. [Lagache, G.] CNRS, UMR 8617, F-91405 Orsay, France. [Lonsdale, C. J.; Owen, F. N.; Pannella, M.; Strazzullo, V.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Stevens, J. A.] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Rigopoulou, D.] Univ Oxford, Oxford OX1 3RH, England. [Pearson, C. P.] Univ Lethbridge, Inst Space Imaging Sci, Lethbridge, AB T1K 3M4, Canada. [Pearson, C. P.; Rigopoulou, D.] Rutherford Appleton Lab, Space Sci & Technol Dept, Didcot OX11 0QX, Oxon, England. [Page, M. J.; Rawlings, J. I.; Seymour, N.; Symeonidis, M.; Tugwell, K. E.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Morrison, G. E.] Canada France Hawaii Telescope, Kamuela, HI 96743 USA. [Morrison, G. E.; Omont, A.; Vigroux, L.] Univ Paris 06, CNRS, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France. [Maffei, B.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Maffei, B.] Univ Manchester, Sch Phys & Astron, Manchester M13 9PL, Lancs, England. RP Eales, SA (reprint author), Cardiff Univ, Cardiff Sch Phys & Astron, Queens Bldg, Cardiff CF24 3AA, S Glam, Wales. EM Steve.Eales@astro.cf.ac.uk RI Dwek, Eli/C-3995-2012; amblard, alexandre/L-7694-2014; Ivison, R./G-4450-2011; Vaccari, Mattia/R-3431-2016; Cava, Antonio/C-5274-2017; OI amblard, alexandre/0000-0002-2212-5395; Ivison, R./0000-0001-5118-1313; Vaccari, Mattia/0000-0002-6748-0577; Cava, Antonio/0000-0002-4821-1275; Scott, Douglas/0000-0002-6878-9840; Marchetti, Lucia/0000-0003-3948-7621; Seymour, Nicholas/0000-0003-3506-5536; Dye, Simon/0000-0002-1318-8343; Altieri, Bruno/0000-0003-3936-0284 FU CSA (Canada); NAOC (China); CEA (France); CNES (France); CNRS (France); ASI (Italy); MCINN (Spain); Stockholm Observatory (Sweden); STFC (UK); NASA (USA) FX SPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK) and including Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); Stockholm Observatory (Sweden); STFC (UK); and NASA (USA). NR 28 TC 38 Z9 38 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL-AUG PY 2010 VL 518 AR L23 DI 10.1051/0004-6361/201014675 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 646GQ UT WOS:000281527200024 ER PT J AU Elia, D Schisano, E Molinari, S Robitaille, T Angles-Alcazar, D Bally, J Battersby, C Benedettini, M Billot, N Calzoletti, L Di Giorgio, AM Faustini, F Li, JZ Martin, P Morgan, L Motte, F Mottram, JC Natoli, P Olmi, L Paladini, R Piacentini, F Pestalozzi, M Pezzuto, S Polychroni, D Smith, MD Strafella, F Stringfellow, GS Testi, L Thompson, MA Traficante, A Veneziani, M AF Elia, D. Schisano, E. Molinari, S. Robitaille, T. Angles-Alcazar, D. Bally, J. Battersby, C. Benedettini, M. Billot, N. Calzoletti, L. Di Giorgio, A. M. Faustini, F. Li, J. Z. Martin, P. Morgan, L. Motte, F. Mottram, J. C. Natoli, P. Olmi, L. Paladini, R. Piacentini, F. Pestalozzi, M. Pezzuto, S. Polychroni, D. Smith, M. D. Strafella, F. Stringfellow, G. S. Testi, L. Thompson, M. A. Traficante, A. Veneziani, M. TI A Herschel study of YSO evolutionary stages and formation timelines in two fields of the Hi-GAL survey SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: formation; stars: pre-main sequence ID YOUNG STELLAR OBJECTS; SPECTRAL ENERGY-DISTRIBUTIONS; GALACTIC PLANE; SEDS AB We present a first study of the star-forming compact dust condensations revealed by Herschel in the two 2 degrees x2 degrees Galactic Plane fields centered at [l, b] = [30 degrees, 0 degrees] and [l, b] = [59 degrees, 0 degrees], respectively, and observed during the science demonstration phase for the Herschel Infrared GALactic plane survey (Hi-GAL) key-project. Compact source catalogs extracted for the two fields in the five Hi-GAL bands (70, 160, 250, 350 and 500 mu m) were merged based on simple criteria of positional association and spectral energy distribution (SED) consistency into a final catalog which contains only coherent SEDs with counterparts in at least three adjacent Herschel bands. These final source lists contain 528 entries for the l = 30 degrees field, and 444 entries for the l = 59 degrees field. The SED coverage has been augmented with ancillary data at 24 mu m and 1.1 mm. SED modeling for the subset of 318 and 101 sources (in the two fields, respectively) for which the distance is known was carried out using both a structured star/disk/envelope radiative transfer model and a simple isothermal grey-body. Global parameters like mass, luminosity, temperature and dust properties have been estimated. The L(bo)l/M(env) ratio spans four orders of magnitudes from values compatible with the pre-protostellar phase to embedded massive zero-age main sequence stars. Sources in the l = 59 degrees field have on average lower L/M, possibly outlining an overall earlier evolutionary stage with respect to the sources in the l = 30 degrees field. Many of these cores are actively forming high-mass stars, although the estimated core surface densities appear to be an order of magnitude below the 1 g cm(-2) critical threshold for high-mass star formation. C1 [Elia, D.; Schisano, E.; Molinari, S.; Benedettini, M.; Di Giorgio, A. M.; Pestalozzi, M.; Pezzuto, S.; Polychroni, D.] INAF, Ist Fis Spazio Interplanetario, I-00133 Rome, Italy. [Elia, D.] Observ Astron Lisboa, P-1349018 Lisbon, Portugal. [Schisano, E.] Univ Naples Federico 2, Dipartimento Sci Fisiche, Naples, Italy. [Robitaille, T.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Angles-Alcazar, D.] Univ Arizona, Dept Phys, Tucson, AZ 85721 USA. [Olmi, L.] Univ Puerto Rico, Dept Phys, UPR Stn, San Juan, PR 00936 USA. [Bally, J.; Battersby, C.; Stringfellow, G. S.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Billot, N.] CALTECH, NASA, Herschel Sci Ctr, IPAC, Pasadena, CA 91125 USA. [Calzoletti, L.; Faustini, F.] ASI Sci Data Ctr, I-00044 Frascati, Italy. [Li, J. Z.] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. [Martin, P.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Martin, P.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Morgan, L.] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England. [Motte, F.] Univ Paris Diderot, Lab AIM, CEA IRFU, CNRS,Serv Astrophys, F-91191 Gif Sur Yvette, France. [Mottram, J. C.] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England. [Olmi, L.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Paladini, R.] CALTECH, Spitzer Sci Ctr, IPAC, Pasadena, CA 91125 USA. [Smith, M. D.] Univ Kent, Ctr Astrophys & Planetary Sci, Canterbury CT2 7NH, Kent, England. [Strafella, F.] Univ Salento, Dipartimento Fis, I-73100 Lecce, Italy. [Testi, L.] ESO, D-85748 Garching, Germany. [Thompson, M. A.] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Natoli, P.; Traficante, A.] Univ Roma Tor Vergata, Dipartimento Fis, I-00173 Rome, Italy. [Piacentini, F.; Veneziani, M.] Univ Roma 1 La Sapienza, Dipartimento Fis, Rome, Italy. RP Elia, D (reprint author), INAF, Ist Fis Spazio Interplanetario, Via Fosso del Cavaliere, I-00133 Rome, Italy. EM davide.elia@ifsi-roma.inaf.it RI Molinari, Sergio/O-4095-2016; Piacentini, Francesco/E-7234-2010; OI Molinari, Sergio/0000-0002-9826-7525; Piacentini, Francesco/0000-0002-5444-9327; Pezzuto, Stefano/0000-0001-7852-1971; Olmi, Luca/0000-0002-1162-7947; Elia, Davide/0000-0002-9120-5890; Robitaille, Thomas/0000-0002-8642-1329 FU ASI [I/038/080/0] FX Data processing and maps production has been possible thanks to ASI generous support via contract I/038/080/0. NR 19 TC 40 Z9 40 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 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL-AUG PY 2010 VL 518 AR L97 DI 10.1051/0004-6361/201014651 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 646GQ UT WOS:000281527200098 ER PT J AU Fich, M Johnstone, D van Kempen, TA McCoey, C Fuente, A Caselli, P Kristensen, LE Plume, R Cernicharo, J Herczeg, GJ van Dishoeck, EF Wampfler, S Gaufre, P Gill, JJ Javadi, H Justen, M Laauwen, W Luinge, W Ossenkopf, V Pearson, J Bachiller, R Baudry, A Benedettini, M Bergin, E Benz, AO Bjerkeli, P Blake, G Bontemps, S Braine, J Bruderer, S Codella, C Daniel, F di Giorgio, AM Dominik, C Doty, SD Encrenaz, P Giannini, T Goicoechea, JR de Graauw, T Helmich, F Herpin, F Hogerheijde, MR Jacq, T Jorgensen, JK Larsson, B Lis, D Liseau, R Marseille, M Melnick, G Nisini, B Olberg, M Parise, B Risacher, C Santiago, J Saraceno, P Shipman, R Tafalla, M van der Tak, F Visser, R Wyrowski, F Yildiz, UA AF Fich, M. Johnstone, D. van Kempen, T. A. McCoey, C. Fuente, A. Caselli, P. Kristensen, L. E. Plume, R. Cernicharo, J. Herczeg, G. J. van Dishoeck, E. F. Wampfler, S. Gaufre, P. Gill, J. J. Javadi, H. Justen, M. Laauwen, W. Luinge, W. Ossenkopf, V. Pearson, J. Bachiller, R. Baudry, A. Benedettini, M. Bergin, E. Benz, A. O. Bjerkeli, P. Blake, G. Bontemps, S. Braine, J. Bruderer, S. Codella, C. Daniel, F. di Giorgio, A. M. Dominik, C. Doty, S. D. Encrenaz, P. Giannini, T. Goicoechea, J. R. de Graauw, Th. Helmich, F. Herpin, F. Hogerheijde, M. R. Jacq, T. Jorgensen, J. K. Larsson, B. Lis, D. Liseau, R. Marseille, M. Melnick, G. Nisini, B. Olberg, M. Parise, B. Risacher, C. Santiago, J. Saraceno, P. Shipman, R. Tafalla, M. van der Tak, F. Visser, R. Wyrowski, F. Yildiz, U. A. TI Herschel-PACS spectroscopy of the intermediate mass protostar NGC 7129 FIRS 2 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: formation; ISM: molecules ID YOUNG STELLAR OBJECTS; STAR-FORMATION; HH 46; EVOLUTION; OUTFLOW; REGIONS; GAS; I. AB Aims. We present preliminary results of the first Herschel spectroscopic observations of NGC 7129 FIRS2, an intermediate mass star-forming region. We attempt to interpret the observations in the framework of an in-falling spherical envelope. Methods. The PACS instrument was used in line spectroscopy mode ( R = 1000-5000) with 15 spectral bands between 63 and 185 mu m. This provided good detections of 26 spectral lines seen in emission, including lines of H2O, CO, OH, O I, and C II. Results. Most of the detected lines, particularly those of H2O and CO, are substantially stronger than predicted by the spherical envelope models, typically by several orders of magnitude. In this paper we focus on what can be learned from the detected CO emission lines. Conclusions. It is unlikely that the much stronger than expected line emission arises in the (spherical) envelope of the YSO. The region hot enough to produce such high excitation lines within such an envelope is too small to produce the amount of emission observed. Virtually all of this high excitation emission must arise in structures such as as along the walls of the outflow cavity with the emission produced by a combination of UV photon heating and/or non-dissociative shocks. C1 [Fich, M.; McCoey, C.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G, Canada. [Johnstone, D.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Johnstone, D.; Kristensen, L. E.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 1A1, Canada. [van Kempen, T. A.; van Dishoeck, E. F.; Hogerheijde, M. R.; Melnick, G.; Visser, R.; Yildiz, U. A.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [van Kempen, T. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [McCoey, C.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [Fuente, A.; Bachiller, R.; Santiago, J.; Tafalla, M.] IGN Observ Astron Nacl, Alcala De Henares 28800, Spain. [Caselli, P.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Plume, R.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Cernicharo, J.; Goicoechea, J. R.] INTA CSIC, Dept Astrophys, CAB, Torrejon De Ardoz 28850, Spain. [Herczeg, G. J.; van Dishoeck, E. F.] Max Planck Inst Extraterr Phys, D-37075 Garching, Germany. [Wampfler, S.; Benz, A. O.; Bruderer, S.] ETH, Inst Astron, CH-8093 Zurich, Switzerland. [Gaufre, P.; Baudry, A.; Bontemps, S.; Braine, J.; Herpin, F.; Jacq, T.] Univ Bordeaux, Lab Astrophys Bordeaux, CNRS INSU, UMR 5804, Floirac, France. [Gill, J. J.; Javadi, H.; Pearson, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Justen, M.; Ossenkopf, V.] Univ Cologne, KOSMA, Inst Phys 1, D-50937 Cologne, Germany. [Laauwen, W.; Luinge, W.; de Graauw, Th.; Helmich, F.; Marseille, M.; Risacher, C.; Shipman, R.; van der Tak, F.] SRON Netherlands Inst Space Res, NL-9747 AD Groningen, Netherlands. [Bjerkeli, P.; Liseau, R.; Olberg, M.] Chalmers, Dept Radio & Space Sci, Onsala Space Observ, S-43992 Onsala, Sweden. [van der Tak, F.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Benedettini, M.; Codella, C.; di Giorgio, A. M.; Giannini, T.; Nisini, B.; Saraceno, P.] INAF, Ist Fis Spazio Interplanetario, Area Ric Tor Vergata, I-00133 Rome, Italy. [Benedettini, M.; Bergin, E.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Blake, G.; Lis, D.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Daniel, F.] CNRS, Observ Paris Meudon, LERMA, UMR 8112, F-92195 Meudon, France. [Daniel, F.] CSIC, Dept Mol & Infrared Astrophys, Madrid 28006, Spain. [Dominik, C.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. [Doty, S. D.] Denison Univ, Dept Phys & Astron, Granville, OH 43023 USA. [Encrenaz, P.] Observ Paris, LERMA, F-75014 Paris, France. [Encrenaz, P.] Observ Paris, CNRS, UMR 8112, F-75014 Paris, France. [Jorgensen, J. K.] Univ Copenhagen, Ctr Star & Planet Format, Nat Hist Museum Denmark, DK-1350 Copenhagen, Denmark. [Larsson, B.] Stockholm Univ, Dept Astron, S-10691 Stockholm, Sweden. [Parise, B.; Wyrowski, F.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Parise, B.] Univ Cologne, Inst Phys, D-50937 Cologne, Germany. [Caselli, P.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. RP Fich, M (reprint author), Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G, Canada. EM fich@uwaterloo.ca RI Yildiz, Umut/C-5257-2011; Kristensen, Lars/F-4774-2011; Visser, Ruud/J-8574-2012; Wampfler, Susanne/D-2270-2015; Fuente, Asuncion/G-1468-2016; OI Codella, Claudio/0000-0003-1514-3074; Yildiz, Umut/0000-0001-6197-2864; Kristensen, Lars/0000-0003-1159-3721; Giannini, Teresa/0000-0002-0224-096X; Wampfler, Susanne/0000-0002-3151-7657; Fuente, Asuncion/0000-0001-6317-6343; Bjerkeli, Per/0000-0002-7993-4118; , Brunella Nisini/0000-0002-9190-0113 FU Spanish MCINN [CSD2009-00038]; National Aeronautics and Space Administration; [AYA2006-14786]; [AYA2009-07304] FX We thank Bruno Merin, Jeroen Bouwman, and Bart VandenBussche of the PACS ICC for all of their help with the data reduction. J.C. and A. F. thank theo Spanish MCINN for funding support under program CONSOLIDER INGENIO 2010 ref: CSD2009-00038, and J.C., under programs AYA2006-14786 and AYA2009-07304. 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. This program is made possible thanks to the HIFI guaranteed time program and the PACS instrument builders. HIFI has been designed and built by a consortium of institutes and university departments from across Europe, Canada and the United States under the leadership of SRON Netherlands Institute for Space Research Groningen, The Netherlands and with major contributions from Germany, France, and the US. Consortium members are: Canada: CSA, U. Waterloo; France: CESR, LAB, LERMA, IRAM; Germany: KOSMA, MPIfR, MPS; Ireland: NUI Maynooth; Italy: ASI, IFSI-INAF, Osservatorio Astrofisico di Arcetri-INAF; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astronomico Nacional (IGN), Centro de Astrobiologia (CSIC-INT); Sweden: Chalmers University of Technology - MC2, RSS & GARD, Onsala Space Observatory, Swedish National Space Board, Stockholm University - Stockholm Obseratory; Switzerland: ETH Zurich, FHNW; USA: Caltech, JPL, NHSC. NR 23 TC 19 Z9 19 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 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL-AUG PY 2010 VL 518 AR L86 DI 10.1051/0004-6361/201014672 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 646GQ UT WOS:000281527200087 ER PT J AU Fischer, WJ Megeath, ST Ali, B Tobin, JJ Osorio, M Allen, LE Kryukova, E Stanke, T Stutz, AM Bergin, E Calvet, N Di Francesco, J Furlan, E Hartmann, L Henning, T Krause, O Manoj, P Maret, S Muzerolle, J Myers, P Neufeld, D Pontoppidan, K Poteet, CA Watson, DM Wilson, T AF Fischer, W. J. Megeath, S. T. Ali, B. Tobin, J. J. Osorio, M. Allen, L. E. Kryukova, E. Stanke, T. Stutz, A. M. Bergin, E. Calvet, N. Di Francesco, J. Furlan, E. Hartmann, L. Henning, T. Krause, O. Manoj, P. Maret, S. Muzerolle, J. Myers, P. Neufeld, D. Pontoppidan, K. Poteet, C. A. Watson, D. M. Wilson, T. TI Herschel-PACS imaging of protostars in the HH 1-2 outflow complex SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: formation; stars: protostars; circumstellar matter; infrared: ISM; infrared: stars ID HERBIG-HARO OBJECT-1; INTERMEDIATE-MASS STARS; PROPER MOTIONS; DISTRIBUTIONS; EXTINCTION; CLOUD AB We present 70 and 160 mu m Herschel science demonstration images of a field in the Orion A molecular cloud that contains the prototypical Herbig-Haro objects HH 1 and 2, obtained with the Photodetector Array Camera and Spectrometer (PACS). These observations demonstrate Herschel's unprecedented ability to study the rich population of protostars in the Orion molecular clouds at the wavelengths where they emit most of their luminosity. The four protostars previously identified by Spitzer 3.6-40 mu m imaging and spectroscopy are detected in the 70 mu m band, and three are clearly detected at 160 mu m. We measure photometry of the protostars in the PACS bands and assemble their spectral energy distributions (SEDs) from 1 to 870 mu m with these data, Spitzer spectra and photometry, 2MASS data, and APEX sub-mm data. The SEDs are fit to models generated with radiative transfer codes. From these fits we can constrain the fundamental properties of the protostars. We find luminosities in the range 12-84 L(circle dot) and envelope densities spanning over two orders of magnitude. This implies that the four protostars have a wide range of envelope infall rates and evolutionary states: two have dense, infalling envelopes, while the other two have only residual envelopes. We also show the highly irregular and filamentary structure of the cold dust and gas surrounding the protostars as traced at 160 mu m. C1 [Fischer, W. J.; Megeath, S. T.; Kryukova, E.; Poteet, C. A.] Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA. [Ali, B.] CALTECH, IPAC, NHSC, Pasadena, CA 91125 USA. [Tobin, J. J.; Bergin, E.; Calvet, N.; Hartmann, L.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Osorio, M.] CSIC, Inst Astrofis Andalucia, Granada 18008, Spain. [Allen, L. E.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Stanke, T.; Wilson, T.] ESO, D-85748 Garching, Germany. [Stutz, A. M.; Henning, T.; Krause, O.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Stutz, A. M.] Univ Arizona, Dept Astron & Steward Observ, Tucson, AZ 85721 USA. [Di Francesco, J.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8W 3P6, Canada. [Di Francesco, J.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Furlan, E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Manoj, P.; Watson, D. M.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. [Maret, S.] Univ Grenoble 1, CNRS, UMR 571, Lab Astrophys Grenoble, F-38041 Grenoble, France. [Muzerolle, J.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Myers, P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Neufeld, D.] Johns Hopkins Univ, Baltimore, MD 21218 USA. [Pontoppidan, K.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. RP Fischer, WJ (reprint author), Univ Toledo, Dept Phys & Astron, 2801 W Bancroft St, Toledo, OH 43606 USA. EM wfische@utnet.utoledo.edu OI Fischer, William J/0000-0002-3747-2496; Stutz, Amelia/0000-0003-2300-8200; Furlan, Elise/0000-0001-9800-6248; Maret, Sebastien/0000-0003-1104-4554 FU NASA FX This work is based on observations made with the Herschel Space Observatory, a European Space Agency Cornerstone Mission with significant participation by NASA, and with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Support for the Herschel and Spitzer analysis was provided by NASA through awards issued by JPL/Caltech. We are grateful to Barbara Whitney and her collaborators for making their radiative transfer code available to the community. NR 20 TC 24 Z9 24 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 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL-AUG PY 2010 VL 518 AR L122 DI 10.1051/0004-6361/201014636 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 646GQ UT WOS:000281527200123 ER PT J AU Gonzalez-Alfonso, E Fischer, J Isaak, K Rykala, A Savini, G Spaans, M van der Werf, P Meijerink, R Israel, FP Loenen, AF Vlahakis, C Smith, HA Charmandaris, V Aalto, S Henkel, C Weiss, A Walter, F Greve, TR Martin-Pintado, J Naylor, DA Spinoglio, L Veilleux, S Harris, AI Armus, L Lord, S Mazzarella, J Xilouris, EM Sanders, DB Dasyra, KM Wiedner, MC Kramer, C Papadopoulos, PP Stacey, GJ Evans, AS Gao, Y AF Gonzalez-Alfonso, E. Fischer, J. Isaak, K. Rykala, A. Savini, G. Spaans, M. van der Werf, P. Meijerink, R. Israel, F. P. Loenen, A. F. Vlahakis, C. Smith, H. A. Charmandaris, V. Aalto, S. Henkel, C. Weiss, A. Walter, F. Greve, T. R. Martin-Pintado, J. Naylor, D. A. Spinoglio, L. Veilleux, S. Harris, A. I. Armus, L. Lord, S. Mazzarella, J. Xilouris, E. M. Sanders, D. B. Dasyra, K. M. Wiedner, M. C. Kramer, C. Papadopoulos, P. P. Stacey, G. J. Evans, A. S. Gao, Y. TI Herschel observations of water vapour in Markarian 231 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: molecules; galaxies: ISM; galaxies: individual: Mrk 231; line: formation; infrared: ISM; submillimeter: galaxies ID ULTRALUMINOUS INFRARED GALAXIES; EXCITATION; NUCLEI; H2O AB The Ultra luminous infrared galaxy (ULIRG) Mrk 231 reveals up to seven rotational lines of water (H(2)O) in emission, including a very high-lying (Eupper = 640 K) line detected at a 4 sigma level, within the Herschel/SPIRE wavelength range (190 < lambda(mu m) < 640), whereas PACS observations show one H(2)O line at 78 mu m in absorption, as found for other H(2)O lines previously detected by ISO. The absorption/emission dichotomy is caused by the pumping of the rotational levels by far-infrared radiation emitted by dust, and subsequent relaxation through lines at longer wavelengths, which allows us to estimate both the column density of H(2)O and the general characteristics of the underlying far-infrared continuum source. Radiative transfer models including excitation through both absorption of far-infrared radiation emitted by dust and collisions are used to calculate the equilibrium level populations of H(2)O and the corresponding line fluxes. The highest-lying H(2)O lines detected in emission, with levels at 300-640 K above the ground state, indicate that the source of far-infrared radiation responsible for the pumping is compact (radius = 110-180 pc) and warm (T(dust) = 85-95 K), accounting for at least 45% of the bolometric luminosity. The high column density, N(H(2)O) similar to 5 x 10(17) cm(-2), found in this nuclear component, is most probably the consequence of shocks/cosmic rays, an XDR chemistry, and/or an "undepleted chemistry" where grain mantles are evaporated. A more extended region, presumably the inner region of the 1-kpc disk observed in other molecular species, could contribute to the flux observed in low-lying H(2)O lines through dense hot cores, and/or shocks. The H(2)O 78 mu m line observed with PACS shows hints of a blue-shifted wing seen in absorption, possibly indicating the occurrence of H(2)O in the prominent outflow detected in OH (Fischer et al. 2010, A&A, 518, L41). Additional PACS/HIFI observations of H(2)O lines are required to constrain the kinematics of the nuclear component, as well as the distribution of H(2)O relative to the warm dust. C1 [Gonzalez-Alfonso, E.] Univ Alcala de Henares, Dept Fis, Madrid 28871, Spain. [Fischer, J.] USN, Res Lab, Remote Sensing Div, Washington, DC 20375 USA. [Isaak, K.; Rykala, A.] ESTEC SRE SA, Res & Sci Support Dept, ESA Astrophys Missions Div, NL-2201 AZ Noordwijk, Netherlands. [Savini, G.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Spaans, M.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [van der Werf, P.; Meijerink, R.; Israel, F. P.; Loenen, A. F.; Vlahakis, C.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Smith, H. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Charmandaris, V.] Univ Crete, Dept Phys, Iraklion 71003, Greece. [Aalto, S.] Chalmers, Onsala Space Observ, S-43992 Onsala, Sweden. [Henkel, C.; Weiss, A.] MPIfR, D-53121 Bonn, Germany. [Walter, F.; Greve, T. R.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Greve, T. R.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. [Martin-Pintado, J.] Ctr Astrobiol CSIC INTA, Madrid 28850, Spain. [Naylor, D. A.] Univ Lethbridge, Dept Phys & Astron, Inst Space Imaging Sci, Space Astron Div, Lethbridge, AB T1K 3M4, Canada. [Spinoglio, L.] CNR, Ist Fis Spazio Interplanetario, I-00133 Rome, Italy. [Veilleux, S.; Harris, A. I.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Armus, L.; Lord, S.; Mazzarella, J.] CALTECH, IPAC, Pasadena, CA 91125 USA. [Xilouris, E. M.] Natl Observ Athens, Inst Astron & Astrophys, GR-15236 Athens, Greece. [Sanders, D. B.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Dasyra, K. M.] Univ Paris Diderot, CEA Saclay, CNRS, Lab AIM,CEA DSM,Irfu Serv Astrophys, F-91191 Gif Sur Yvette, France. [Charmandaris, V.; Wiedner, M. C.] UCP, UPMC, ENS, OP,CNRS,UMR 8112,LERMA, F-75014 Paris, France. [Kramer, C.] IRAM, E-18012 Granada, Spain. [Papadopoulos, P. P.] Argelander Inst Fuer Astron, D-53121 Bonn, Germany. [Stacey, G. J.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Evans, A. S.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Gao, Y.] Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Peoples R China. RP Gonzalez-Alfonso, E (reprint author), Univ Alcala de Henares, Dept Fis, Madrid 28871, Spain. EM eduardo.gonzalez@uah.es RI Charmandaris, Vassilis/A-7196-2008; Xilouris, Emmanuel/K-9459-2013; Martin-Pintado, Jesus/H-6107-2015; OI Charmandaris, Vassilis/0000-0002-2688-1956; Martin-Pintado, Jesus/0000-0003-4561-3508; Meijerink, Rowin/0000-0001-7584-9293; Dasyra, Kalliopi/0000-0002-1482-2203; Mazzarella, Joseph/0000-0002-8204-8619; Spinoglio, Luigi/0000-0001-8840-1551; Savini, Giorgio/0000-0003-4449-9416 FU DNRF FX We thank the SHINING consortium for proving us with the spectrum of the H2O 423 -> 312, E. Habart for providing us the SPIRE spectrum of the Orion Bar prior to its publication in this volume, and the SPIRE ICC FTS team for their great help in data reduction/analysis. E. G-A is a Research Associate at the Harvard-Smithsonian Center for Astrophysics. Dark Cosmology Centre is funded by DNRF. NR 22 TC 40 Z9 40 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL-AUG PY 2010 VL 518 AR L43 DI 10.1051/0004-6361/201014664 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 646GQ UT WOS:000281527200044 ER PT J AU Mathews, GS Dent, WRF Williams, JP Howard, CD Meeus, G Riaz, B Roberge, A Sandell, G Vandenbussche, B Duchene, G Kamp, I Menard, F Montesinos, B Pinte, C Thi, WF Woitke, P Alacid, JM Andrews, SM Ardila, DR Aresu, G Augereau, JC Barrado, D Brittain, S Ciardi, DR Danchi, W Eiroa, C Fedele, D Grady, CA de Gregorio-Monsalvo, I Heras, A Huelamo, N Krivov, A Lebreton, J Liseau, R Martin-Zaidi, C Mendigutia, I Mora, A Morales-Calderon, M Nomura, H Pantin, E Pascucci, I Phillips, N Podio, L Poelman, DR Ramsay, S Rice, K Riviere-Marichalar, P Solano, E Tilling, I Walker, H White, GJ Wright, G AF Mathews, G. S. Dent, W. R. F. Williams, J. P. Howard, C. D. Meeus, G. Riaz, B. Roberge, A. Sandell, G. Vandenbussche, B. Duchene, G. Kamp, I. Menard, F. Montesinos, B. Pinte, C. Thi, W. F. Woitke, P. Alacid, J. M. Andrews, S. M. Ardila, D. R. Aresu, G. Augereau, J. C. Barrado, D. Brittain, S. Ciardi, D. R. Danchi, W. Eiroa, C. Fedele, D. Grady, C. A. de Gregorio-Monsalvo, I. Heras, A. Huelamo, N. Krivov, A. Lebreton, J. Liseau, R. Martin-Zaidi, C. Mendigutia, I. Mora, A. Morales-Calderon, M. Nomura, H. Pantin, E. Pascucci, I. Phillips, N. Podio, L. Poelman, D. R. Ramsay, S. Rice, K. Riviere-Marichalar, P. Solano, E. Tilling, I. Walker, H. White, G. J. Wright, G. TI GAS in Protoplanetary Systems (GASPS) I. First results SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: pre-main sequence; protoplanetary disks; infrared: stars ID ETA-CHAMAELEONTIS CLUSTER; FINE-STRUCTURE LINES; HERBIG-AE; TW-HYDRAE; YOUNG STARS; MASS-LOSS; ISO-LWS; MU-M; DISK; EMISSION AB Context. Circumstellar discs are ubiquitous around young stars, but rapidly dissipate their gas and dust on timescales of a few Myr. The Herschel Space Observatory allows for the study of the warm disc atmosphere, using far-infrared spectroscopy to measure gas content and excitation conditions, and far-IR photometry to constrain the dust distribution. Aims. We aim to detect and characterize the gas content of circumstellar discs in four targets as part of the Herschel science demonstration phase. Methods. We carried out sensitive medium resolution spectroscopy and high sensitivity photometry at gimel similar to 60-190 mu m using the Photodetector Array Camera and Spectrometer instrument on the Herschel Space Observatory. Results. We detect [OI] 63 mu m emission from the young stars HD 169142, TW Hydrae, and RECX 15, but not HD 181327. No other lines, including [CII] 158 and [OI] 145, are significantly detected. All four stars are detected in photometry at 70 and 160 mu m. Extensive models are presented in associated papers. C1 [Mathews, G. S.; Williams, J. P.] Univ Hawaii, Inst Astron IfA, Honolulu, HI 96822 USA. [Dent, W. R. F.; de Gregorio-Monsalvo, I.] ALMA, Santiago, Chile. [Dent, W. R. F.; de Gregorio-Monsalvo, I.] European So Observ, Santiago 19, Chile. [Howard, C. D.; Sandell, G.] NASA, Ames Res Ctr, SOFIA USRA, Moffett Field, CA 94035 USA. [Riaz, B.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Roberge, A.; Grady, C. A.] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA. [Vandenbussche, B.; Lebreton, J.; Martin-Zaidi, C.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium. [Duchene, G.; Menard, F.; Pinte, C.; Thi, W. F.; Augereau, J. C.] Univ Grenoble 1, CNRS, Lab Astrophys Grenoble LAOG, UMR 5571, F-38041 Grenoble 09, France. [Duchene, G.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Kamp, I.; Aresu, G.; Huelamo, N.; Podio, L.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Montesinos, B.; Barrado, D.; Mendigutia, I.; Riviere-Marichalar, P.] CSIC, INTA, Ctr Astrobiol, Dept Astrofis,LAEX, Villanueva De La Canada 28691, Spain. [Pinte, C.] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England. [Thi, W. F.; Woitke, P.; Rice, K.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Woitke, P.; Phillips, N.; Tilling, I.; Wright, G.] Univ Edinburgh, Royal Observ, UK Inst Astron, Royal Observ Edinburgh,Inst Astron,SUPA, Edinburgh EH9 3HJ, Midlothian, Scotland. [Woitke, P.; Poelman, D. R.] Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. [Alacid, J. M.; Solano, E.] CSIC, INTA, Ctr Astrobiol, Dept Astrofis,Unidad Archivo Datos, Villanueva De La Canada 28691, Spain. [Andrews, S. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ardila, D. R.] CALTECH, NASA Herschel Sci Ctr, Pasadena, CA 91125 USA. [Barrado, D.] Ctr Astron Hispano Aleman, Calar Alto Observ, Almeria 04004, Spain. [Brittain, S.] Clemson Univ, Clemson, SC 29631 USA. [Ciardi, D. R.] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Danchi, W.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Fedele, D.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Fedele, D.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21210 USA. [Heras, A.; Mora, A.] ESA ESAC Gaia SOC, Madrid 28691, Spain. [Krivov, A.] Univ Jena, Inst Astrophys, D-07745 Jena, Germany. [Krivov, A.] Univ Jena, Univ Sternwarte, D-07745 Jena, Germany. [Liseau, R.] Chalmers, Dept Radio & Space Sci, Onsala Space Observ, S-43992 Onsala, Sweden. [Morales-Calderon, M.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Nomura, H.] Kyoto Univ, Grad Sch Sci, Dept Astron, Kyoto 6068502, Japan. [Pantin, E.] CEA, IRFU SAp, AIM UMR 7158, F-91191 Gif Sur Yvette, France. [Ramsay, S.] European So Observ, D-85748 Garching, Germany. [Walker, H.; White, G. J.] Rutherford Appleton Lab, Didcot OX11 ONL, Oxon, England. [White, G. J.] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England. [Meeus, G.; Eiroa, C.; Fedele, D.; Pascucci, I.] Univ Autonoma Madrid, Fac Ciencias, Dep Fis Teor, E-28049 Madrid, Spain. RP Mathews, GS (reprint author), Univ Hawaii, Inst Astron IfA, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. EM gmathews@ifa.hawaii.edu RI Rice, Ken/H-5084-2011; Roberge, Aki/D-2782-2012; Brittain, Sean/K-9001-2012; Fedele, Davide/L-8688-2013; Barrado Navascues, David/C-1439-2017; Solano, Enrique/C-2895-2017; Huelamo, Nuria/C-3042-2017; Montesinos, Benjamin/C-3493-2017; Morales-Calderon, Maria/C-8384-2017; OI Rice, Ken/0000-0002-6379-9185; Roberge, Aki/0000-0002-2989-3725; Brittain, Sean/0000-0001-5638-1330; Fedele, Davide/0000-0001-6156-0034; Barrado Navascues, David/0000-0002-5971-9242; Huelamo, Nuria/0000-0002-2711-8143; Montesinos, Benjamin/0000-0002-7982-2095; Williams, Jonathan/0000-0001-5058-695X; Morales-Calderon, Maria/0000-0001-9526-9499; Mendigutia, Ignacio/0000-0002-0233-5328; Ciardi, David/0000-0002-5741-3047 FU NASA/JPL; EC [PIEF-GA-2008-220891]; Spanish MICINN [AYA2008-02156]; PNPS; CNES; ANR [ANR-07-BLAN-0221]; NASA; BMVIT (Austria); ESA-PRODEX (Belgium); CEA/CNES (France); DLR (Germany); ASI/INAF (Italy); CICYT/MCYT (Spain); [AYA 2008-01727] FX We thank the PACS instrument team for their dedicated support. G.S.M., D.R.A., S.D.B., W.D., C.A.G., C.D.H., I.P., B.R., A.R., G.S. and J.P.W. acknowledge NASA/JPL for funding support. C.E., G.M., I.M., and B.M. are partly supported by Spanish grant AYA 2008-01727, and J.M.A. and E.S. by Spanish grant AYA2008-02156. C.P. acknowledges the funding from the EC 7th Framework Program as a Marie Curie Intra-European Fellow (PIEF-GA-2008-220891). E.S. and J.M.A. acknowledge funding from the Spanish MICINN through grant AYA2008-02156. The members of LAOG acknowledge PNPS, CNES and ANR (contract ANR-07-BLAN-0221) for financial support. 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. PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA (Germany); INAF- IFSI/OAA/OAP/OAT, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy), and CICYT/MCYT (Spain). HIPE is a joint development by the Herschel Science Ground Segment Consortium, consisting of ESA, the NASA Herschel Science Center, and the HIFI, PACS and SPIRE consortia. NR 40 TC 24 Z9 25 U1 0 U2 5 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL-AUG PY 2010 VL 518 AR L127 DI 10.1051/0004-6361/201014595 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 646GQ UT WOS:000281527200128 ER PT J AU Matthews, BC Sibthorpe, B Kennedy, G Phillips, N Churcher, L Duchene, G Greaves, JS Lestrade, JF Moro-Martin, A Wyatt, MC Bastien, P Biggs, A Bouvier, J Butner, HM Dent, WRF Di Francesco, J Eisloffel, J Graham, J Harvey, P Hauschildt, P Holland, WS Horner, J Ibar, E Ivison, RJ Johnstone, D Kalas, P Kavelaars, J Rodriguez, D Udry, S van der Werf, P Wilner, D Zuckerman, B AF Matthews, B. C. Sibthorpe, B. Kennedy, G. Phillips, N. Churcher, L. Duchene, G. Greaves, J. S. Lestrade, J. -F. Moro-Martin, A. Wyatt, M. C. Bastien, P. Biggs, A. Bouvier, J. Butner, H. M. Dent, W. R. F. Di Francesco, J. Eisloeffel, J. Graham, J. Harvey, P. Hauschildt, P. Holland, W. S. Horner, J. Ibar, E. Ivison, R. J. Johnstone, D. Kalas, P. Kavelaars, J. Rodriguez, D. Udry, S. van der Werf, P. Wilner, D. Zuckerman, B. TI Resolving debris discs in the far-infrared: Early highlights from the DEBRIS survey SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE circumstellar matter; stars: individual: beta Leo; infrared: stars; stars: individual: beta UMa; stars: individual: eta Corvi ID MAIN-SEQUENCE STARS; SUN-LIKE STARS; COLLISIONAL PROCESSES; ETA-CORVI; HOT DUST; DISKS; EVOLUTION; SPITZER; IRAS AB We present results from the earliest observations of DEBRIS, a Herschel key programme to conduct a volume-and flux-limited survey for debris discs in A-type through M-type stars. PACS images (from chop/nod or scan-mode observations) at 100 and 160 mu m are presented toward two A-type stars and one F-type star: beta Leo, beta UMa and eta Corvi. All three stars are known disc hosts. Herschel spatially resolves the dust emission around all three stars (marginally, in the case of beta UMa), providing new information about discs as close as 11 pc with sizes comparable to that of the Solar System. We have combined these data with existing flux density measurements of the discs to refine the SEDs and derive estimates of the fractional luminosities, temperatures and radii of the discs. C1 [Matthews, B. C.; Di Francesco, J.; Johnstone, D.; Kavelaars, J.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Matthews, B. C.; Di Francesco, J.; Johnstone, D.; Kavelaars, J.] Univ Victoria, Victoria, BC V8W 3P6, Canada. [Sibthorpe, B.; Biggs, A.; Holland, W. S.; Ibar, E.; Ivison, R. J.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Kennedy, G.; Churcher, L.; Wyatt, M. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Phillips, N.; Ivison, R. J.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Duchene, G.; Bouvier, J.] Univ Grenoble 1, CNRS, Observ Grenoble, Astrophys Lab, F-38041 Grenoble, France. [Duchene, G.; Graham, J.; Kalas, P.] Univ Calif Berkeley, Dept Astron, Berkeley, CA USA. [Greaves, J. S.] Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. [Lestrade, J. -F.] CNRS, Observ Paris, F-75014 Paris, France. [Moro-Martin, A.] CSIC INTA, Ctr Astrobiol, Madrid 28850, Spain. [Moro-Martin, A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Bastien, P.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. [Bastien, P.] Univ Montreal, Observ Mt Megant, Montreal, PQ H3C 3J7, Canada. [Butner, H. M.] James Madison Univ, Dept Phys & Astron, Harrisonburg, VA 22807 USA. [Dent, W. R. F.] ALMA JAO, Santiago, Chile. [Eisloeffel, J.] Thuringer Landessternwarte, D-07778 Tautenburg, Germany. [Harvey, P.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Hauschildt, P.] Hamburger Sternwarte, D-21029 Hamburg, Germany. [Horner, J.] Univ Durham, Dept Phys, Sci Labs, Durham DH1 3LE, England. [Rodriguez, D.; Zuckerman, B.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Udry, S.] Univ Geneva, Dept Astron, Observ Geneva, CH-1211 Geneva 4, Switzerland. [van der Werf, P.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Wilner, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Matthews, BC (reprint author), Natl Res Council Canada, Herzberg Inst Astrophys, 5071 W Saanich Rd, Victoria, BC V9E 2E7, Canada. EM brenda.matthews@nrc-cnrc.gc.ca RI Ivison, R./G-4450-2011; OI Ivison, R./0000-0001-5118-1313; Horner, Jonti/0000-0002-1160-7970; Kennedy, Grant/0000-0001-6831-7547 FU NASA [1353184]; Canadian Space Agency FX We thank our referee, K. Stapelfeldt, for a constructive and insightful report. Support for this work, part of the NASA Herschel Science Center Key Program Data Analysis Program, was provided by NASA through a contract (No. 1353184, PI: H. M. Butner) issued by the Jet Propulsion Laboratory, California Institute of Technology under contract with NASA. This project is supported by a Space Science Enhancement Program grant from the Canadian Space Agency. NR 23 TC 61 Z9 62 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 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL-AUG PY 2010 VL 518 AR L135 DI 10.1051/0004-6361/201014667 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 646GQ UT WOS:000281527200136 ER PT J AU Meeus, G Pinte, C Woitke, P Montesinos, B Mendigutia, I Riviere-Marichalar, P Eiroa, C Mathews, GS Vandenbussche, B Howard, CD Roberge, A Sandell, G Duchene, G Menard, F Grady, CA Dent, WRF Kamp, I Augereau, JC Thi, WF Tilling, I Alacid, JM Andrews, S Ardila, DR Aresu, G Barrado, D Brittain, S Ciardi, DR Danchi, W Fedele, D de Gregorio-Monsalvo, I Heras, A Huelamo, N Krivov, A Lebreton, J Liseau, R Martin-Zaidi, C Mora, A Morales-Calderon, M Nomura, H Pantin, E Pascucci, I Phillips, N Podio, L Poelman, DR Ramsay, S Riaz, B Rice, K Solano, E Walker, H White, GJ Williams, JP Wright, G AF Meeus, G. Pinte, C. Woitke, P. Montesinos, B. Mendigutia, I. Riviere-Marichalar, P. Eiroa, C. Mathews, G. S. Vandenbussche, B. Howard, C. D. Roberge, A. Sandell, G. Duchene, G. Menard, F. Grady, C. A. Dent, W. R. F. Kamp, I. Augereau, J. C. Thi, W. F. Tilling, I. Alacid, J. M. Andrews, S. Ardila, D. R. Aresu, G. Barrado, D. Brittain, S. Ciardi, D. R. Danchi, W. Fedele, D. de Gregorio-Monsalvo, I. Heras, A. Huelamo, N. Krivov, A. Lebreton, J. Liseau, R. Martin-Zaidi, C. Mora, A. Morales-Calderon, M. Nomura, H. Pantin, E. Pascucci, I. Phillips, N. Podio, L. Poelman, D. R. Ramsay, S. Riaz, B. Rice, K. Solano, E. Walker, H. White, G. J. Williams, J. P. Wright, G. TI Gas in the protoplanetary disc of HD 169142: Herschel's view SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE planetary systems; circumstellar matter; stars: pre-main sequence; protoplanetary disks; infrared: planetary systems ID RADIATIVE-TRANSFER; STARS; DUST; SCATTERING; CONTINUUM; HD-169142; EMISSION; SPECTRA; SYSTEMS; GRAINS AB In an effort to simultaneously study the gas and dust components of the disc surrounding the young Herbig Ae star HD 169142, we present far-IR observations obtained with the PACS instrument onboard the Herschel Space Observatory. This work is part of the open time key program GASPS, which is aimed at studying the evolution of protoplanetary discs. To constrain the gas properties in the outer disc, we observed the star at several key gas-lines, including [OI] 63.2 and 145.5 mu m, [CII] 157.7 mu m, CO 72.8 and 90.2 mu m, and o-H(2)O 78.7 and 179.5 mu m. We only detect the [OI] 63.2 mu m line in our spectra, and derive upper limits for the other lines. We complement our data set with PACS photometry and (12/13)CO data obtained with the Submillimeter Array. Furthermore, we derive accurate stellar parameters from optical spectra and UV to mm photometry. We model the dust continuum with the 3D radiative transfer code MCFOST and use this model as an input to analyse the gas lines with the thermo-chemical code ProDIMo. Our dataset is consistent with a simple model in which the gas and dust are well-mixed in a disc with a continuous structure between 20 and 200 AU, but this is not a unique solution. Our modelling effort allows us to constrain the gas-to-dust mass ratio as well as the relative abundance of the PAHs in the disc by simultaneously fitting the lines of several species that originate in different regions. Our results are inconsistent with a gas-poor disc with a large UV excess; a gas mass of 5.0 +/- 2.0 x 10(-3) M(circle dot) is still present in this disc, in agreement with earlier CO observations. C1 [Meeus, G.; Eiroa, C.; Fedele, D.] Univ Autonoma Madrid, Fac Ciencias, Dep Fis Teor, E-28049 Madrid, Spain. [Pinte, C.] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England. [Pinte, C.; Duchene, G.; Menard, F.; Augereau, J. C.; Thi, W. F.; Lebreton, J.; Martin-Zaidi, C.] Univ Grenoble 1, CNRS, Lab Astrophys Grenoble LAOG, UMR 5571, F-38041 Grenoble 09, France. [Woitke, P.; Wright, G.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Woitke, P.; Thi, W. F.; Tilling, I.; Phillips, N.; Rice, K.] Univ Edinburgh, Royal Observ Edinburgh, Inst Astron, SUPA, Edinburgh EH9 3HJ, Midlothian, Scotland. [Woitke, P.; Thi, W. F.; Tilling, I.; Phillips, N.; Rice, K.] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Woitke, P.; Poelman, D. R.] Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. [Montesinos, B.; Mendigutia, I.; Riviere-Marichalar, P.; Barrado, D.; Huelamo, N.] Ctr Astrobiol INTA CSIC, Dept Astrofis, LAEX, Villanueva De La Canada 28691, Spain. [Mathews, G. S.; Williams, J. P.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Vandenbussche, B.] Katholieke Univ Leuven, Inst Sterrenkunde, Leuven, Belgium. [Howard, C. D.; Sandell, G.] NASA, Ames Res Ctr, SOFIA USRA, Moffett Field, CA 94035 USA. [Roberge, A.; Grady, C. A.; Danchi, W.] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA. [Duchene, G.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Grady, C. A.] Eureka Sci, Oakland, CA 96002 USA. [Dent, W. R. F.; de Gregorio-Monsalvo, I.] ALMA, Santiago, Chile. [Dent, W. R. F.; de Gregorio-Monsalvo, I.] European So Observ, Santiago, Chile. [Kamp, I.; Aresu, G.; Podio, L.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Alacid, J. M.; Solano, E.] Ctr Astrobiol INTA CSIC, Dept Astrofis, Unidad Archivo Datos, Spanish Virtual Observ, Villanueva De La Canada 28691, Spain. [Andrews, S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. [Ardila, D. R.] NASA, Herschel Sci Ctr, CALTECH, Pasadena, CA USA. [Barrado, D.] Ctr Astron Hispanoaleman, Calar Alto Observ, Almeria 04004, Spain. [Brittain, S.] Clemson Univ, Dept Phys & Astron, Clemson, SC 29634 USA. [Ciardi, D. R.] NASA, Exoplanet Sci Inst, CALTECH, Pasadena, CA 91125 USA. [Fedele, D.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Fedele, D.; Pascucci, I.; Riaz, B.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Heras, A.] ESTEC SRE C, Res & Sci Support Dept ESA, NL-2200 AG Noordwijk, Netherlands. [Krivov, A.] Univ Jena, Astrophys Inst & Univ Sternwarte, D-07745 Jena, Germany. [Liseau, R.] Chalmers, Dept Radio & Space Sci, Onsala Space Observ, S-43992 Onsala, Sweden. [Mora, A.] ESA ESAC Gaia SOC, Madrid 28691, Spain. [Morales-Calderon, M.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Nomura, H.] Kyoto Univ, Grad Sch Sci, Dept Astron, Kyoto 6068502, Japan. [Pantin, E.] CEA IRFU SAP, AIM UMR 7158, F-91191 Gif Sur Yvette, France. [Ramsay, S.] European So Observ, D-85748 Garching, Germany. [Walker, H.; White, G. J.] Rutherford Appleton Lab, Didcot OX11 OQL, Oxon, England. [White, G. J.] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England. RP Meeus, G (reprint author), Univ Autonoma Madrid, Fac Ciencias, Dep Fis Teor, UAM Campus Cantoblanco, E-28049 Madrid, Spain. EM gwendolyn.meeus@uam.es RI Montesinos, Benjamin/C-3493-2017; Morales-Calderon, Maria/C-8384-2017; Rice, Ken/H-5084-2011; Roberge, Aki/D-2782-2012; Brittain, Sean/K-9001-2012; Fedele, Davide/L-8688-2013; Barrado Navascues, David/C-1439-2017; Solano, Enrique/C-2895-2017; Huelamo, Nuria/C-3042-2017; OI Montesinos, Benjamin/0000-0002-7982-2095; Morales-Calderon, Maria/0000-0001-9526-9499; Mendigutia, Ignacio/0000-0002-0233-5328; Williams, Jonathan/0000-0001-5058-695X; Rice, Ken/0000-0002-6379-9185; Roberge, Aki/0000-0002-2989-3725; Brittain, Sean/0000-0001-5638-1330; Fedele, Davide/0000-0001-6156-0034; Barrado Navascues, David/0000-0002-5971-9242; Huelamo, Nuria/0000-0002-2711-8143; Ciardi, David/0000-0002-5741-3047 FU AYA [2008-01727, 2008-02156, 2008-06189]; EC [PIEF-GA-2008-220891]; PNPS; CNES; ANR [ANR-07-BLAN-0221]; NASA/JPL; BMVIT (Austria); ESA-PRODEX (Belgium); CEA (France); DLR (Germany); ASI (Italy); CICT (Spain); MCT (Spain); CNES (France) FX We thank the PACS instrument team for their dedicated support, O. Panic for a discussion on her data and A. Juhasz for providing the Spitzer/IRS data. C. Eiroa, G. Meeus, I. Mendigutia and B. Montesinos are partly supported by AYA 2008-01727; J. M. Alacid and E. Solano by AYA 2008-02156 and I. d. Gregorio by AYA 2008-06189 (Spanish grants). C. Pinte acknowledges funding from the EC 7th FP as a Marie Curie Intra-European Fellow (PIEF-GA-2008-220891). J.-C. Augereau, G. Duchene, J. Lebreton, C. Martin-Zaidi, F. Mcnard and C. Pinte acknowledge PNPS, CNES and ANR (contract ANR-07-BLAN-0221) for financial support. D. R. Ardila, S. D. Brittain, B. Danchi, C. A. Grady, I. Pascucci, B. Riaz, A. Roberge, G. Sandell and C. D. Howards acknowledge NASA/JPL for funding support. PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KUL, CSL, IMEC (Belgium); CEA, OAMP (France); MPIA (Germany); IFSI, OAP/AOT, OAA/CAISMI, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI (Italy), and CICT/MCT (Spain). NR 26 TC 28 Z9 29 U1 0 U2 5 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL-AUG PY 2010 VL 518 AR L124 DI 10.1051/0004-6361/201014557 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 646GQ UT WOS:000281527200125 ER PT J AU Meixner, M Galliano, F Hony, S Roman-Duval, J Robitaille, T Panuzzo, P Sauvage, M Gordon, K Engelbracht, C Misselt, K Okumura, K Beck, T Bernard, JP Bolatto, A Bot, C Boyer, M Bracker, S Carlson, LR Clayton, GC Chen, CHR Churchwell, E Fukui, Y Galametz, M Hora, JL Hughes, A Indebetouw, R Israel, FP Kawamura, A Kemper, F Kim, S Kwon, E Lawton, B Li, A Long, KS Marengo, M Madden, SC Matsuura, M Oliveira, JM Onishi, T Otsuka, M Paradis, D Poglitsch, A Riebel, D Reach, WT Rubio, M Sargent, B Sewilo, M Simon, JD Skibba, R Smith, LJ Srinivasan, S Tielens, AGGM van Loon, JT Whitney, B Woods, PM AF Meixner, M. Galliano, F. Hony, S. Roman-Duval, J. Robitaille, T. Panuzzo, P. Sauvage, M. Gordon, K. Engelbracht, C. Misselt, K. Okumura, K. Beck, T. Bernard, J. -P. Bolatto, A. Bot, C. Boyer, M. Bracker, S. Carlson, L. R. Clayton, G. C. Chen, C. -H. R. Churchwell, E. Fukui, Y. Galametz, M. Hora, J. L. Hughes, A. Indebetouw, R. Israel, F. P. Kawamura, A. Kemper, F. Kim, S. Kwon, E. Lawton, B. Li, A. Long, K. S. Marengo, M. Madden, S. C. Matsuura, M. Oliveira, J. M. Onishi, T. Otsuka, M. Paradis, D. Poglitsch, A. Riebel, D. Reach, W. T. Rubio, M. Sargent, B. Sewilo, M. Simon, J. D. Skibba, R. Smith, L. J. Srinivasan, S. Tielens, A. G. G. M. van Loon, J. Th. Whitney, B. Woods, P. M. TI HERschel Inventory of The Agents of Galaxy Evolution (HERITAGE): The Large Magellanic Cloud dust SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE Magellanic Clouds; dust, extinction; submillimeter: galaxies; submillimeter: ISM ID INTERSTELLAR DUST; MOLECULAR CLOUDS; SPITZER SURVEY; EXTINCTION; ABUNDANCE; EMISSION; DISTANCE; CARBON; SAGE; IV AB The HERschel Inventory of The Agents of Galaxy Evolution (HERITAGE) of the Magellanic Clouds will use dust emission to investigate the life cycle of matter in both the Large and Small Magellanic Clouds (LMC and SMC). Using the Herschel Space Observatory's PACS and SPIRE photometry cameras, we imaged a 2 degrees x 8 degrees strip through the LMC, at a position angle of similar to 22.5 degrees as part of the science demonstration phase of the Herschel mission. We present the data in all 5 Herschel bands: PACS 100 and 160 mu m and SPIRE 250, 350 and 500 mu m. We present two dust models that both adequately fit the spectral energy distribution for the entire strip and both reveal that the SPIRE 500 mu m emission is in excess of the models by similar to 6 to 17%. The SPIRE emission follows the distribution of the dust mass, which is derived from the model. The PAH-to-dust mass (f(PAH)) image of the strip reveals a possible enhancement in the LMC bar in agreement with previous work. We compare the gas mass distribution derived from the HI 21 cm and CO J = 1-0 line emission maps to the dust mass map from the models and derive gas-to-dust mass ratios (GDRs). The dust model, which uses the standard graphite and silicate optical properties for Galactic dust, has a very low GDR = 65(-18)(+15) making it an unrealistic dust model for the LMC. Our second dust model, which uses amorphous carbon instead of graphite, has a flatter emissivity index in the submillimeter and results in a GDR = 287(-42)(+25) that is more consistent with a GDR inferred from extinction. C1 [Meixner, M.; Roman-Duval, J.; Gordon, K.; Beck, T.; Boyer, M.; Lawton, B.; Long, K. S.; Otsuka, M.; Sargent, B.; Sewilo, M.; Smith, L. J.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Galliano, F.; Hony, S.; Panuzzo, P.; Sauvage, M.; Okumura, K.; Galametz, M.; Madden, S. C.] CEA, Lab AIM, Irfu SAp, F-91191 Gif Sur Yvette, France. [Robitaille, T.; Hora, J. L.] Harvard Univ, Ctr Astrophys, Cambridge, MA 02138 USA. [Engelbracht, C.; Misselt, K.; Skibba, R.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Bernard, J. -P.] CNRS, Ctr Etud Spatiale Rayonnements, F-31028 Toulouse, France. [Bolatto, A.] Univ Maryland, Dept Astron, Lab Millimeter Wave Astron, College Pk, MD 20742 USA. [Bot, C.] Observ Astron, F-67000 Strasbourg, France. [Bracker, S.; Churchwell, E.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Carlson, L. R.; Riebel, D.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Clayton, G. C.] Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA 70803 USA. [Chen, C. -H. R.; Indebetouw, R.] Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. [Chen, C. -H. R.; Indebetouw, R.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Fukui, Y.; Kawamura, A.; Tielens, A. G. G. M.] Nagoya Univ, Dept Astrophys, Chikusa Ku, Nagoya, Aichi 464, Japan. [Hughes, A.] Swinburne Univ Technol, Ctr Supercomp & Astrophys, Hawthorn, Vic 3122, Australia. [Israel, F. P.] Leiden Univ, Sterrewacht Leiden, NL-2300 RA Leiden, Netherlands. [Kemper, F.; Woods, P. M.] Univ Manchester, Jodrell Bank, Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England. [Kim, S.; Kwon, E.] Sejong Univ, Seoul 143747, South Korea. [Li, A.] Univ Missouri, Dept Phys & Astron, Columbia, MO 65211 USA. [Marengo, M.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Matsuura, M.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Matsuura, M.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Oliveira, J. M.; van Loon, J. Th.] Univ Keele, Sch Phys & Geog Sci, Lennard Jones Labs, Keele ST5 5BG, Staffs, England. [Onishi, T.] Osaka Prefecture Univ, Dept Phys Sci, Osaka 5998531, Japan. [Paradis, D.; Reach, W. T.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Poglitsch, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Reach, W. T.] Univ Space Res Assoc, Stratospher Observ Infrared Astron, Moffett Field, CA 94035 USA. [Rubio, M.] Univ Chile, Dept Astron, Santiago, Chile. [Simon, J. D.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [Srinivasan, S.] CNRS, IAP, UPR 341, F-75014 Paris, France. [Whitney, B.] Space Sci Inst, Boulder, CO 80301 USA. [Meixner, M.] Harvard CfA, Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Meixner, M (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. EM meixner@stsci.edu RI Kemper, Francisca/D-8688-2011; Rubio, Monica/J-3384-2016; OI Kemper, Francisca/0000-0003-2743-8240; Bot, Caroline/0000-0001-6118-2985; Hora, Joseph/0000-0002-5599-4650; Reach, William/0000-0001-8362-4094; Robitaille, Thomas/0000-0002-8642-1329 FU NASA Herschel Science Center, JPL [1381522, 1381650]; FONDECYT [1080335]; FONDAP [15010003]; European Space Agency (ESA); PACS and SPIRE; Herschel Science Center; PACS and SPIRE instrument control centers; NASA Herschel Science Center FX We acknowledge financial support from the NASA Herschel Science Center, JPL contracts # 1381522 & 1381650. M. R. is supported by FONDECYT No. 1080335 and FONDAP No. 15010003. We thank the contributions and support from the European Space Agency (ESA), the PACS and SPIRE teams, the Herschel Science Center and the NASA Herschel Science Center (esp. A. Barbar and K. Xu) and the PACS and SPIRE instrument control centers, without which none of this work would be possible. NR 30 TC 84 Z9 84 U1 0 U2 3 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL-AUG PY 2010 VL 518 AR L71 DI 10.1051/0004-6361/201014662 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 646GQ UT WOS:000281527200072 ER PT J AU Molinari, S Swinyard, B Bally, J Barlow, M Bernard, JP Martin, P Moore, T Noriega-Crespo, A Plume, R Testi, L Zavagno, A Abergel, A Ali, B Anderson, L Andre, P Baluteau, JP Battersby, C Beltran, MT Benedettini, M Billot, N Blommaert, J Bontemps, S Boulanger, F Brand, J Brunt, C Burton, M Calzoletti, L Carey, S Caselli, P Cesaroni, R Cernicharo, J Chakrabarti, S Chrysostomou, A Cohen, M Compiegne, M de Bernardis, P de Gasperis, G di Giorgio, AM Elia, D Faustini, F Flagey, N Fukui, Y Fuller, GA Ganga, K Garcia-Lario, P Glenn, J Goldsmith, PF Griffin, M Hoare, M Huang, M Ikhenaode, D Joblin, C Joncas, G Juvela, M Kirk, JM Lagache, G Li, JZ Lim, TL Lord, SD Marengo, M Marshall, DJ Masi, S Massi, F Matsuura, M Minier, V Miville-Deschenes, MA Montier, LA Morgan, L Motte, F Mottram, JC Muller, TG Natoli, P Neves, J Olmi, L Paladini, R Paradis, D Parsons, H Peretto, N Pestalozzi, M Pezzuto, S Piacentini, F Piazzo, L Polychroni, D Pomares, M Popescu, CC Reach, WT Ristorcelli, I Robitaille, JF Robitaille, T Rodon, JA Roy, A Royer, P Russeil, D Saraceno, P Sauvage, M Schilke, P Schisano, E Schneider, N Schuller, F Schulz, B Sibthorpe, B Smith, HA Smith, MD Spinoglio, L Stamatellos, D Strafella, F Stringfellow, GS Sturm, E Taylor, R Thompson, MA Traficante, A Tuffs, RJ Umana, G Valenziano, L Vavrek, R Veneziani, M Viti, S Waelkens, C Ward-Thompson, D White, G Wilcock, LA Wyrowski, F Yorke, HW Zhang, Q AF Molinari, S. Swinyard, B. Bally, J. Barlow, M. Bernard, J. -P. Martin, P. Moore, T. Noriega-Crespo, A. Plume, R. Testi, L. Zavagno, A. Abergel, A. Ali, B. Anderson, L. Andre, P. Baluteau, J. -P. Battersby, C. Beltran, M. T. Benedettini, M. Billot, N. Blommaert, J. Bontemps, S. Boulanger, F. Brand, J. Brunt, C. Burton, M. Calzoletti, L. Carey, S. Caselli, P. Cesaroni, R. Cernicharo, J. Chakrabarti, S. Chrysostomou, A. Cohen, M. Compiegne, M. de Bernardis, P. de Gasperis, G. di Giorgio, A. M. Elia, D. Faustini, F. Flagey, N. Fukui, Y. Fuller, G. A. Ganga, K. Garcia-Lario, P. Glenn, J. Goldsmith, P. F. Griffin, M. Hoare, M. Huang, M. Ikhenaode, D. Joblin, C. Joncas, G. Juvela, M. Kirk, J. M. Lagache, G. Li, J. Z. Lim, T. L. Lord, S. D. Marengo, M. Marshall, D. J. Masi, S. Massi, F. Matsuura, M. Minier, V. Miville-Deschenes, M. -A. Montier, L. A. Morgan, L. Motte, F. Mottram, J. C. Mueller, T. G. Natoli, P. Neves, J. Olmi, L. Paladini, R. Paradis, D. Parsons, H. Peretto, N. Pestalozzi, M. Pezzuto, S. Piacentini, F. Piazzo, L. Polychroni, D. Pomares, M. Popescu, C. C. Reach, W. T. Ristorcelli, I. Robitaille, J. -F. Robitaille, T. Rodon, J. A. Roy, A. Royer, P. Russeil, D. Saraceno, P. Sauvage, M. Schilke, P. Schisano, E. Schneider, N. Schuller, F. Schulz, B. Sibthorpe, B. Smith, H. A. Smith, M. D. Spinoglio, L. Stamatellos, D. Strafella, F. Stringfellow, G. S. Sturm, E. Taylor, R. Thompson, M. A. Traficante, A. Tuffs, R. J. Umana, G. Valenziano, L. Vavrek, R. Veneziani, M. Viti, S. Waelkens, C. Ward-Thompson, D. White, G. Wilcock, L. A. Wyrowski, F. Yorke, H. W. Zhang, Q. TI Clouds, filaments, and protostars: The Herschel Hi-GAL Milky Way SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: formation; ISM: structure; ISM: clouds; Galaxy: general ID MOLECULAR CLOUDS; GALACTIC PLANE; MU-M AB We present the first results from the science demonstration phase for the Hi-GAL survey, the Herschel key program that will map the inner Galactic plane of the Milky Way in 5 bands. We outline our data reduction strategy and present some science highlights on the two observed 2 degrees x 2 degrees tiles approximately centered at l = 30 degrees and l = 59 degrees. The two regions are extremely rich in intense and highly structured extended emission which shows a widespread organization in filaments. Source SEDs can be built for hundreds of objects in the two fields, and physical parameters can be extracted, for a good fraction of them where the distance could be estimated. The compact sources (which we will call cores' in the following) are found for the most part to be associated with the filaments, and the relationship to the local beam-averaged column density of the filament itself shows that a core seems to appear when a threshold around A(V) similar to 1 is exceeded for the regions in the l = 59 degrees field; a A(V) value between 5 and 10 is found for the l = 30 degrees field, likely due to the relatively higher distances of the sources. This outlines an exciting scenario where diffuse clouds first collapse into filaments, which later fragment to cores where the column density has reached a critical level. In spite of core L/M ratios being well in excess of a few for many sources, we find core surface densities between 0.03 and 0.5 g cm(-2). Our results are in good agreement with recent MHD numerical simulations of filaments forming from large-scale converging flows. C1 [Molinari, S.; Benedettini, M.; di Giorgio, A. M.; Elia, D.; Pestalozzi, M.; Pezzuto, S.; Polychroni, D.; Saraceno, P.; Schisano, E.; Spinoglio, L.] INAF Ist Fis Spazio Interplanetario, I-00133 Rome, Italy. [Swinyard, B.; Lim, T. L.; White, G.] Rutherford Appleton Labs, STFC, Didcot, Oxon, England. [Bally, J.; Battersby, C.; Glenn, J.; Stringfellow, G. S.] Univ Colorado, Dept Astrophys & Planetary Sci, CASA, Boulder, CO 80309 USA. [Barlow, M.; Matsuura, M.; Viti, S.] UCL, Dept Phys & Astron, London, England. [Barlow, M.; Matsuura, M.; Viti, S.] Univ Toulouse, UPS, CESR, Toulouse, France. [Barlow, M.; Matsuura, M.; Viti, S.] CNRS, UMR5187, Toulouse, France. [Martin, P.; Roy, A.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON, Canada. [Moore, T.; Morgan, L.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5UX, Merseyside, England. [Noriega-Crespo, A.; Carey, S.; Flagey, N.; Paladini, R.; Paradis, D.; Reach, W. T.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Plume, R.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Testi, L.; Beltran, M. T.; Cesaroni, R.; Massi, F.; Olmi, L.] INAF Osservatorio Astrofis Arcetri, Florence, Italy. [Testi, L.] European So Observ, D-8046 Garching, Germany. [Zavagno, A.; Anderson, L.; Baluteau, J. -P.; Pomares, M.; Rodon, J. A.; Russeil, D.] Univ Aix Marseille 1, LAM, Marseille, France. [Abergel, A.; Boulanger, F.; Lagache, G.; Miville-Deschenes, M. -A.] Univ Paris 11, Inst Astrophys Spatiale, Orsay, France. [Ali, B.; Billot, N.; Lord, S. D.; Schulz, B.] CALTECH, NASA Herschel Sci Ctr, Pasadena, CA 91125 USA. [Andre, P.; Bontemps, S.; Minier, V.; Motte, F.; Peretto, N.; Sauvage, M.; Schneider, N.] Univ Paris Diderot, CEA DSM INSU CNRS, Lab AIM, IRFU SAp,CEA Saclay, F-91191 Gif Sur Yvette, France. [Blommaert, J.; Royer, P.; Waelkens, C.] Katholieke Univ Leuven, Inst Astron, Louvain, Belgium. [Bontemps, S.] Univ Bordeaux, LAB, CNRS, F-33271 Floirac, France. [Brand, J.] INAF Ist Radioastron, Bologna, Italy. Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England. [Burton, M.] Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia. [Strafella, F.] Univ Salento, Dipartimento Fis, Lecce, Italy. [Caselli, P.; Hoare, M.] Univ Leeds, Sch Phys & Astron, Leeds, W Yorkshire, England. [Cernicharo, J.] CSIC, INTA, Ctr Astrobiol, Madrid, Spain. [Marengo, M.; Robitaille, T.; Smith, H. A.; Zhang, Q.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Chrysostomou, A.] Joint Astron Ctr, Hilo, HI USA. [Cohen, M.] UCB, Radio Astron Lab, Berkeley, CA USA. [Compiegne, M.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 1A1, Canada. [de Bernardis, P.; Masi, S.; Piacentini, F.; Veneziani, M.] Univ Rome 1, Dipartimento Fis, I-00185 Rome, Italy. [de Gasperis, G.; Natoli, P.; Traficante, A.] Univ Roma Tor Vergata, Dipartimento Fis, I-00173 Rome, Italy. [Schilke, P.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Fukui, Y.] Nagoya Univ, Dept Astrophys, Nagoya, Aichi 464, Japan. [Fuller, G. A.; Peretto, N.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Ganga, K.] Univ Paris 07, APC, CNRS, F-75205 Paris 13, France. [Garcia-Lario, P.; Vavrek, R.] European Space Astron Ctr, Herschel Sci Ctr, Madrid 28080, Spain. [Goldsmith, P. F.; Yorke, H. W.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Griffin, M.; Kirk, J. M.; Sibthorpe, B.; Stamatellos, D.; Ward-Thompson, D.; Wilcock, L. A.] Cardiff Univ, Sch Phys & Astron, Cardiff, S Glam, Wales. [Huang, M.; Li, J. Z.] Chinese Acad Sci, Natl Astron Observ, Beijing, Peoples R China. [Joncas, G.; Robitaille, J. -F.] Univ Laval, Dept Phys, Quebec City, PQ G1K 7P4, Canada. [Juvela, M.] Univ Helsinki, Dept Phys, FIN-00014 Helsinki, Finland. [Neves, J.; Parsons, H.; Thompson, M. A.] Univ Hertfordshire, Sci & Technol Res Inst, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Mueller, T. G.; Sturm, E.] MPE MPG, Garching, Germany. [Popescu, C. C.] Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England. [Schuller, F.; Wyrowski, F.] MPifR MPG, Bonn, Germany. [Smith, M. D.] Univ Kent, Ctr Astrophys & Planetary Sci, Canterbury, Kent, England. [Taylor, R.] Univ Calgary, Ctr Radio Astron, Calgary, AB, Canada. [Tuffs, R. J.] Max Planck Inst Kernphys, D-69117 Heidelberg, Germany. [Umana, G.] INAF Osservatorio Astrofis Catania, Catania, Italy. [Valenziano, L.] INAF Ist Astrofis Spaziale & Fis Cosm, Bologna, Italy. [Ikhenaode, D.; Piazzo, L.] Univ Roma 1 La Sapienza, Dipartimento Sci & Tecn Informaz & Comunicaz, Rome, Italy. [Calzoletti, L.; Faustini, F.] ASI Sci Data Ctr, I-00044 Frascati, Roma, Italy. [White, G.] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England. [Chakrabarti, S.] UCB Berkeley, Dept Astron, Berkeley, CA USA. [Schisano, E.] Univ Naples Federico 2, Dipartimento Fis, Naples, Italy. [Matsuura, M.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. RP Molinari, S (reprint author), INAF Ist Fis Spazio Interplanetario, Via Fosso Cavaliere 100, I-00133 Rome, Italy. EM sergio.molinari@ifsi-roma.inaf.it RI Goldsmith, Paul/H-3159-2016; Molinari, Sergio/O-4095-2016; Piacentini, Francesco/E-7234-2010; Juvela, Mika/H-6131-2011; Barlow, Michael/A-5638-2009; de Gasperis, Giancarlo/C-8534-2012; OI Reach, William/0000-0001-8362-4094; Robitaille, Thomas/0000-0002-8642-1329; Zhang, Qizhou/0000-0003-2384-6589; Molinari, Sergio/0000-0002-9826-7525; Piacentini, Francesco/0000-0002-5444-9327; Brand, Jan/0000-0003-1615-9043; Massi, Fabrizio/0000-0001-6407-8032; Valenziano, Luca/0000-0002-1170-0104; Juvela, Mika/0000-0002-5809-4834; Barlow, Michael/0000-0002-3875-1171; de Gasperis, Giancarlo/0000-0003-2899-2171; Cesaroni, Riccardo/0000-0002-2430-5103; Stamatellos, Dimitris/0000-0002-4502-8344 FU Italian Space Agency [I/038/080/0] FX Data processing and map production has been possible thanks to generous support from the Italian Space Agency via contract I/038/080/0. We are indebted to Nicola Giordano for the production of the trichromatic overlay images. Data presented in this paper were also analyzed using The Herschel interactive processing environment (HIPE), a joint development by the Herschel Science Ground Segment Consortium, consisting of ESA, the NASA Herschel Science Center, and the HIFI, PACS, and SPIRE consortia. NR 34 TC 259 Z9 260 U1 1 U2 22 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 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL-AUG PY 2010 VL 518 AR L100 DI 10.1051/0004-6361/201014659 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 646GQ UT WOS:000281527200101 ER PT J AU Nisini, B Benedettini, M Codella, C Giannini, T Liseau, R Neufeld, D Tafalla, M van Dishoeck, EF Bachiller, R Baudry, A Benz, AO Bergin, E Bjerkeli, P Blake, G Bontemps, S Braine, J Bruderer, S Caselli, P Cernicharo, J Daniel, F Encrenaz, P di Giorgio, AM Dominik, C Doty, S Fich, M Fuente, A Goicoechea, JR de Graauw, T Helmich, F Herczeg, G Herpin, F Hogerheijde, M Jacq, T Johnstone, D Jorgensen, J Kaufman, M Kristensen, L Larsson, B Lis, D Marseille, M McCoey, C Melnick, G Olberg, M Parise, B Pearson, J Plume, R Risacher, C Santiago, J Saraceno, P Shipman, R van Kempen, TA Visser, R Viti, S Wampfler, S Wyrowski, F van der Tak, F Yildiz, UA Delforge, B Desbat, J Hatch, WA Peron, I Schieder, R Stern, JA Teyssier, D Whyborn, N AF Nisini, B. Benedettini, M. Codella, C. Giannini, T. Liseau, R. Neufeld, D. Tafalla, M. van Dishoeck, E. F. Bachiller, R. Baudry, A. Benz, A. O. Bergin, E. Bjerkeli, P. Blake, G. Bontemps, S. Braine, J. Bruderer, S. Caselli, P. Cernicharo, J. Daniel, F. Encrenaz, P. di Giorgio, A. M. Dominik, C. Doty, S. Fich, M. Fuente, A. Goicoechea, J. R. de Graauw, Th. Helmich, F. Herczeg, G. Herpin, F. Hogerheijde, M. Jacq, T. Johnstone, D. Jorgensen, J. Kaufman, M. Kristensen, L. Larsson, B. Lis, D. Marseille, M. McCoey, C. Melnick, G. Olberg, M. Parise, B. Pearson, J. Plume, R. Risacher, C. Santiago, J. Saraceno, P. Shipman, R. van Kempen, T. A. Visser, R. Viti, S. Wampfler, S. Wyrowski, F. van der Tak, F. Yildiz, U. A. Delforge, B. Desbat, J. Hatch, W. A. Peron, I. Schieder, R. Stern, J. A. Teyssier, D. Whyborn, N. TI Water cooling of shocks in protostellar outflows Herschel-PACS map of L1157 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: formation; ISM: jets and outflows; ISM: molecules ID CHESS SPECTRAL SURVEY; CLASS-0 SOURCES; ARRAY CAMERA; EMISSION; REGIONS; GAS; PROGRAM; DUST; SWAS; ICE AB Context. The far-IR/sub-mm spectral mapping facility provided by the Herschel-PACS and HIFI instruments has made it possible to obtain, for the first time, images of H2O emission with a spatial resolution comparable to ground based mm/sub-mm observations. Aims. In the framework of the Water In Star-forming regions with Herschel (WISH) key program, maps in water lines of several outflows from young stars are being obtained, to study the water production in shocks and its role in the outflow cooling. This paper reports the first results of this program, presenting a PACS map of the o-H2O 179 mu m transition obtained toward the young outflow L1157. Methods. The 179 mu m map is compared with those of other important shock tracers, and with previous single-pointing ISO, SWAS, and Odin water observations of the same source that allow us to constrain the H2O abundance and total cooling. Results. Strong H2O peaks are localized on both shocked emission knots and the central source position. The H2O 179 mu m emission is spatially correlated with emission from H-2 rotational lines, excited in shocks leading to a significant enhancement of the water abundance. Water emission peaks along the outflow also correlate with peaks of other shock-produced molecular species, such as SiO and NH3. A strong H2O peak is also observed at the location of the proto-star, where none of the other molecules have significant emission. The absolute 179 mu m intensity and its intensity ratio to the H2O 557 GHz line previously observed with Odin/SWAS indicate that the water emission originates in warm compact clumps, spatially unresolved by PACS, having a H2O abundance of the order of 10(-4). This testifies that the clumps have been heated for a time long enough to allow the conversion of almost all the available gas-phase oxygen into water. The total H2O cooling is similar to 10(-1) L-circle dot, about 40% of the cooling due to H-2 and 23% of the total energy released in shocks along the L1157 outflow. C1 [Nisini, B.; Giannini, T.; Bergin, E.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy. [Benedettini, M.; di Giorgio, A. M.; Saraceno, P.; Viti, S.] INAF Ist Fis Spazio Interplanetario, Area Ric Tor Vergata, I-00133 Rome, Italy. [Codella, C.; Caselli, P.] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. [Liseau, R.; Bjerkeli, P.] Chalmers, Onsala Space Observ, Dept Radio & Space Sci, S-43992 Onsala, Sweden. [Neufeld, D.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Tafalla, M.; Bachiller, R.; Fuente, A.; Santiago, J.] IGN Observ Astron Nacl, Alcala De Henares 28800, Spain. [van Dishoeck, E. F.; Hogerheijde, M.; Kristensen, L.; Visser, R.; Yildiz, U. A.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [van Dishoeck, E. F.; Herczeg, G.] Max Planck Inst Extraterr Phys, D-37075 Garching, Germany. [Baudry, A.; Bontemps, S.; Braine, J.; Herpin, F.; Jacq, T.; Desbat, J.] Univ Bordeaux, Lab Astrophys Bordeaux, Bordeaux, France. [Baudry, A.; Bontemps, S.; Braine, J.; Herpin, F.; Jacq, T.; Desbat, J.] CNRS INSU, UMR 5804, F-33271 Floirac, France. [Benz, A. O.; Bruderer, S.; Wampfler, S.] ETH, Inst Astron, CH-8093 Zurich, Switzerland. [Bergin, E.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Blake, G.; Lis, D.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Caselli, P.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Cernicharo, J.; Daniel, F.; Goicoechea, J. R.] CSIC INTA, Dept Astrofis, Ctr Astrobiol, Madrid 28850, Spain. [Encrenaz, P.] Observ Paris, CNRS, LERMA, F-75014 Paris, France. [Encrenaz, P.] Observ Paris, CNRS, UMR 8112, F-75014 Paris, France. [Dominik, C.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. [Dominik, C.] Radboud Univ Nijmegen, Dept Astrophys, IMAPP, NL-6500 GL Nijmegen, Netherlands. [Doty, S.] Denison Univ, Dept Phys & Astron, Granville, OH 43023 USA. [Fich, M.; McCoey, C.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [de Graauw, Th.; Helmich, F.; Marseille, M.; Risacher, C.; Shipman, R.; van der Tak, F.] SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [Johnstone, D.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Johnstone, D.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 1A1, Canada. [Jorgensen, J.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark. [Kaufman, M.] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA. [Larsson, B.; Parise, B.] Stockholm Univ, Dept Astron, S-10691 Stockholm, Sweden. [Melnick, G.; van Kempen, T. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Wyrowski, F.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Pearson, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Plume, R.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Viti, S.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [van der Tak, F.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Delforge, B.; Peron, I.] UCP, UPMC, Inst Lab Etud Rayonnement & Matire Astrophys,ENS, UMR 8112,CNRS,INSU,OP, Paris, France. [Peron, I.] IRAM, Inst Inst Radioastron Millimetr, F-38406 St Martin Dheres, France. [Schieder, R.] Univ Cologne, KOSMA, Inst Phys 1, D-50937 Cologne, Germany. [Teyssier, D.] ESA, European Space Astron Ctr, Madrid 28691, Spain. RP Nisini, B (reprint author), Osserv Astron Roma, INAF, Via Frascati 33, I-00040 Monte Porzio Catone, Italy. EM nisini@oa-roma.inaf.it RI Yildiz, Umut/C-5257-2011; Kristensen, Lars/F-4774-2011; Visser, Ruud/J-8574-2012; Wampfler, Susanne/D-2270-2015; Fuente, Asuncion/G-1468-2016; OI Yildiz, Umut/0000-0001-6197-2864; Kristensen, Lars/0000-0003-1159-3721; Wampfler, Susanne/0000-0002-3151-7657; Fuente, Asuncion/0000-0001-6317-6343; Codella, Claudio/0000-0003-1514-3074 NR 29 TC 60 Z9 60 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 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL-AUG PY 2010 VL 518 AR L120 DI 10.1051/0004-6361/201014603 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 646GQ UT WOS:000281527200121 ER PT J AU Peretto, N Fuller, GA Plume, R Anderson, LD Bally, J Battersby, C Beltran, MT Bernard, JP Calzoletti, L DiGiorgio, AM Faustini, F Kirk, JM Lenfestey, C Marshall, D Martin, P Molinari, S Montier, L Motte, F Ristorcelli, I Rodon, JA Smith, HA Traficante, A Veneziani, M Ward-Thompson, D Wilcock, L AF Peretto, N. Fuller, G. A. Plume, R. Anderson, L. D. Bally, J. Battersby, C. Beltran, M. T. Bernard, J. -P. Calzoletti, L. DiGiorgio, A. M. Faustini, F. Kirk, J. M. Lenfestey, C. Marshall, D. Martin, P. Molinari, S. Montier, L. Motte, F. Ristorcelli, I. Rodon, J. A. Smith, H. A. Traficante, A. Veneziani, M. Ward-Thompson, D. Wilcock, L. TI Mapping the column density and dust temperature structure of IRDCs with Herschel SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: formation; ISM: clouds ID INITIAL MASS FUNCTION; FEEDBACK; CLOUDS; CORES AB Infrared dark clouds (IRDCs) are cold and dense reservoirs of gas potentially available to form stars. Many of these clouds are likely to be pristine structures representing the initial conditions for star formation. The study presented here aims to construct and analyze accurate column density and dust temperature maps of IRDCs by using the first Herschel data from the Hi-GAL galactic plane survey. These fundamental quantities, are essential for understanding processes such as fragmentation in the early stages of the formation of stars in molecular clouds. We have developed a simple pixel-by-pixel SED fitting method, which accounts for the background emission. By fitting a grey-body function at each position, we recover the spatial variations in both the dust column density and temperature within the IRDCs. This method is applied to a sample of 22 IRDCs exhibiting a range of angular sizes and peak column densities. Our analysis shows that the dust temperature decreases significantly within IRDCs, from background temperatures of 20-30 K to minimum temperatures of 8-15 K within the clouds, showing that dense molecular clouds are not isothermal. Temperature gradients have most likely an important impact on the fragmentation of IRDCs. Local temperature minima are strongly correlated with column density peaks, which in a few cases reach N(H2) = 1 x 10(23) cm(-2), identifying these clouds as candidate massive prestellar cores. Applying this technique to the full Hi-GAL data set will provide important constraints on the fragmentation and thermal properties of IRDCs, and help identify hundreds of massive prestellar core candidates. C1 [Peretto, N.; Fuller, G. A.; Lenfestey, C.] Univ Manchester, Jodrell Bank Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England. [Peretto, N.; Motte, F.] Univ Paris Diderot, Lab AIM, CEA DSM, CNRS,IRFU Serv Astrophys,CE Saclay, F-91191 Gif Sur Yvette, France. [Plume, R.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Anderson, L. D.; Rodon, J. A.] CNRS, Lab Astrophys Marseille, UMR 6110, F-75700 Paris, France. [Anderson, L. D.; Rodon, J. A.] Univ Aix Marseille 1, F-13331 Marseille 3, France. [Bally, J.; Battersby, C.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Beltran, M. T.] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. [Kirk, J. M.; Ward-Thompson, D.; Wilcock, L.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Bernard, J. -P.; Marshall, D.; Montier, L.; Ristorcelli, I.] Ctr Etud Spatiale Rayonnements, F-31022 Toulouse, France. [Martin, P.] INAF Inst Fis Spazio Interplanetario, I-00133 Rome, Italy. [DiGiorgio, A. M.; Molinari, S.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON, Canada. [Smith, H. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Calzoletti, L.; Faustini, F.; Traficante, A.; Veneziani, M.] Univ Roma Tor Vergata, Dipartimento Fis, I-00173 Rome, Italy. ASI Sci Data Ctr, I-000444 Rome, Italy. RP Peretto, N (reprint author), Univ Manchester, Jodrell Bank Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England. EM nicolas.peretto@manchester.ac.uk RI Molinari, Sergio/O-4095-2016 OI Molinari, Sergio/0000-0002-9826-7525 NR 17 TC 50 Z9 50 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 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL-AUG PY 2010 VL 518 AR L98 DI 10.1051/0004-6361/201014652 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 646GQ UT WOS:000281527200099 ER PT J AU Phillips, TG Bergin, EA Lis, DC Neufeld, DA Bell, TA Wang, S Crockett, NR Emprechtinger, M Blake, GA Caux, E Ceccarelli, C Cernicharo, J Comito, C Daniel, F Dubernet, ML Encrenaz, P Gerin, M Giesen, TF Goicoechea, JR Goldsmith, PF Herbst, E Joblin, C Johnstone, D Langer, WD Latter, WD Lord, SD Maret, S Martin, PG Melnick, GJ Menten, KM Morris, P Muller, HSP Murphy, JA Ossenkopf, V Pearson, JC Perault, M Plume, R Qin, SL Schilke, P Schlemmer, S Stutzki, J Trappe, N van der Tak, FFS Vastel, C Yorke, HW Yu, S Zmuidzinas, J Boogert, A Gusten, R Hartogh, P Honingh, N Karpov, A Kooi, J Krieg, JM Schieder, R AF Phillips, T. G. Bergin, E. A. Lis, D. C. Neufeld, D. A. Bell, T. A. Wang, S. Crockett, N. R. Emprechtinger, M. Blake, G. A. Caux, E. Ceccarelli, C. Cernicharo, J. Comito, C. Daniel, F. Dubernet, M. -L. Encrenaz, P. Gerin, M. Giesen, T. F. Goicoechea, J. R. Goldsmith, P. F. Herbst, E. Joblin, C. Johnstone, D. Langer, W. D. Latter, W. D. Lord, S. D. Maret, S. Martin, P. G. Melnick, G. J. Menten, K. M. Morris, P. Mueller, H. S. P. Murphy, J. A. Ossenkopf, V. Pearson, J. C. Perault, M. Plume, R. Qin, S. -L. Schilke, P. Schlemmer, S. Stutzki, J. Trappe, N. van der Tak, F. F. S. Vastel, C. Yorke, H. W. Yu, S. Zmuidzinas, J. Boogert, A. Guesten, R. Hartogh, P. Honingh, N. Karpov, A. Kooi, J. Krieg, J. -M. Schieder, R. TI Herschel observations of EXtra-Ordinary Sources (HEXOS): Detection of hydrogen fluoride in absorption towards Orion KL SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: abundances; ISM: molecules; submillimeter: ISM ID MOLECULAR-SPECTROSCOPY; ROTATIONAL-EXCITATION; COLOGNE DATABASE; LINE SURVEY; REGION; CLOUDS; WATER; SUBMILLIMETER; SATELLITE; EMISSION AB We report a detection of the fundamental rotational transition of hydrogen fluoride in absorption towards Orion KL using Herschel/HIFI. After the removal of contaminating features associated with common molecules ("weeds"), the HF spectrum shows a P-Cygni profile, with weak redshifted emission and strong blue-shifted absorption, associated with the low-velocity molecular outflow. We derive an estimate of 2.9 x 10(13) cm(-2) for the HF column density responsible for the broad absorption component. Using our best estimate of the H(2) column density within the low-velocity molecular outflow, we obtain a lower limit of similar to 1.6 x 10(-10) for the HF abundance relative to hydrogen nuclei, corresponding to similar to 0.6% of the solar abundance of fluorine. This value is close to that inferred from previous ISO observations of HF J = 2-1 absorption towards Sgr B2, but is in sharp contrast to the lower limit of 6 x 10(-9) derived by Neufeld et al. for cold, foreground clouds on the line of sight towards G10.6-0.4. C1 [Phillips, T. G.; Lis, D. C.; Bell, T. A.; Emprechtinger, M.; Blake, G. A.; Zmuidzinas, J.; Krieg, J. -M.; Schieder, R.] CALTECH, Cahill Ctr Astron & Astrophys 301 17, Pasadena, CA 91125 USA. [Bergin, E. A.; Wang, S.; Crockett, N. R.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Neufeld, D. A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Caux, E.; Joblin, C.; Vastel, C.] Univ Toulouse UPS, Ctr Etud Spatiale Rayonnements, F-31062 Toulouse 3, France. [Caux, E.; Joblin, C.; Vastel, C.] CNRS INSU, UMR 5187, F-31028 Toulouse 4, France. [Ceccarelli, C.; Maret, S.] Lab Astrophys Observ Grenoble, F-38041 Grenoble 9, France. [Cernicharo, J.; Daniel, F.; Goicoechea, J. R.] Ctr Astrobiol CSIC INTA, Lab Astrofis Mol, Madrid 28850, Spain. [Comito, C.; Menten, K. M.; Schilke, P.; Guesten, R.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Daniel, F.; Encrenaz, P.; Gerin, M.; Perault, M.; Krieg, J. -M.] Observ Paris, UMR8112, CNRS, LERMA, F-75231 Paris 05, France. [Daniel, F.; Encrenaz, P.; Gerin, M.; Perault, M.; Krieg, J. -M.] Ecole Normale Super, F-75231 Paris 05, France. [Dubernet, M. -L.] Univ Paris 06, UMR7092, LPMAA, Paris, France. [Dubernet, M. -L.] Observ Paris, UMR8102, LUTH, Meudon, France. [Giesen, T. F.; Mueller, H. S. P.; Ossenkopf, V.; Qin, S. -L.; Schilke, P.; Schlemmer, S.; Stutzki, J.; Honingh, N.; Schieder, R.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Goldsmith, P. F.; Langer, W. D.; Pearson, J. C.; Yorke, H. W.; Yu, S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Herbst, E.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Herbst, E.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Herbst, E.] Ohio State Univ, Dept Chem, Columbus, OH 43210 USA. [Johnstone, D.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Latter, W. D.; Lord, S. D.; Morris, P.; Boogert, A.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Martin, P. G.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Melnick, G. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Murphy, J. A.; Trappe, N.] Natl Univ Ireland Maynooth, Maynooth, Kildare, Ireland. [Ossenkopf, V.] Univ Groningen, SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [Plume, R.; van der Tak, F. F. S.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Hartogh, P.] MPI Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. RP Phillips, TG (reprint author), CALTECH, Cahill Ctr Astron & Astrophys 301 17, Pasadena, CA 91125 USA. EM tgp@submm.caltech.edu RI Giesen, Thomas /B-9476-2015; Schlemmer, Stephan/E-2903-2015; Trappe, Neil/C-9014-2016; Yu, Shanshan/D-8733-2016; Goldsmith, Paul/H-3159-2016; OI Giesen, Thomas /0000-0002-2401-0049; Schlemmer, Stephan/0000-0002-1421-7281; Trappe, Neil/0000-0003-2527-9821; Mueller, Holger/0000-0002-0183-8927; Maret, Sebastien/0000-0003-1104-4554 FU NASA; NSF [AST-0540882] 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; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astronomico Nacional (IGN), Centro de Astrobiolog a (CSIC-INTA). Sweden: Chalmers University of Technology - MC2, RSS & GARD; Onsala Space Observatory; Swedish National Space Board, Stockholm University - Stockholm Observatory; Switzerland: ETH Zurich, FHNW; USA: Caltech, JPL, NHSC. Support for this work was provided by NASA through an award issued by JPL/Caltech. CSO is supported by the NSF, award AST-0540882. NR 32 TC 33 Z9 33 U1 0 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL-AUG PY 2010 VL 518 AR L109 DI 10.1051/0004-6361/201014570 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 646GQ UT WOS:000281527200110 ER PT J AU Pinte, C Woitke, P Menard, F Duchene, G Kamp, I Meeus, G Mathews, G Howard, CD Grady, CA Thi, WF Tilling, I Augereau, JC Dent, WRF Alacid, JM Andrews, S Ardila, DR Aresu, G Barrado, D Brittain, S Ciardi, DR Danchi, W Eiroa, C Fedele, D de Gregorio-Monsalvo, I Heras, A Huelamo, N Krivov, A Lebreton, J Liseau, R Martin-Zaidi, C Mendigutia, I Montesinos, B Mora, A Morales-Calderon, M Nomura, H Pantin, E Pascucci, I Phillips, N Podio, L Poelman, DR Ramsay, S Riaz, B Rice, K Riviere-Marichalar, P Roberge, A Sandell, G Solano, E Vandenbussche, B Walker, H Williams, JP White, GJ Wright, G AF Pinte, C. Woitke, P. Menard, F. Duchene, G. Kamp, I. Meeus, G. Mathews, G. Howard, C. D. Grady, C. A. Thi, W. -F. Tilling, I. Augereau, J. -C. Dent, W. R. F. Alacid, J. M. Andrews, S. Ardila, D. R. Aresu, G. Barrado, D. Brittain, S. Ciardi, D. R. Danchi, W. Eiroa, C. Fedele, D. de Gregorio-Monsalvo, I. Heras, A. Huelamo, N. Krivov, A. Lebreton, J. Liseau, R. Martin-Zaidi, C. Mendigutia, I. Montesinos, B. Mora, A. Morales-Calderon, M. Nomura, H. Pantin, E. Pascucci, I. Phillips, N. Podio, L. Poelman, D. R. Ramsay, S. Riaz, B. Rice, K. Riviere-Marichalar, P. Roberge, A. Sandell, G. Solano, E. Vandenbussche, B. Walker, H. Williams, J. P. White, G. J. Wright, G. TI The Herschel view of GAS in Protoplanetary Systems (GASPS) First comparisons with a large grid of models SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE astrochemistry; circumstellar matter; protoplanetary disks; stars: formation; radiative transfer; line: formation ID RADIATIVE-TRANSFER; DISK STRUCTURE; MASS STARS; EMISSION; CONTINUUM; ACCRETION; EVOLUTION; DUST AB The Herschel GASPS key program is a survey of the gas phase of protoplanetary discs, targeting 240 objects which cover a large range of ages, spectral types, and disc properties. To interpret this large quantity of data and initiate self-consistent analyses of the gas and dust properties of protoplanetary discs, we have combined the capabilities of the radiative transfer code MCFOST with the gas thermal balance and chemistry code ProDiMo to compute a grid of approximate to 300 000 disc models (DENT). We present a comparison of the first Herschel/GASPS line and continuum data with the predictions from the DENT grid of models. Our objective is to test some of the main trends already identified in the DENT grid, as well as to define better empirical diagnostics to estimate the total gas mass of protoplanetary discs. Photospheric UV radiation appears to be the dominant gas-heating mechanism for Herbig stars, whereas UV excess and/or X-rays emission dominates for T Tauri stars. The DENT grid reveals the complexity in the analysis of far-IR lines and the difficulty to invert these observations into physical quantities. The combination of Herschel line observations with continuum data and/or with rotational lines in the (sub-)millimetre regime, in particular CO lines, is required for a detailed characterisation of the physical and chemical properties of circumstellar discs. C1 [Pinte, C.; Menard, F.; Duchene, G.; Thi, W. -F.; Augereau, J. -C.; Lebreton, J.; Martin-Zaidi, C.] Univ Grenoble 1, CNRS, Lab Astrophys Grenoble LAOG, UMR 5571, F-38041 Grenoble 09, France. [Pinte, C.] Univ Exeter, Sch Phys, Exeter EX4 4QJ, Devon, England. [Woitke, P.; Thi, W. -F.; Tilling, I.; Phillips, N.; Rice, K.] Univ Edinburgh, Royal Observ, Inst Astron, SUPA, Edinburgh EH9 3HJ, Midlothian, Scotland. [Woitke, P.; Wright, G.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Woitke, P.; Poelman, D. R.] Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. [Duchene, G.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Kamp, I.; Aresu, G.; Podio, L.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Meeus, G.; Eiroa, C.; Fedele, D.] Univ Autonoma Madrid, Fac Ciencias, Dep Fis Teor, E-28049 Madrid, Spain. [Mathews, G.; Williams, J. P.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Howard, C. D.] NASA, Ames Res Ctr, SOFIA USRA, Moffett Field, CA 94035 USA. [Grady, C. A.] NASA, Goddard Space Flight Ctr, Eureka Sci & Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA. [Dent, W. R. F.; de Gregorio-Monsalvo, I.; Solano, E.] Joint ALMA Off, ALMA, Santiago, Chile. [Dent, W. R. F.; de Gregorio-Monsalvo, I.; Solano, E.] European So Observ, Santiago 19, Chile. [Alacid, J. M.] CSIC, INTA, Ctr Astrobiol, Dept Astrofis,Unidad Archivo Datos, Villanueva De La Canada 28691, Spain. [Andrews, S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ardila, D. R.] CALTECH, NASA Herschel Sci Ctr, Pasadena, CA 91125 USA. [Barrado, D.] Ctr Astron Hispano Aleman, Calar Alto Observ, Almeria 04004, Spain. [Barrado, D.; Huelamo, N.; Mendigutia, I.; Montesinos, B.; Riviere-Marichalar, P.] CSIC, INTA, Ctr Astrobiol, Dept Astrofis,LAEX, Villanueva De La Canada 28691, Spain. [Brittain, S.] Clemson Univ, Clemson, SC 29631 USA. [Ciardi, D. R.] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Fedele, D.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Fedele, D.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21210 USA. [Heras, A.] ESA ESTEC, Res & Sci Support Dept, NL-2200 AG Noordwijk, Netherlands. [Krivov, A.] Univ Jena, Inst Astrophys, D-07745 Jena, Germany. [Krivov, A.] Univ Jena, Univ Sternwarte, D-07745 Jena, Germany. [Liseau, R.] Chalmers, Onsala Space Observ, Dept Radio & Space Sci, S-43992 Onsala, Sweden. [Mora, A.] ESA ESAC Gaia SOC, Madrid 28691, Spain. [Morales-Calderon, M.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Nomura, H.] Kyoto Univ, Grad Sch Sci, Dept Astron, Kyoto 6068502, Japan. [Pantin, E.] CEA IRFU SAp, AIM UMR 7158, F-91191 Gif Sur Yvette, France. [Pascucci, I.; Riaz, B.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Ramsay, S.] European So Observ, D-85748 Garching, Germany. [Roberge, A.; Sandell, G.] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA. [Vandenbussche, B.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium. [Walker, H.; White, G. J.] Rutherford Appleton Lab, Didcot OX11 OQL, Oxon, England. [White, G. J.] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England. RP Pinte, C (reprint author), Univ Grenoble 1, CNRS, Lab Astrophys Grenoble LAOG, UMR 5571, BP 53, F-38041 Grenoble 09, France. EM christophe.pinte@obs.ujf-grenoble.fr RI Rice, Ken/H-5084-2011; Roberge, Aki/D-2782-2012; Brittain, Sean/K-9001-2012; Fedele, Davide/L-8688-2013; Barrado Navascues, David/C-1439-2017; Solano, Enrique/C-2895-2017; Huelamo, Nuria/C-3042-2017; Montesinos, Benjamin/C-3493-2017; Morales-Calderon, Maria/C-8384-2017; OI Rice, Ken/0000-0002-6379-9185; Roberge, Aki/0000-0002-2989-3725; Brittain, Sean/0000-0001-5638-1330; Fedele, Davide/0000-0001-6156-0034; Barrado Navascues, David/0000-0002-5971-9242; Huelamo, Nuria/0000-0002-2711-8143; Montesinos, Benjamin/0000-0002-7982-2095; Morales-Calderon, Maria/0000-0001-9526-9499; Mendigutia, Ignacio/0000-0002-0233-5328; Williams, Jonathan/0000-0001-5058-695X; Ciardi, David/0000-0002-5741-3047 FU European Commission [PIEF-GA-2008-220891]; PNPS; CNES; ANR [ANR-07-BLAN-0221]; SUPA; NASA/JPL; Spanish MICINN [AYA2008-02156]; [AYA 2008-01727] FX C. Pinte acknowledges funding from the European Commission's 7th Framework Program as a Marie Curie Intra-European Fellow (PIEF-GA-2008-220891). The members of LAOG, Grenoble acknowledge PNPS, CNES and ANR (contract ANR-07-BLAN-0221) for financial support. W.F. Thi acknowledges a SUPA astrobiology fellowship. G. Meeus, C. Eiroa, I. Mendigutia and B. Montesinos are partly supported by Spanish grant AYA 2008-01727. D.R. Ardila, S.D. Brittain, W. Danchi, C.A. Grady, C.D. Howard, G.S. Mathews, I. Pascucci, A. Roberge, B. Riaz, G. Sandell and J.P. Williams acknowledge NASA/JPL for funding support. J.M. Alcid and E. Solano acknowledges funding from the Spanish MICINN (grant AYA2008-02156). NR 25 TC 19 Z9 19 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 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL-AUG PY 2010 VL 518 AR L126 DI 10.1051/0004-6361/201014591 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 646GQ UT WOS:000281527200127 ER PT J AU Sewilo, M Indebetouw, R Carlson, LR Whitney, BA Chen, CHR Meixner, M Robitaille, T van Loon, JT Oliveira, JM Churchwell, E Simon, JD Hony, S Panuzzo, P Sauvage, M Roman-Duval, J Gordon, K Engelbracht, C Misselt, K Okumura, K Beck, T Hora, J Woods, PM AF Sewilo, M. Indebetouw, R. Carlson, L. R. Whitney, B. A. Chen, C. -H. R. Meixner, M. Robitaille, T. van Loon, J. Th. Oliveira, J. M. Churchwell, E. Simon, J. D. Hony, S. Panuzzo, P. Sauvage, M. Roman-Duval, J. Gordon, K. Engelbracht, C. Misselt, K. Okumura, K. Beck, T. Hora, J. Woods, P. M. TI The youngest massive protostars in the Large Magellanic Cloud SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: formation; stars: protostars; Magellanic Clouds ID 2-DIMENSIONAL RADIATIVE-TRANSFER; SPECTRAL ENERGY-DISTRIBUTIONS; STELLAR OBJECTS; PROTOSTELLAR ENVELOPES; STAR-FORMATION; H2O MASERS; EVOLUTION; SPECTROSCOPY; SEDS; OH AB We demonstrate the unique capabilities of Herschel to study very young luminous extragalactic young stellar objects (YSOs) by analyzing a central strip of the Large Magellanic Cloud obtained through the HERITAGE science demonstration program. We combine PACS 100 and 160, and SPIRE 250, 350, and 500 mu m photometry with 2MASS (1.25-2.17 mu m) and Spitzer IRAC and MIPS (3.6-70 mu m) to construct complete spectral energy distributions (SEDs) of compact sources. From these, we identify 207 candidate embedded YSOs in the observed region, similar to 40% never-before identified. We discuss their position in far-infrared color-magnitude space, comparing with previously studied, spectroscopically confirmed YSOs and maser emission. All have red colors indicating massive cool envelopes and great youth. We analyze four example YSOs, determining their physical properties by fitting their SEDs with radiative transfer models. Fitting full SEDs including the Herschel data requires us to increase the size and mass of envelopes included in the models. This implies higher accretion rates (>= 10(-4)M(circle dot)yr(-1)), in agreement with previous outflow studies of high-mass protostars. Our results show that Herschel provides reliable longwave SEDs of large samples of high-mass YSOs; discovers the youngest YSOs whose SEDs peak in Herschel bands; and constrains the physical properties and evolutionary stages of YSOs more precisely than was previously possible. C1 [Sewilo, M.; Meixner, M.; Roman-Duval, J.; Gordon, K.; Beck, T.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Indebetouw, R.; Chen, C. -H. R.] Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. [Carlson, L. R.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Whitney, B. A.] Space Sci Inst, Boulder, CO 80301 USA. [Robitaille, T.; Hora, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [van Loon, J. Th.; Oliveira, J. M.] Univ Keele, Lennard Jones Labs, Sch Phys & Geog Sci, Keele ST5 5BG, Staffs, England. [Churchwell, E.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Simon, J. D.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [Hony, S.; Panuzzo, P.; Sauvage, M.; Okumura, K.] CEA, Lab AIM, Irfu SAp, F-91191 Gif Sur Yvette, France. [Engelbracht, C.; Misselt, K.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Woods, P. M.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. RP Sewilo, M (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. EM mmsewilo@stsci.edu RI Woods, Paul/E-6926-2011; OI Woods, Paul/0000-0003-4340-3590; Hora, Joseph/0000-0002-5599-4650; Robitaille, Thomas/0000-0002-8642-1329 FU NASA Herschel Science Center, JPL [1381522, 1381650]; European Space Agency (ESA); PACS and SPIRE; Herschel Science Center; NASA Herschel Science Center; PACS and SPIRE instrument control center at CEA-Saclay FX We acknowledge financial support from the NASA Herschel Science Center, JPL contracts # 1381522 & 1381650. We thank the contributions and support from the European Space Agency (ESA), the PACS and SPIRE teams, the Herschel Science Center and the NASA Herschel Science Center (esp. A. Barbar and K. Xu) and the PACS and SPIRE instrument control center at CEA-Saclay, without which none of this work would be possible. NR 33 TC 16 Z9 16 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL-AUG PY 2010 VL 518 AR L73 DI 10.1051/0004-6361/201014688 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 646GQ UT WOS:000281527200074 ER PT J AU Stanke, T Stutz, AM Tobin, JJ Ali, B Megeath, ST Krause, O Linz, H Allen, L Bergin, E Calvet, N Di Francesco, J Fischer, WJ Furlan, E Hartmann, L Henning, T Manoj, P Maret, S Muzerolle, J Myers, PC Neufeld, D Osorio, M Pontoppidan, K Poteet, CA Watson, DM Wilson, T AF Stanke, T. Stutz, A. M. Tobin, J. J. Ali, B. Megeath, S. T. Krause, O. Linz, H. Allen, L. Bergin, E. Calvet, N. Di Francesco, J. Fischer, W. J. Furlan, E. Hartmann, L. Henning, T. Manoj, P. Maret, S. Muzerolle, J. Myers, P. C. Neufeld, D. Osorio, M. Pontoppidan, K. Poteet, C. A. Watson, D. M. Wilson, T. TI Hier ist wahrhaftig ein Loch im Himmel The NGC 1999 dark globule is not a globule SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: clouds; ISM: individual objects: NGC 1999; ISM: jets and outflows; infrared: ISM; dust, extinction ID HERBIG AE/BE STARS; SPITZER; CORES; EXTINCTION AB The NGC1999 reflection nebula features a dark patch with a size of similar to 10 000 AU, which has been interpreted as a small, dense foreground globule and possible site of imminent star formation. We present Herschel PACS far-infrared 70 and 160 mu m maps, which reveal a flux deficit at the location of the globule. We estimate the globule mass needed to produce such an absorption feature to be a few tenths to a few M(circle dot). Inspired by this Herschel observation, we obtained APEX LABOCA and SABOCA submillimeter continuum maps, and Magellan PANIC near-infrared images of the region. We do not detect a submillimer source at the location of the Herschel flux decrement; furthermore our observations place an upper limit on the mass of the globule of similar to 2.4x10(-2) M(circle dot). Indeed, the submillimeter maps appear to show a flux depression as well. Furthermore, the near-infrared images detect faint background stars that are less affected by extinction inside the dark patch than in its surroundings. We suggest that the dark patch is in fact a hole or cavity in the material producing the NGC1999 reflection nebula, excavated by protostellar jets from the V380 Ori multiple system. C1 [Stanke, T.; Wilson, T.] ESO, D-85748 Garching, Germany. [Stutz, A. M.; Krause, O.; Linz, H.; Henning, T.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Stutz, A. M.] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. [Stutz, A. M.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Tobin, J. J.; Bergin, E.; Calvet, N.; Hartmann, L.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Ali, B.] CALTECH, Herschel Sci Ctr, NASA, Pasadena, CA 91125 USA. [Megeath, S. T.; Fischer, W. J.; Poteet, C. A.] Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA. [Allen, L.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Di Francesco, J.] Univ Victoria, Dept Phys & Astron, STN CSC, Victoria, BC V8W 3P6, Canada. [Di Francesco, J.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Furlan, E.] CALTECH, JPL, Pasadena, CA 91109 USA. [Manoj, P.; Watson, D. M.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. [Maret, S.] Univ Grenoble 1, Lab Astrophys Grenoble, CNRS, UMR 571, F-38041 Grenoble, France. [Muzerolle, J.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Myers, P. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Neufeld, D.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Osorio, M.] CSIC, Inst Astrofis Andalucia, E-18008 Granada, Spain. [Pontoppidan, K.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. RP Stanke, T (reprint author), ESO, Karl Schwarzschild Str 2, D-85748 Garching, Germany. EM tstanke@eso.org RI Cava, Antonio/C-5274-2017; OI Cava, Antonio/0000-0002-4821-1275; Stutz, Amelia/0000-0003-2300-8200; Maret, Sebastien/0000-0003-1104-4554 FU NASA; [HST-GO-11548.04-A] FX We thank Frank Bertoldi and Markus Albrecht for their invaluable help with BOA, Giorgio Siringo for his help with the SABOCA data, Jonathan Williams for encouraging discussions, and the APEX staff for their help wiht taking the data. Based in part on observations made with Herschel, a European Space Agency Cornerstone Mission with significant participation by NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. J.J.T. acknowledges funding through HST-GO-11548.04-A. Figure 1 produced from data taken with the NASA/ESA Hubble Space Telescope, and obtained from the Hubble Legacy Archive, which is a collaboration between the Space Telescope Science Institute (STScI/NASA), the Space Telescope European Coordinating Facility (ST-ECF/ESA) and the Canadian Astronomy Data Centre (CADC/NRC/CSA). NR 25 TC 15 Z9 15 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL-AUG PY 2010 VL 518 AR L94 DI 10.1051/0004-6361/201014612 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 646GQ UT WOS:000281527200095 ER PT J AU Sturm, B Bouwman, J Henning, T Evans, NJ Acke, B Mulders, GD Waters, LBFM van Dishoeck, EF Meeus, G Green, JD Augereau, JC Olofsson, J Salyk, C Najita, J Herczeg, GJ van Kempen, TA Kristensen, LE Dominik, C Carr, JS Waelkens, C Bergin, E Blake, GA Brown, JM Chen, JH Cieza, L Dunham, MM Glassgold, A Gudel, M Harvey, PM Hogerheijde, MR Jaffe, D Jorgensen, JK Kim, HJ Knez, C Lacy, JH Lee, JE Maret, S Meijerink, R Merin, B Mundy, L Pontoppidan, KM Visser, R Yildiz, UA AF Sturm, B. Bouwman, J. Henning, Th. Evans, N. J., II Acke, B. Mulders, G. D. Waters, L. B. F. M. van Dishoeck, E. F. Meeus, G. Green, J. D. Augereau, J. C. Olofsson, J. Salyk, C. Najita, J. Herczeg, G. J. van Kempen, T. A. Kristensen, L. E. Dominik, C. Carr, J. S. Waelkens, C. Bergin, E. Blake, G. A. Brown, J. M. Chen, J. -H. Cieza, L. Dunham, M. M. Glassgold, A. Guedel, M. Harvey, P. M. Hogerheijde, M. R. Jaffe, D. Jorgensen, J. K. Kim, H. J. Knez, C. Lacy, J. H. Lee, J. -E. Maret, S. Meijerink, R. Merin, B. Mundy, L. Pontoppidan, K. M. Visser, R. Yildiz, U. A. TI First results of the Herschel key program "Dust, Ice and Gas In Time" (DIGIT): Dust and gas spectroscopy of HD 100546 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: individual: HD 100546; infrared: general; stars: pre-main sequence; techniques: spectroscopic ID COMET HALE-BOPP; STAR HD-100546; CORONAGRAPHIC OBSERVATIONS; PROTOPLANETARY DISKS; ASTRONOMICAL UNITS; INFRARED-SPECTRA; ISO-LWS; HERBIG; INNER; TEMPERATURE AB Context. We present far-infrared spectroscopic observations, taken with the Photodetector Array Camera and Spectrometer (PACS) on the Herschel Space Observatory, of the protoplanetary disk around the pre-main-sequence star HD 100546. These observations are the first within the DIGIT Herschel key program, which aims to follow the evolution of dust, ice, and gas from young stellar objects still embedded in their parental molecular cloud core, through the final pre-main-sequence phases when the circumstellar disks are dissipated. Aims. Our aim is to improve the constraints on temperature and chemical composition of the crystalline olivines in the disk of HD 100546 and to give an inventory of the gas lines present in its far-infrared spectrum. Methods. The 69 mu m feature is analyzed in terms of position and shape to derive the dust temperature and composition. Furthermore, we detected 32 emission lines from five gaseous species and measured their line fluxes. Results. The 69 mu m emission comes either from dust grains with similar to 70 K at radii larger than 50 AU, as suggested by blackbody fitting, or it arises from similar to 200K dust at similar to 13AU, close to the midplane, as supported by radiative transfer models. We also conclude that the forsterite crystals have few defects and contain at most a few percent iron by mass. Forbidden line emission from [C II] at 157 mu m and [OI] at 63 and 145 mu m, most likely due to photodissociation by stellar photons, is detected. Furthermore, five H(2)O and several OH lines are detected. We also found high-J rotational transition lines of CO, with rotational temperatures of similar to 300K for the transitions up to J = 22-21 and T similar to 800 K for higher transitions. C1 [Sturm, B.; Bouwman, J.; Henning, Th.; Olofsson, J.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Evans, N. J., II; Green, J. D.; Salyk, C.; Chen, J. -H.; Dunham, M. M.; Harvey, P. M.; Jaffe, D.; Kim, H. J.; Lacy, J. H.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Mulders, G. D.; Waters, L. B. F. M.; Dominik, C.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands. [van Dishoeck, E. F.; Kristensen, L. E.; Hogerheijde, M. R.; Meijerink, R.; Visser, R.; Yildiz, U. A.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Meeus, G.] Univ Autonoma Madrid, Fac Ciencias, Dpt Fis Teor, E-28049 Madrid, Spain. [van Dishoeck, E. F.; Herczeg, G. J.; Brown, J. M.] Max Planck Inst Extraterr Phys, Garching, Germany. [van Kempen, T. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Merin, B.] European Space Astron Ctr ESA, Herschel Sci Ctr, Villanueva De La Canada 28691, Madrid, Spain. [Augereau, J. C.; Maret, S.] Univ Grenoble 1, CNRS, Lab Astrophys Grenoble, UMR5571, F-38041 Grenoble 9, France. [Acke, B.; Waters, L. B. F. M.; Waelkens, C.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium. [Lee, J. -E.] Sejong Univ, Astrophys Res Ctr Struct & Evolut Cosmos, Dept Astron & Space Sci, Seoul 143747, South Korea. [Blake, G. A.; Pontoppidan, K. M.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Carr, J. S.] USN, Res Lab, Washington, DC 20375 USA. [Najita, J.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Knez, C.; Mundy, L.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Cieza, L.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Bergin, E.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Glassgold, A.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Guedel, M.] Univ Vienna, Dept Astron, A-1180 Vienna, Austria. [Mulders, G. D.] Univ Groningen, SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [Dominik, C.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands. [Jorgensen, J. K.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen K, Denmark. RP Sturm, B (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. EM sturm@mpia-hd.mpg.de RI Visser, Ruud/J-8574-2012; Lee , Jeong-Eun/E-2387-2013; Jorgensen, Jes Kristian/L-7936-2014; Yildiz, Umut/C-5257-2011; Kristensen, Lars/F-4774-2011; Guedel, Manuel/C-8486-2015; OI Jorgensen, Jes Kristian/0000-0001-9133-8047; Yildiz, Umut/0000-0001-6197-2864; Kristensen, Lars/0000-0003-1159-3721; Guedel, Manuel/0000-0001-9818-0588; Merin, Bruno/0000-0002-8555-3012; Maret, Sebastien/0000-0003-1104-4554 FU NASA; [AYA 2008-01727] FX Support for this work, part of the Herschel open time key program, was provided by NASA through an award issued by the Jet Propulsion Laboratory, California Institute of Technology. G. Meeus is partly supported by Spanish grant AYA 2008-01727. The authors thank the referee C. Grady for helpful comments that improved the paper. NR 26 TC 58 Z9 58 U1 0 U2 5 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL-AUG PY 2010 VL 518 AR L129 DI 10.1051/0004-6361/201014674 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 646GQ UT WOS:000281527200130 ER PT J AU Thi, WF Mathews, G Menard, F Woitke, P Meeus, G Riviere-Marichalar, P Pinte, C Howard, CD Roberge, A Sandell, G Pascucci, I Riaz, B Grady, CA Dent, WRF Kamp, I Duchene, G Augereau, JC Pantin, E Vandenbussche, B Tilling, I Williams, JP Eiroa, C Barrado, D Alacid, JM Andrews, S Ardila, DR Aresu, G Brittain, S Ciardi, DR Danchi, W Fedele, D de Gregorio-Monsalvo, I Heras, A Huelamo, N Krivov, A Lebreton, J Liseau, R Martin-Zaidi, C Mendigutia, I Montesinos, B Mora, A Morales-Calderon, M Nomura, H Phillips, N Podio, L Poelman, DR Ramsay, S Rice, K Solano, E Walker, H White, GJ Wright, G AF Thi, W. -F. Mathews, G. Menard, F. Woitke, P. Meeus, G. Riviere-Marichalar, P. Pinte, C. Howard, C. D. Roberge, A. Sandell, G. Pascucci, I. Riaz, B. Grady, C. A. Dent, W. R. F. Kamp, I. Duchene, G. Augereau, J. -C. Pantin, E. Vandenbussche, B. Tilling, I. Williams, J. P. Eiroa, C. Barrado, D. Alacid, J. M. Andrews, S. Ardila, D. R. Aresu, G. Brittain, S. Ciardi, D. R. Danchi, W. Fedele, D. de Gregorio-Monsalvo, I. Heras, A. Huelamo, N. Krivov, A. Lebreton, J. Liseau, R. Martin-Zaidi, C. Mendigutia, I. Montesinos, B. Mora, A. Morales-Calderon, M. Nomura, H. Phillips, N. Podio, L. Poelman, D. R. Ramsay, S. Rice, K. Solano, E. Walker, H. White, G. J. Wright, G. TI Herschel-PACS observation of the 10 Myr old T Tauri disk TW Hya Constraining the disk gas mass SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE circumstellar disks ID MAIN-SEQUENCE STARS; PROTOPLANETARY DISKS; YOUNG STARS; X-RAY; HYDRAE; EMISSION; SPECTRA; MODELS; ARRAY AB Planets are formed in disks around young stars. With an age of similar to 10 Myr, TW Hya is one of the nearest T Tauri stars that is still surrounded by a relatively massive disk. In addition a large number of molecules has been found in the TW Hya disk, making TW Hya the perfect test case in a large survey of disks with Herschel-PACS to directly study their gaseous component. We aim to constrain the gas and dust mass of the circumstellar disk around TW Hya. We observed the fine-structure lines of [OI] and [CII] as part of the open-time large program GASPS. We complement this with continuum data and ground-based (12) CO 3-2 and (13)CO 3-2 observations. We simultaneously model the continuum and the line fluxes with the 3D Monte-Carlo code MCFOST and the thermo-chemical code ProDiMo to derive the gas and dust masses. We detect the [OI] line at 63 mu m. The other lines that were observed, [OI] at 145 mu m and [CII] at 157 mu m, are not detected. No extended emission has been found. Preliminary modeling of the photometric and line data assuming [(12)CO]/[(13)CO] = 69 suggests a dust mass for grains with radius < 1 mm of similar to 1.9 x 10(-4) M(circle dot) (total solid mass of 3 x 10(-3) M(circle dot)) and a gas mass of (0.5-5) x 10(-3) M(circle dot). The gas-to-dust mass may be lower than the standard interstellar value of 100. C1 [Thi, W. -F.; Woitke, P.; Tilling, I.; Phillips, N.; Rice, K.] Univ Edinburgh, Inst Astron, SUPA, Royal Observ Edinburgh, Edinburgh EH8 9YL, Midlothian, Scotland. [Thi, W. -F.; Menard, F.; Pinte, C.; Duchene, G.; Augereau, J. -C.; Lebreton, J.; Martin-Zaidi, C.] Univ Grenoble 1, CNRS, Lab Astrophys Grenoble LAOG, UMR 5571, F-38041 Grenoble 09, France. [Mathews, G.; Williams, J. P.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Woitke, P.; Huelamo, N.; Mendigutia, I.; Montesinos, B.; Wright, G.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Woitke, P.; Poelman, D. R.] Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. [Meeus, G.; Eiroa, C.] Univ Autonoma Madrid, Fac Ciencias, Dep Fis Teor, E-28049 Madrid, Spain. [Riviere-Marichalar, P.; Barrado, D.] CSIC, INTA, Ctr Astrobiol, Dept Astrofis,LAEX, Villanueva De La Canada 28691, Spain. [Pinte, C.] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England. [Howard, C. D.] NASA, Ames Res Ctr, SOFIA USRA, Moffett Field, CA 94035 USA. [Roberge, A.] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA. [Pascucci, I.; Riaz, B.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Grady, C. A.] NASA, Goddard Space Flight Ctr, Eureka Sci & Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA. [Dent, W. R. F.; de Gregorio-Monsalvo, I.] ESO ALMA, Santiago, Chile. [Kamp, I.; Aresu, G.; Podio, L.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Duchene, G.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Pantin, E.] CEA IRFU SAp, AIM UMR 7158, F-91191 Gif Sur Yvette, France. [Vandenbussche, B.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium. [Barrado, D.] Ctr Astron Hispano Aleman, Calar Alto Observ, Almeria 04004, Spain. [Sandell, G.; Alacid, J. M.; Solano, E.] CSIC, INTA, Ctr Astrobiol, Dept Astrofis,Unidad Archivo Datos, Villanueva De La Canada 28691, Spain. [Andrews, S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ardila, D. R.] CALTECH, NASA Herschel Sci Ctr, Pasadena, CA 91125 USA. [Brittain, S.] Clemson Univ, Clemson, SC USA. [Ciardi, D. R.] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Fedele, D.] Univ Autonomade Madrid, Fac Ciencias, Dept Fis Teor, Madrid 28049, Spain. [Fedele, D.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Fedele, D.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21210 USA. [Heras, A.] ESA ESTEC, Res & Sci Support Dept, NL-2200 AG Noordwijk, Netherlands. [Krivov, A.] Univ Jena, Inst Astrophys, D-07745 Jena, Germany. [Krivov, A.] Univ Jena, Univ Sternwarte, D-07745 Jena, Germany. [Liseau, R.; Mora, A.] Chalmers, Onsala Space Observ, Dept Radio & Space Sci, S-43992 Onsala, Sweden. [Morales-Calderon, M.] ESA ESAC Gaia SOC, Madrid 28691, Spain. [Nomura, H.] Kyoto Univ, Grad Sch Sci, Dept Astron, Kyoto 6068502, Japan. [Ramsay, S.] European So Observ, D-85748 Garching, Germany. [Walker, H.; White, G. J.] Rutherford Appleton Lab, Didcot OX11 OQL, Oxon, England. [White, G. J.] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England. RP Thi, WF (reprint author), Univ Edinburgh, Inst Astron, SUPA, Royal Observ Edinburgh, Edinburgh EH8 9YL, Midlothian, Scotland. EM wfdt@roe.ac.uk RI Rice, Ken/H-5084-2011; Roberge, Aki/D-2782-2012; Brittain, Sean/K-9001-2012; Fedele, Davide/L-8688-2013; Barrado Navascues, David/C-1439-2017; Solano, Enrique/C-2895-2017; Huelamo, Nuria/C-3042-2017; Montesinos, Benjamin/C-3493-2017; Morales-Calderon, Maria/C-8384-2017; OI Ciardi, David/0000-0002-5741-3047; Rice, Ken/0000-0002-6379-9185; Roberge, Aki/0000-0002-2989-3725; Brittain, Sean/0000-0001-5638-1330; Fedele, Davide/0000-0001-6156-0034; Barrado Navascues, David/0000-0002-5971-9242; Huelamo, Nuria/0000-0002-2711-8143; Montesinos, Benjamin/0000-0002-7982-2095; Morales-Calderon, Maria/0000-0001-9526-9499; Mendigutia, Ignacio/0000-0002-0233-5328; Williams, Jonathan/0000-0001-5058-695X FU SUPA astrobiology fellowship; Spanish [AYA 2008-01727]; EC 7th Framework Program [PIEF-GA-2008-220891]; NASA/JPL; Spanish MICINN [AYA2008-02156]; PNPS, CNES and ANR [ANR-07-BLAN-0221] FX W.-F. Thi acknowledges a SUPA astrobiology fellowship. G. Meeus, C. Eiroa, J. Maldonado and B. Montesinos are partly supported by Spanish grant AYA 2008-01727. C. Pinte acknowledges the funding from the EC 7th Framework Program as a Marie Curie Intra-European Fellow (PIEF-GA-2008-220891). D.R. Ardila, S.D. Brittain, C.A. Grady, I. Pascucci, B. Riaz, G. Sandell and C.D. Howards, J.-P. Williams, G. Matthews, A. Roberge, W. Danchi acknowledge NASA/JPL for funding support. E. Solano and J.M. Alacid acknowledge the funding from the Spanish MICINN through grant AYA2008-02156. The LAOG group acknowledges PNPS, CNES and ANR (contract ANR-07-BLAN-0221) for financial support. NR 33 TC 43 Z9 44 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 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL-AUG PY 2010 VL 518 AR L125 DI 10.1051/0004-6361/201014578 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 646GQ UT WOS:000281527200126 ER PT J AU Vaccari, M Marchetti, L Franceschini, A Altieri, B Amblard, A Arumugam, V Auld, R Aussel, H Babbedge, T Blain, A Bock, J Boselli, A Buat, V Burgarella, D Castro-Rodriguez, N Cava, A Chanial, P Clements, DL Conley, A Conversi, L Cooray, A Dowell, CD Dwek, E Dye, S Eales, S Elbaz, D Farrah, D Fox, M Gear, W Glenn, J Solares, EAG Griffin, M Halpern, M Hatziminaoglou, E Huang, J Ibar, E Isaak, K Ivison, RJ Lagache, G Levenson, L Lu, N Madden, S Maffei, B Mainetti, G Mortier, AMJ Nguyen, HT O'Halloran, B Oliver, SJ Omont, A Page, MJ Panuzzo, P Papageorgiou, A Pearson, CP Perez-Fournon, I Pohlen, M Rawlings, JI Raymond, G Rigopoulou, D Rizzo, D Rodighiero, G Roseboom, IG Rowan-Robinson, M Portal, MS Schulz, B Scott, D Seymour, N Shupe, DL Smith, AJ Stevens, JA Symeonidis, M Trichas, M Tugwell, KE Valiante, E Valtchanov, I Vigroux, L Wang, L Ward, R Wright, G Xu, CK Zemcov, M AF Vaccari, M. Marchetti, L. Franceschini, A. Altieri, B. Amblard, A. Arumugam, V. Auld, R. Aussel, H. Babbedge, T. Blain, A. Bock, J. Boselli, A. Buat, V. Burgarella, D. Castro-Rodriguez, N. Cava, A. Chanial, P. Clements, D. L. Conley, A. Conversi, L. Cooray, A. Dowell, C. D. Dwek, E. Dye, S. Eales, S. Elbaz, D. Farrah, D. Fox, M. Gear, W. Glenn, J. Solares, E. A. Gonzalez Griffin, M. Halpern, M. Hatziminaoglou, E. Huang, J. Ibar, E. Isaak, K. Ivison, R. J. Lagache, G. Levenson, L. Lu, N. Madden, S. Maffei, B. Mainetti, G. Mortier, A. M. J. Nguyen, H. T. O'Halloran, B. Oliver, S. J. Omont, A. Page, M. J. Panuzzo, P. Papageorgiou, A. Pearson, C. P. Perez-Fournon, I. Pohlen, M. Rawlings, J. I. Raymond, G. Rigopoulou, D. Rizzo, D. Rodighiero, G. Roseboom, I. G. Rowan-Robinson, M. Sanchez Portal, M. Schulz, B. Scott, D. Seymour, N. Shupe, D. L. Smith, A. J. Stevens, J. A. Symeonidis, M. Trichas, M. Tugwell, K. E. Valiante, E. Valtchanov, I. Vigroux, L. Wang, L. Ward, R. Wright, G. Xu, C. K. Zemcov, M. TI The HerMES SPIRE submillimeter local luminosity function SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: luminosity function, mass functions; galaxies: evolution; galaxies: statistics; submillimeter: galaxies ID DIGITAL SKY SURVEY; PHOTOMETRIC REDSHIFTS; INFRARED SURVEYS; STAR-FORMATION; GALAXIES; UNIVERSE; DISTRIBUTIONS; EVOLUTION; HISTORY; ENERGY AB Local luminosity functions are fundamental benchmarks for high-redshift galaxy formation and evolution studies as well as for models describing these processes. Determining the local luminosity function in the submillimeter range can help to better constrain in particular the bolometric luminosity density in the local Universe, and Herschel offers the first opportunity to do so in an unbiased way by imaging large sky areas at several submillimeter wavelengths. We present the first Herschel measurement of the submillimeter 0 < z < 0.2 local luminosity function and infrared bolometric (8-1000 mu m) local luminosity density based on SPIRE data from the HerMES Herschel key program over 14.7 deg(2). Flux measurements in the three SPIRE channels at 250, 350 and 500 mu m are combined with Spitzer photometry and archival data. We fit the observed optical-to-submillimeter spectral energy distribution of SPIRE sources and use the 1/V(max) estimator to provide the first constraints on the monochromatic 250, 350 and 500 mu m as well as on the infrared bolometric (8-1000 mu m) local luminosity function based on Herschel data. We compare our results with modeling predictions and find a slightly more abundant local submillimeter population than predicted by a number of models. Our measurement of the infrared bolometric (8-1000 mu m) local luminosity function suggests a flat slope at low luminosity, and the inferred local luminosity density, 1.31(-0.21)(+ 0.24) x 10(8) L(circle dot) Mpc(-3), is consistent with the range of values reported in recent literature. C1 [Vaccari, M.; Marchetti, L.; Franceschini, A.; Mainetti, G.; Rodighiero, G.] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy. [Altieri, B.; Amblard, A.; Conversi, L.; Sanchez Portal, M.; Valtchanov, I.] European Space Astron Ctr, Herschel Sci Ctr, Madrid 28691, Spain. [Amblard, A.; Cooray, A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Arumugam, V.; Ivison, R. J.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Auld, R.; Dye, S.; Eales, S.; Gear, W.; Isaak, K.; Papageorgiou, A.; Pohlen, M.; Raymond, G.] Cardiff Univ, Cardiff Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Aussel, H.; Elbaz, D.; Madden, S.; Panuzzo, P.] Univ Paris Diderot, CE Saclay, Lab AIM Paris Saclay, CEA DSM Irfu CNRS, F-91191 Gif Sur Yvette, France. [Babbedge, T.; Chanial, P.; Clements, D. L.; Fox, M.; Mortier, A. M. J.; O'Halloran, B.; Rizzo, D.; Rowan-Robinson, M.; Trichas, M.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England. [Lu, N.; Schulz, B.; Shupe, D. L.; Xu, C. K.] CALTECH, JPL, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Pearson, C. P.; Rigopoulou, D.] Rutherford Appleton Lab, Space Sci & Technol Dept, Didcot OX11 0QX, Oxon, England. [Pearson, C. P.] Univ Lethbridge, Inst Space Imaging Sci, Lethbridge, AB T1K 3M4, Canada. [Rigopoulou, D.] Univ Oxford, Oxford OX1 3RH, England. [Stevens, J. A.] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Page, M. J.; Rawlings, J. I.; Seymour, N.; Symeonidis, M.; Tugwell, K. E.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Omont, A.; Vigroux, L.] Univ Paris 06, CNRS, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France. [Maffei, B.] Univ Manchester, Sch Phys & Astron, Manchester M13 9PL, Lancs, England. [Lagache, G.] Univ Paris 11, IAS, F-91405 Orsay, France. [Lagache, G.] CNRS, UMR 8617, F-91405 Orsay, France. [Ibar, E.; Ivison, R. J.; Wright, G.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Huang, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hatziminaoglou, E.] ESO, D-85748 Garching, Germany. [Halpern, M.; Scott, D.; Valiante, E.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Solares, E. A. Gonzalez] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Farrah, D.; Griffin, M.; Oliver, S. J.; Roseboom, I. G.; Smith, A. J.; Wang, L.; Ward, R.] Univ Sussex, Ctr Astron, Dept Phys & Astron, Brighton BN1 9QH, E Sussex, England. [Bock, J.; Dowell, C. D.; Levenson, L.; Nguyen, H. T.; Zemcov, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Boselli, A.; Buat, V.; Burgarella, D.] Univ Aix marseille, OAMP, Lab Astrophys Marseille, F-13388 Marseille 13, France. [Castro-Rodriguez, N.; Cava, A.; Perez-Fournon, I.] Inst Astrofis Canarias, Tenerife 38200, Spain. [Castro-Rodriguez, N.; Cava, A.; Perez-Fournon, I.] Univ La Laguna, Dept Astrofis, Tenerife 38205, Spain. [Conley, A.; Glenn, J.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Dwek, E.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. RP Vaccari, M (reprint author), Univ Padua, Dipartimento Astron, Vicolo Osservatorio 3, I-35122 Padua, Italy. EM mattia@mattiavaccari.net RI Dwek, Eli/C-3995-2012; amblard, alexandre/L-7694-2014; Ivison, R./G-4450-2011; Vaccari, Mattia/R-3431-2016; Cava, Antonio/C-5274-2017; OI Seymour, Nicholas/0000-0003-3506-5536; Dye, Simon/0000-0002-1318-8343; Rodighiero, Giulia/0000-0002-9415-2296; amblard, alexandre/0000-0002-2212-5395; Ivison, R./0000-0001-5118-1313; Vaccari, Mattia/0000-0002-6748-0577; Cava, Antonio/0000-0002-4821-1275; Scott, Douglas/0000-0002-6878-9840; Marchetti, Lucia/0000-0003-3948-7621; Altieri, Bruno/0000-0003-3936-0284 FU University of Padova; ASI [I/005/07/0]; CSA (Canada); NAOC (China); CEA (France); CNES (France); CNRS (France); ASI (Italy); MCINN (Spain); Stockholm Observatory (Sweden); STFC (UK); NASA (USA) FX M. V. acknowledges support from a University of Padova "Herschel & ALMA" Fellowship and ASI "Herschel Science" Contract I/005/07/0. Micol Bolzonella kindly provided advice on the use of hyperz and Mattia Negrello swiftly produced additional predictions based on his models. SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); Stockholm Observatory (Sweden); STFC (UK); and NASA (USA). The data presented in this paper will be released through the Herschel Database in Marseille (HeDaM, http://hedam. oamp. fr/HerMES). NR 29 TC 35 Z9 35 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL-AUG PY 2010 VL 518 AR L20 DI 10.1051/0004-6361/201014694 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 646GQ UT WOS:000281527200021 ER PT J AU van der Tak, FFS Marseille, MG Herpin, F Wyrowski, F Baudry, A Bontemps, S Braine, J Doty, S Frieswijk, W Melnick, G Shipman, R van Dishoeck, EF Benz, AO Caselli, P Hogerheijde, M Johnstone, D Liseau, R Bachiller, R Benedettini, M Bergin, E Bjerkeli, P Blake, G Bruderer, S Cernicharo, J Codella, C Daniel, F di Giorgio, AM Dominik, C Encrenaz, P Fich, M Fuente, A Giannini, T Goicoechea, J de Graauw, T Helmich, F Herczeg, G Jorgensen, J Kristensen, L Larsson, B Lis, D McCoey, C Neufeld, D Nisini, B Olberg, M Parise, B Pearson, J Plume, R Risacher, C Santiago, J Saraceno, P Tafalla, M van Kempen, T Visser, R Wampfler, S Yildiz, U Ravera, L Roelfsema, P Siebertz, O Teyssier, D AF van der Tak, F. F. S. Marseille, M. G. Herpin, F. Wyrowski, F. Baudry, A. Bontemps, S. Braine, J. Doty, S. Frieswijk, W. Melnick, G. Shipman, R. van Dishoeck, E. F. Benz, A. O. Caselli, P. Hogerheijde, M. Johnstone, D. Liseau, R. Bachiller, R. Benedettini, M. Bergin, E. Bjerkeli, P. Blake, G. Bruderer, S. Cernicharo, J. Codella, C. Daniel, F. di Giorgio, A. M. Dominik, C. Encrenaz, P. Fich, M. Fuente, A. Giannini, T. Goicoechea, J. de Graauw, Th. Helmich, F. Herczeg, G. Jorgensen, J. Kristensen, L. Larsson, B. Lis, D. McCoey, C. Neufeld, D. Nisini, B. Olberg, M. Parise, B. Pearson, J. Plume, R. Risacher, C. Santiago, J. Saraceno, P. Tafalla, M. van Kempen, T. Visser, R. Wampfler, S. Yildiz, U. Ravera, L. Roelfsema, P. Siebertz, O. Teyssier, D. TI Water abundance variations around high-mass protostars: HIFI observations of the DR21 region SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: molecules; stars: formation; astrochemistry; ISM: individual objects: DR21 ID MONTE-CARLO METHOD; STAR-FORMATION; RADIATIVE-TRANSFER; LINE EMISSION; YOUNG STARS; CYGNUS-X; EXCITATION; EVOLUTION; H-2; ABSORPTION AB Context. Water is a key molecule in the star formation process, but its spatial distribution in star-forming regions is not well known. Aims. We study the distribution of dust continuum and H(2)O and (13)CO line emission in DR21, a luminous star-forming region with a powerful outflow and a compact H II region. Methods. Herschel-HIFI spectra near 1100 GHz show narrow (13)CO 10-9 emission and H(2)O 1(11)-0(00) absorption from the dense core and broad emission from the outflow in both lines. The H2O line also shows absorption by a foreground cloud known from ground-based observations of low-J CO lines. Results. The dust continuum emission is extended over 36 '' FWHM, while the (13)CO and H(2)O lines are confined to approximate to 24 '' or less. The foreground absorption appears to peak further North than the other components. Radiative transfer models indicate very low abundances of similar to 2 x 10(-10) for H(2)O and similar to 8 x 10(-7) for (13)CO in the dense core, and higher H(2)O abundances of similar to 4 x 10(-9) in the foreground cloud and similar to 7 x 10(-7) in the outflow. Conclusions. The high H(2)O abundance in the warm outflow is probably due to the evaporation of water-rich icy grain mantles, while the H(2)O abundance is kept down by freeze-out in the dense core and by photodissociation in the foreground cloud. C1 [van der Tak, F. F. S.; Marseille, M. G.; Shipman, R.; Helmich, F.; Risacher, C.; Roelfsema, P.] SRON Netherlands Inst Space Res, NL-9747 AD Groningen, Netherlands. [van der Tak, F. F. S.; Frieswijk, W.] Univ Groningen, Kapteyn Inst, NL-9700 AB Groningen, Netherlands. [Herpin, F.; Baudry, A.; Bontemps, S.; Braine, J.] Univ Groningen, Kapteyn Inst, NL-9700 AB Groningen, Netherlands. [Wyrowski, F.; Parise, B.] Max Planck Inst Radioastron, D-5300 Bonn, Germany. [van Dishoeck, E. F.; Hogerheijde, M.; Kristensen, L.; Visser, R.; Yildiz, U.] Leiden Univ, NL-2300 RA Leiden, Netherlands. [Parise, B.; Siebertz, O.] Univ Cologne, Inst Phys 1, KOSMA, D-5000 Cologne 41, Germany. [Ravera, L.] Univ Toulouse, CESR, Toulouse, France. [Liseau, R.; Bjerkeli, P.; Olberg, M.] Chalmers, S-41296 Gothenburg, Sweden. [Benz, A. O.; Bruderer, S.; Wampfler, S.] ETH, Inst Astron, CH-8093 Zurich, Switzerland. [de Graauw, Th.] Joint ALMA Observ, Santiago, Chile. [Teyssier, D.] ESA, European Space Astron Ctr, Madrid, Spain. [Melnick, G.; van Kempen, T.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. [Doty, S.] Denison Univ, Granville, OH 43023 USA. [van Dishoeck, E. F.; Herczeg, G.] MPI Extraterr Phys, Garching, Germany. [Caselli, P.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Johnstone, D.] Herzberg Inst Astrophys, Victoria, BC, Canada. [Johnstone, D.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8W 2Y2, Canada. [Bachiller, R.; Fuente, A.; Santiago, J.; Tafalla, M.] Observ Astron Nacl, Alcala De Henares, Spain. [Benedettini, M.; Codella, C.; di Giorgio, A. M.; Giannini, T.; Nisini, B.; Saraceno, P.] Ist Fis Spazio Interplanetario, INAF, Rome, Italy. [Bergin, E.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Blake, G.; Lis, D.] CALTECH, Pasadena, CA 91125 USA. [Cernicharo, J.; Daniel, F.; Goicoechea, J.] INTA CSIC, CAB, Torrejon De Ardoz, Spain. [Dominik, C.] Univ Amsterdam, NL-1012 WX Amsterdam, Netherlands. [Encrenaz, P.] Observ Paris, CNRS, LERMA, Paris, France. [Encrenaz, P.] Observ Paris, CNRS, UMR 8112, Paris, France. [Fich, M.; McCoey, C.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [Jorgensen, J.] U Copenhagen, Ctr Star & Planet Format, Copenhagen, Denmark. [Larsson, B.] Stockholm Univ, Dept Astron, Stockholm, Sweden. [Neufeld, D.] Johns Hopkins Univ, Baltimore, MD USA. [Pearson, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Plume, R.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Daniel, F.] Observ Paris, Meudon, France. RP van der Tak, FFS (reprint author), SRON Netherlands Inst Space Res, NL-9747 AD Groningen, Netherlands. EM vdtak@sron.nl RI Yildiz, Umut/C-5257-2011; Kristensen, Lars/F-4774-2011; Visser, Ruud/J-8574-2012; Jorgensen, Jes Kristian/L-7936-2014; Wampfler, Susanne/D-2270-2015; Fuente, Asuncion/G-1468-2016; OI Codella, Claudio/0000-0003-1514-3074; Giannini, Teresa/0000-0002-0224-096X; Yildiz, Umut/0000-0001-6197-2864; Kristensen, Lars/0000-0003-1159-3721; Jorgensen, Jes Kristian/0000-0001-9133-8047; Wampfler, Susanne/0000-0002-3151-7657; Fuente, Asuncion/0000-0001-6317-6343; Bjerkeli, Per/0000-0002-7993-4118; , Brunella Nisini/0000-0002-9190-0113 NR 30 TC 26 Z9 26 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL-AUG PY 2010 VL 518 AR L107 DI 10.1051/0004-6361/201014515 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 646GQ UT WOS:000281527200108 ER PT J AU van der Werf, PP Isaak, KG Meijerink, R Spaans, M Rykala, A Fulton, T Loenen, AF Walter, F Weiss, A Armus, L Fischer, J Israel, FP Harris, AI Veilleux, S Henkel, C Savini, G Lord, S Smith, HA Gonzalez-Alfonso, E Naylor, D Aalto, S Charmandaris, V Dasyra, KM Evans, A Gao, Y Greve, TR Gusten, R Kramer, C Martin-Pintado, J Mazzarella, J Papadopoulos, PP Sanders, DB Spinoglio, L Stacey, G Vlahakis, C Wiedner, MC Xilouris, EM AF van der Werf, P. P. Isaak, K. G. Meijerink, R. Spaans, M. Rykala, A. Fulton, T. Loenen, A. F. Walter, F. Weiss, A. Armus, L. Fischer, J. Israel, F. P. Harris, A. I. Veilleux, S. Henkel, C. Savini, G. Lord, S. Smith, H. A. Gonzalez-Alfonso, E. Naylor, D. Aalto, S. Charmandaris, V. Dasyra, K. M. Evans, A. Gao, Y. Greve, T. R. Guesten, R. Kramer, C. Martin-Pintado, J. Mazzarella, J. Papadopoulos, P. P. Sanders, D. B. Spinoglio, L. Stacey, G. Vlahakis, C. Wiedner, M. C. Xilouris, E. M. TI Black hole accretion and star formation as drivers of gas excitation and chemistry in Markarian 231 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: individual: Mrk 231; galaxies: active; galaxies: ISM; galaxies: nuclei; galaxies: starburst; infrared: galaxies ID GALAXY NUCLEI; DENSE GAS; DIAGNOSTICS; EMISSION; LINES; CO AB We present a full high resolution SPIRE FTS spectrum of the nearby ultraluminous infrared galaxy Mrk 231. In total 25 lines are detected, including CO J = 5-4 through J = 13-12, 7 rotational lines of H(2)O, 3 of OH(+) and one line each of H(2)O(+), CH(+), and HF. We find that the excitation of the CO rotational levels up to J = 8 can be accounted for by UV radiation from star formation. However, the approximately flat luminosity distribution of the CO lines over the rotational ladder above J = 8 requires the presence of a separate source of excitation for the highest CO lines. We explore X-ray heating by the accreting supermassive black hole in Mrk 231 as a source of excitation for these lines, and find that it can reproduce the observed luminosities. We also consider a model with dense gas in a strong UV radiation field to produce the highest CO lines, but find that this model strongly overpredicts the hot dust mass in Mrk 231. Our favoured model consists of a star forming disk of radius 560 pc, containing clumps of dense gas exposed to strong UV radiation, dominating the emission of CO lines up to J = 8. X-rays from the accreting supermassive black hole in Mrk 231 dominate the excitation and chemistry of the inner disk out to a radius of 160 pc, consistent with the X-ray power of the AGN in Mrk 231. The extraordinary luminosity of the OH(+) and H(2)O(+) lines reveals the signature of X-ray driven excitation and chemistry in this region. C1 [van der Werf, P. P.; Meijerink, R.; Loenen, A. F.; Israel, F. P.; Vlahakis, C.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Isaak, K. G.; Rykala, A.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Isaak, K. G.] Estec, ESA Astrophys Missions Div, NL-2200 AG Noordwijk, Netherlands. [Spaans, M.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Fulton, T.] Blue Sky Spect, Lethbridge, AB, Canada. [Walter, F.; Greve, T. R.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Weiss, A.; Henkel, C.; Guesten, R.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Armus, L.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Fischer, J.] USN, Res Lab, Remote Sensing Div, Washington, DC 20375 USA. [Harris, A. I.; Veilleux, S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Savini, G.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Lord, S.; Mazzarella, J.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Smith, H. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gonzalez-Alfonso, E.] Univ Alcala de Henares, Dept Fis, Madrid 28871, Spain. [Naylor, D.] Univ Lethbridge, Dept Phys, Lethbridge, AB T1J 1B1, Canada. [Aalto, S.] Chalmers, Onsala Observ, Dept Radio & Space Sci, S-43992 Onsala, Sweden. [Charmandaris, V.] Univ Crete, Dept Phys, Iraklion 71003, Greece. [Dasyra, K. M.] CEA Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France. [Evans, A.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Evans, A.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Gao, Y.] Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Peoples R China. [Greve, T. R.] Univ Copenhagen, Dark Cosmol Ctr, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Kramer, C.] IRAM, E-18012 Granada, Spain. [Martin-Pintado, J.] CSIC, Dept Astrofis Mol & Infrarroja, Inst Estruct Mat, E-28006 Madrid, Spain. [Papadopoulos, P. P.] Argelander Inst Astron, D-53121 Bonn, Germany. [Sanders, D. B.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Spinoglio, L.] CNR, Ist Fis Spazio Interplanetario, I-00133 Rome, Italy. [Stacey, G.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Wiedner, M. C.] LERMA, Observ Paris, F-75014 Paris, France. [Xilouris, E. M.] Natl Observ Athens, Inst Astron & Astrophys, Athens 15236, Greece. RP van der Werf, PP (reprint author), Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. EM pvdwerf@strw.leidenuniv.nl RI Charmandaris, Vassilis/A-7196-2008; Xilouris, Emmanuel/K-9459-2013; Martin-Pintado, Jesus/H-6107-2015; OI Charmandaris, Vassilis/0000-0002-2688-1956; Martin-Pintado, Jesus/0000-0003-4561-3508; Meijerink, Rowin/0000-0001-7584-9293; Dasyra, Kalliopi/0000-0002-1482-2203; Mazzarella, Joseph/0000-0002-8204-8619; Spinoglio, Luigi/0000-0001-8840-1551; Savini, Giorgio/0000-0003-4449-9416 FU DNRF; CSA in Canada; NAOC in China; CNES; CNRS; CEA in France; ASI in Italy; MEC in Spain; Stockholm Observatory in Sweden; STFC in the UK; NASA in the USA; ESA FX We thank Ewine van Dishoeck, Xander Tielens, and Thomas Nikola for useful discussions. We especially thank Ed Polehampton, Peter Imhof-Davies and Bruce Swinyard for their help with the FTS data processing. JF thanks MPE for its hospitality. The Dark Cosmology Centre is funded by the DNRF. The following institutes have provided hardware and software elements to the SPIRE project: University of Lethbridge, Canada; NAOC, Beijing, China; CEA Saclay, CEA Grenoble and LAM in France; IFSI, Rome, and University of Padua, Italy; IAC, Tenerife, Spain; Stockholm Observatory, Sweden; Cardiff University, Imperial College London, UCL-MSSL, STFC-RAL, UK ATC Edinburgh, and the University of Sussex in the UK. Funding for SPIRE has been provided by the national agencies of the participating countries and by internal institute funding: CSA in Canada; NAOC in China; CNES, CNRS, and CEA in France; ASI in Italy; MEC in Spain; Stockholm Observatory in Sweden; STFC in the UK; and NASA in the USA. Additional funding support for some instrument activities has been provided by ESA. NR 21 TC 152 Z9 152 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 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL-AUG PY 2010 VL 518 AR L42 DI 10.1051/0004-6361/201014682 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 646GQ UT WOS:000281527200043 ER PT J AU van Kempen, TA Green, JD Evans, NJ van Dishoeck, EF Kristensen, LE Herczeg, GJ Merin, B Lee, JE Jorgensen, JK Bouwman, J Acke, B Adamkovics, M Augereau, JC Bergin, E Blake, GA Brown, JM Carr, JS Chen, JH Cieza, L Dominik, C Dullemond, CP Dunham, MM Glassgold, A Gudel, M Harvey, PM Henning, T Hogerheijde, MR Jaffe, D Kim, HJ Knez, C Lacy, JH Maret, S Meeus, G Meijerink, R Mulders, GD Mundy, L Najita, J Olofsson, J Pontoppidan, KM Salyk, C Sturm, B Visser, R Waters, LBFM Waelkens, C Yildiz, UA AF van Kempen, T. A. Green, J. D. Evans, N. J., II van Dishoeck, E. F. Kristensen, L. E. Herczeg, G. J. Merin, B. Lee, J. -E. Jorgensen, J. K. Bouwman, J. Acke, B. Adamkovics, M. Augereau, J. C. Bergin, E. Blake, G. A. Brown, J. M. Carr, J. S. Chen, J. -H. Cieza, L. Dominik, C. Dullemond, C. P. Dunham, M. M. Glassgold, A. Guedel, M. Harvey, P. M. Henning, Th. Hogerheijde, M. R. Jaffe, D. Kim, H. J. Knez, C. Lacy, J. H. Maret, S. Meeus, G. Meijerink, R. Mulders, G. D. Mundy, L. Najita, J. Olofsson, J. Pontoppidan, K. M. Salyk, C. Sturm, B. Visser, R. Waters, L. B. F. M. Waelkens, C. Yildiz, U. A. TI Dust, Ice, and Gas In Time (DIGIT) Herschel program first results A full PACS-SED scan of the gas line emission in protostar DK Chamaeleontis SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE astrochemistry; circumstellar matter; stars: formation; stars: protostars; infrared: ISM; submillimeter: ISM ID YOUNG STELLAR OBJECTS; SPITZER C2D SURVEY; ISO-LWS OBSERVATIONS; INTERSTELLAR CLOUDS; HERBIG AE; POPULATION; NEARBY; STAR; SPECTROSCOPY; OUTFLOW AB Aims. We aim to study the composition and energetics of the circumstellar material of DK Cha, an intermediate-mass star in transition from an embedded configuration to a star plus disk stage, during this pivotal stage of its evolution. Methods. Using the range scan mode of PACS on the Herschel Space Observatory, we obtained a spectrum of DK Cha from 55 to 210 mu m as part of the DIGIT key program. Results. Almost 50 molecular and atomic lines were detected, many more than the 7 lines detected in ISO-LWS. Nearly the entire ladder of CO from J = 14-13 to 38-37 (E(u)/k = 4080 K), water from levels as excited as J(K-1K+1) = 7(07) (E(u)/k = 843 K), and OH lines up to E(u)/k = 290 K were detected. Conclusions. The continuum emission in our PACS SED scan matches the flux expected by a model consisting of a star, a surrounding disk of 0.03 M(circle dot), and an envelope of a similar mass, supporting the suggestion that the object is emerging from its main accretion stage. Molecular, atomic, and ionic emission lines in the far-infrared reveal the outflow's influence on the envelope. The inferred hot gas may be photon-heated, but some emission may be caused by C-shocks in the walls of the outflow cavity. C1 [van Kempen, T. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Green, J. D.; Evans, N. J., II; Chen, J. -H.; Dunham, M. M.; Harvey, P. M.; Jaffe, D.; Kim, H. J.; Lacy, J. H.; Salyk, C.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [van Dishoeck, E. F.; Kristensen, L. E.; Hogerheijde, M. R.; Meijerink, R.; Visser, R.; Yildiz, U. A.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [van Dishoeck, E. F.; Herczeg, G. J.; Brown, J. M.] Max Planck Inst Extraterr Phys, Garching, Germany. [Merin, B.] European Space Astron Ctr ESA, Herschel Sci Ctr, Villanueva De La Canada 28691, Madrid, Spain. [Lee, J. -E.] Sejong Univ, Astrophys Res Ctr Struct & Evolut Cosmos, Dept Astron & Space Sci, Seoul 143747, South Korea. [Jorgensen, J. K.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen K, Denmark. [Bouwman, J.; Dullemond, C. P.; Henning, Th.; Olofsson, J.; Sturm, B.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Acke, B.; Waters, L. B. F. M.; Waelkens, C.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium. [Adamkovics, M.; Glassgold, A.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Augereau, J. C.; Maret, S.] Univ Grenoble 1, CNRS, Lab Astrophys Grenoble, UMR5571, F-38041 Grenoble 9, France. [Bergin, E.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Blake, G. A.; Pontoppidan, K. M.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Carr, J. S.] USN, Res Lab, Washington, DC 20375 USA. [Cieza, L.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Dominik, C.; Mulders, G. D.; Waters, L. B. F. M.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands. [Dominik, C.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands. [Dullemond, C. P.] Univ Heidelberg, Inst Theoret Astrophys, D-69120 Heidelberg, Germany. [Guedel, M.] Univ Vienna, Dept Astron, A-1180 Vienna, Austria. [Knez, C.; Mundy, L.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Meeus, G.] Univ Autonoma Madrid, Fac Ciencias, Dpt Fis Teor, E-28049 Madrid, Spain. [Mulders, G. D.] Univ Groningen, SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [Najita, J.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Acke, B.] Fund Sci Res, Flanders, Belgium. RP van Kempen, TA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 78, Cambridge, MA 02138 USA. EM tvankempen@cfa.harvard.edu RI Visser, Ruud/J-8574-2012; Lee , Jeong-Eun/E-2387-2013; Jorgensen, Jes Kristian/L-7936-2014; Guedel, Manuel/C-8486-2015; Yildiz, Umut/C-5257-2011; Kristensen, Lars/F-4774-2011 OI Jorgensen, Jes Kristian/0000-0001-9133-8047; Guedel, Manuel/0000-0001-9818-0588; Merin, Bruno/0000-0002-8555-3012; Maret, Sebastien/0000-0003-1104-4554; Yildiz, Umut/0000-0001-6197-2864; Kristensen, Lars/0000-0003-1159-3721 FU NASA 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. The authors would like to thank Bart VandenBussche and Alessandra Contursi for help with the data reduction, and David Ardila for his help in scheduling the observations prior to the ESAC SDP workshop. NR 26 TC 33 Z9 33 U1 0 U2 5 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL-AUG PY 2010 VL 518 AR L128 DI 10.1051/0004-6361/201014686 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 646GQ UT WOS:000281527200129 ER PT J AU van Kempen, TA Kristensen, LE Herczeg, GJ Visser, R van Dishoeck, EF Wampfler, SF Bruderer, S Benz, AO Doty, SD Brinch, C Hogerheijde, MR Jorgensen, JK Tafalla, M Neufeld, D Bachiller, R Baudry, A Benedettini, M Bergin, EA Bjerkeli, P Blake, GA Bontemps, S Braine, J Caselli, P Cernicharo, J Codella, C Daniel, F di Giorgio, AM Dominik, C Encrenaz, P Fich, M Fuente, A Giannini, T Goicoechea, JR de Graauw, T Helmich, F Herpin, F Jacq, T Johnstone, D Kaufman, MJ Larsson, B Lis, D Liseau, R Marseille, M McCoey, C Melnick, G Nisini, B Olberg, M Parise, B Pearson, JC Plume, R Risacher, C Santiago-Garcia, J Saraceno, P Shipman, R van der Tak, F Wyrowski, F Yildiz, UA Ciechanowicz, M Dubbeldam, L Glenz, S Huisman, R Lin, RH Morris, P Murphy, JA Trappe, N AF van Kempen, T. A. Kristensen, L. E. Herczeg, G. J. Visser, R. van Dishoeck, E. F. Wampfler, S. F. Bruderer, S. Benz, A. O. Doty, S. D. Brinch, C. Hogerheijde, M. R. Jorgensen, J. K. Tafalla, M. Neufeld, D. Bachiller, R. Baudry, A. Benedettini, M. Bergin, E. A. Bjerkeli, P. Blake, G. A. Bontemps, S. Braine, J. Caselli, P. Cernicharo, J. Codella, C. Daniel, F. di Giorgio, A. M. Dominik, C. Encrenaz, P. Fich, M. Fuente, A. Giannini, T. Goicoechea, J. R. de Graauw, Th. Helmich, F. Herpin, F. Jacq, T. Johnstone, D. Kaufman, M. J. Larsson, B. Lis, D. Liseau, R. Marseille, M. McCoey, C. Melnick, G. Nisini, B. Olberg, M. Parise, B. Pearson, J. C. Plume, R. Risacher, C. Santiago-Garcia, J. Saraceno, P. Shipman, R. van der Tak, F. Wyrowski, F. Yildiz, U. A. Ciechanowicz, M. Dubbeldam, L. Glenz, S. Huisman, R. Lin, R. H. Morris, P. Murphy, J. A. Trappe, N. TI Origin of the hot gas in low-mass protostars Herschel-PACS spectroscopy of HH 46 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE astrochemistry; stars: formation; ISM: molecules; ISM: jets and outflows; ISM: individual objects: HH 46 ID EMISSION; WATER; SHOCK; HH-46/47; OUTFLOW; JETS; I. AB Aims. "Water In Star-forming regions with Herschel" (WISH) is a Herschel key programme aimed at understanding the physical and chemical structure of young stellar objects (YSOs) with a focus on water and related species. Methods. The low-mass protostar HH 46 was observed with the Photodetector Array Camera and Spectrometer (PACS) on the Herschel Space Observatory to measure emission in H(2)O, CO, OH, [O I], and [C II] lines located between 63 and 186 mu m. The excitation and spatial distribution of emission can disentangle the different heating mechanisms of YSOs, with better spatial resolution and sensitivity than previously possible. Results. Far-IR line emission is detected at the position of the protostar and along the outflow axis. The OH emission is concentrated at the central position, CO emission is bright at the central position and along the outflow, and H(2)O emission is concentrated in the outflow. In addition, [O I] emission is seen in low-velocity gas, assumed to be related to the envelope, and is also seen shifted up to 170 km s(-1) in both the red-and blue-shifted jets. Envelope models are constructed based on previous observational constraints. They indicate that passive heating of a spherical envelope by the protostellar luminosity cannot explain the high-excitation molecular gas detected with PACS, including CO lines with upper levels at >2500 K above the ground state. Instead, warm CO and H(2)O emission is probably produced in the walls of an outflow-carved cavity in the envelope, which are heated by UV photons and non-dissociative C-type shocks. The bright OH and [O I] emission is attributed to J-type shocks in dense gas close to the protostar. In the scenario described here, the combined cooling by far-IR lines within the central spatial pixel is estimated to be 2 x 10(-2) L(circle dot), with 60-80% attributed to J- and C-type shocks produced by interactions between the jet and the envelope. C1 [van Kempen, T. A.; Kristensen, L. E.; Visser, R.; van Dishoeck, E. F.; Brinch, C.; Hogerheijde, M. R.; Yildiz, U. A.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [van Kempen, T. A.; Melnick, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Herczeg, G. J.; van Dishoeck, E. F.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Wampfler, S. F.; Bruderer, S.; Benz, A. O.] ETH, Inst Astron, CH-8093 Zurich, Switzerland. [Doty, S. D.] Denison Univ, Dept Phys & Astron, Granville, OH 43023 USA. [Jorgensen, J. K.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen K, Denmark. [Tafalla, M.; Bachiller, R.] Observ Astron Nacl IGN, Madrid 28014, Spain. [Neufeld, D.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Baudry, A.; Bontemps, S.; Braine, J.; Herpin, F.; Jacq, T.] Univ Bordeaux, Lab Astrophys Bordeaux, Floirac, France. [Baudry, A.; Bontemps, S.; Braine, J.; Herpin, F.; Jacq, T.] CNRS INSU, UMR 5804, Floirac, France. [Benedettini, M.; di Giorgio, A. M.; Saraceno, P.] INAF Inst Fis Spazio Interplanetario, Area Ric Tor Vergata, I-00133 Rome, Italy. [Bergin, E. A.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Bjerkeli, P.; Liseau, R.; Olberg, M.] Chalmers, Onsala Space Observ, Dept Radio & Space Sci, S-43992 Onsala, Sweden. [Blake, G. A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Caselli, P.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Caselli, P.; Codella, C.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Cernicharo, J.; Daniel, F.; Goicoechea, J. R.] CSIC INTA, Dept Astrofis, Ctr Astrobiol, Madrid 28850, Spain. [Dominik, C.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. [Dominik, C.] Radboud Univ Nijmegen, Dept Astrophys, IMAPP, NL-6500 GL Nijmegen, Netherlands. [Encrenaz, P.] Observ Paris, CNRS, LERMA, F-75014 Paris, France. [Encrenaz, P.] Observ Paris, CNRS, UMR 8112, F-75014 Paris, France. [Fich, M.; McCoey, C.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [Fuente, A.] Observ Astron Nacl, Alcala De Henares 28803, Spain. [Giannini, T.; Nisini, B.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy. [de Graauw, Th.; Helmich, F.; Marseille, M.; Risacher, C.; Shipman, R.; van der Tak, F.; Dubbeldam, L.; Huisman, R.] SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [Johnstone, D.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Johnstone, D.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 1A1, Canada. [Kaufman, M. J.] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA. [Larsson, B.] Stockholm Univ, Dept Astron, S-10691 Stockholm, Sweden. [Lis, D.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Parise, B.; Wyrowski, F.; Ciechanowicz, M.; Lin, R. H.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Pearson, J. C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Plume, R.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Santiago-Garcia, J.] Inst RadioAstron Milimetr, E-18012 Granada, Spain. [van der Tak, F.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Glenz, S.] Univ Cologne, Inst Phys 1, KOSMA, D-50937 Cologne, Germany. [Murphy, J. A.; Trappe, N.] Natl Univ Ireland, Expt Phys Dept, Maynooth, Kildare, Ireland. RP van Kempen, TA (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. EM kristensen@strw.leidenuniv.nl RI Yildiz, Umut/C-5257-2011; Kristensen, Lars/F-4774-2011; Visser, Ruud/J-8574-2012; Jorgensen, Jes Kristian/L-7936-2014; Wampfler, Susanne/D-2270-2015; Brinch, Christian/G-5157-2015; Trappe, Neil/C-9014-2016; Fuente, Asuncion/G-1468-2016; OI Yildiz, Umut/0000-0001-6197-2864; Kristensen, Lars/0000-0003-1159-3721; Jorgensen, Jes Kristian/0000-0001-9133-8047; Wampfler, Susanne/0000-0002-3151-7657; Brinch, Christian/0000-0002-5074-7183; Trappe, Neil/0000-0003-2527-9821; Fuente, Asuncion/0000-0001-6317-6343; Bjerkeli, Per/0000-0002-7993-4118; Codella, Claudio/0000-0003-1514-3074; Giannini, Teresa/0000-0002-0224-096X; , Brunella Nisini/0000-0002-9190-0113 NR 25 TC 70 Z9 70 U1 0 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL-AUG PY 2010 VL 518 AR L121 DI 10.1051/0004-6361/201014615 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 646GQ UT WOS:000281527200122 ER PT J AU Zavagno, A Anderson, LD Russeil, D Morgan, L Stringfellow, GS Deharveng, L Rodon, JA Robitaille, TP Mottram, JC Schuller, F Testi, L Billot, N Molinari, S di Gorgio, A Kirk, JM Brunt, C Ward-Thompson, D Traficante, A Veneziani, M Faustini, F Calzoletti, L AF Zavagno, A. Anderson, L. D. Russeil, D. Morgan, L. Stringfellow, G. S. Deharveng, L. Rodon, J. A. Robitaille, T. P. Mottram, J. C. Schuller, F. Testi, L. Billot, N. Molinari, S. di Gorgio, A. Kirk, J. M. Brunt, C. Ward-Thompson, D. Traficante, A. Veneziani, M. Faustini, F. Calzoletti, L. TI Star formation triggered by H II regions in our Galaxy First results for N49 from the Herschel infrared survey of the Galactic plane SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: formation; H II regions; infrared: general ID GLIMPSE SURVEY; HII-REGIONS; CANDIDATES; COLLECT; BORDERS; BUBBLES; OBJECTS AB Context. It has been shown that by means of different physical mechanisms the expansion of H II regions can trigger the formation of new stars of all masses. This process may be important to the formation of massive stars but has never been quantified in the Galaxy. Aims. We use Herschel-PACS and -SPIRE images from the Herschel infrared survey of the Galactic plane, Hi-GAL, to perform this study. Methods. We combine the Spitzer-GLIMPSE and -MIPSGAL, radio-continuum and submillimeter surveys such as ATLASGAL with Hi-GAL to study young stellar objects (YSOs) observed towards Galactic H II regions. We select a representative H II region, N49, located in the field centered on l = 30 degrees observed as part of the Hi-GAL science demonstration phase, to demonstrate the importance Hi-GAL will have to this field of research. Results. Hi-GAL PACS and SPIRE images reveal a new population of embedded young stars, coincident with bright ATLASGAL condensations. The Hi-GAL images also allow us, for the first time, to constrain the physical properties of the newly formed stars by means of fits to their spectral energy distribution. Massive young stellar objects are observed at the borders of the N49 region and represent second generation massive stars whose formation has been triggered by the expansion of the ionized region. Conclusions. The first Hi-GAL images obtained using PACS and SPIRE have demonstrated the capability to investigate star formation triggered by H II regions. With radio, submillimeter, and shorter wavelength infrared data from other surveys, the Hi-GAL images reveal young massive star-forming clumps surrounding the perimeter of the N49 H II generated bubble. Hi-GAL enables us to detect a population of young stars at different evolutionary stages, cold condensations only being detected in the SPIRE wavelength range. The far IR coverage of Hi-GAL strongly constrains the physical properties of the YSOs. The large and unbiased spatial coverage of this survey offers us a unique opportunity to lead, for the first time, a global study of star formation triggered by H II regions in our Galaxy. C1 [Zavagno, A.; Anderson, L. D.; Russeil, D.; Deharveng, L.; Rodon, J. A.] CNRS, UMR 6110, Lab Astrophys Marseille, F-13388 Marseille 13, France. [Zavagno, A.; Anderson, L. D.; Russeil, D.; Deharveng, L.; Rodon, J. A.] Univ Aix Marseille 1, F-13388 Marseille 13, France. [Morgan, L.] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England. [Stringfellow, G. S.] UCB Boulder Colorado, Ctr Astrophys & Space Astron, Dept Astrophys & Planetary Sci 389, Boulder, CO USA. [Robitaille, T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Mottram, J. C.; Brunt, C.] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England. [Schuller, F.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Testi, L.] ESO, D-85748 Garching, Germany. [Billot, N.] CALTECH, IPAC, NASA Herschel Sci Ctr, Pasadena, CA 91125 USA. [Molinari, S.; di Gorgio, A.] INAF IFSI, I-00133 Rome, Italy. [Kirk, J. M.; Ward-Thompson, D.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Traficante, A.; Veneziani, M.] Univ Roma Tor Vergata, Dipartimento Fis, I-00173 Rome, Italy. [Faustini, F.; Calzoletti, L.] ASI Sci Data Ctr, I-00044 Frascati, Rome, Italy. RP Zavagno, A (reprint author), CNRS, UMR 6110, Lab Astrophys Marseille, 38 Rue E Joliot Curie, F-13388 Marseille 13, France. EM annie.zavagno@oamp.fr RI Molinari, Sergio/O-4095-2016; OI Molinari, Sergio/0000-0002-9826-7525; Robitaille, Thomas/0000-0002-8642-1329 FU ANR (Agence Nationale pour la Recherche) [ANR-08-BLAN-0241] FX Part of this work was supported by the ANR (Agence Nationale pour la Recherche) project "PROBeS", number ANR-08-BLAN-0241 (LA). NR 25 TC 42 Z9 42 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 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL-AUG PY 2010 VL 518 AR L101 DI 10.1051/0004-6361/201014587 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 646GQ UT WOS:000281527200102 ER EF