FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Kuntner, M Kralj-Fiser, S Gregoric, M AF Kuntner, Matjaz Kralj-Fiser, Simona Gregoric, Matjaz TI Ladder webs in orb-web spiders: ontogenetic and evolutionary patterns in Nephilidae SO BIOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE Araneae; Araneoidea; Clitaetra; Herennia; hub displacement; ladder index; Nephilengys; Nephila; architecture; web allometry ID ARANEAE-THERIDIIDAE; BUILDING SPIDERS; CLAVIPES ARANEAE; PREY-CAPTURE; MECHANICAL-PROPERTIES; CONVERGENT EVOLUTION; PHILOPONELLA-VICINA; ADAPTIVE RADIATION; WEAVING SPIDERS; SILK AB Spider web research bridges ethology, ecology, functional morphology, material science, development, genetics, and evolution. Recent work proposes the aerial orb web as a one-time key evolutionary innovation that has freed spider-web architecture from substrate constraints. However, the orb has repeatedly been modified or lost within araneoid spiders. Modifications include not only sheet- and cobwebs, but also ladder webs, which secondarily utilize the substrate. A recent nephilid species level phylogeny suggests that the ancestral nephilid web architecture was an arboricolous ladder and that round aerial webs were derived. Because the web biology of the basalmost Clitaetra and the derived Nephila are well understood, the present study focuses on the webs of the two phylogenetically intervening genera, Herennia and Nephilengys, to establish ontogenetic and macroevolutionary patterns across the nephilid tree. We compared juvenile and adult webs of 95 Herennia multipuncta and 143 Nephilengys malabarensis for two measures of ontogenetic allometric web changes: web asymmetry quantified by the ladder index, and hub asymmetry quantified by the hub displacement index. We define a 'ladder web' as a vertically elongated orb exceeding twice the length over width (ladder index >= 2) and possessing (sub)parallel rather than round side frames. Webs in both genera allometrically grew from orbs to ladders, more so in Herennia. Such allometric web growth enables the spider to maintain its arboricolous web site. Unexpectedly, hub asymmetry only increased significantly in heavy-bodied Nephilengys females, and not in Herennia, challenging the commonly invoked gravity hypothesis. The findings obtained in the present study support the intrageneric uniformness of nephilid webs, with Herennia etruscilla webs being identical to H. multipuncta. The nephilid web evolution suggests that the ancestor of Nephila reinvented the aerial orb web because the orb arises at a much more inclusive phylogenetic level, and all intervening nephilids retained the secondarily acquired substrate-dependent ladder web. (C) 2010 The Linnean Society of London, Biological Journal of the Linnean Society, 2010, 99, 849-866. C1 [Kuntner, Matjaz; Kralj-Fiser, Simona; Gregoric, Matjaz] Slovenian Acad Sci & Arts, Ctr Sci Res, Inst Biol, SI-1001 Ljubljana, Slovenia. [Kuntner, Matjaz] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. RP Kuntner, M (reprint author), Slovenian Acad Sci & Arts, Ctr Sci Res, Inst Biol, Novi Trg 2,POB 306, SI-1001 Ljubljana, Slovenia. EM kuntner@gmail.com FU European Community Sixth Framework Programme [MIRG-CT-2005 036536]; Slovenian Research Agency [Z1-7082-0618]; National University of Singapore FX We thank D. Li, D. Court, C. Koh, J. Woon, L. Yap, E. Tan, J. Koh, and P. Ng for field and/or logistical help, and three anonymous reviewers for their suggestions on how to improve the manuscript. This work was funded by the grants to MK from the European Community Sixth Framework Programme (a Marie Curie International Reintegration Grant MIRG-CT-2005 036536), the Slovenian Research Agency (grant Z1-7082-0618) and the National University of Singapore (Raffles Museum Fellowship). NR 79 TC 23 Z9 27 U1 1 U2 17 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0024-4066 J9 BIOL J LINN SOC JI Biol. J. Linnean Soc. PD APR PY 2010 VL 99 IS 4 BP 849 EP 866 PG 18 WC Evolutionary Biology SC Evolutionary Biology GA 576SH UT WOS:000276168100017 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 Stomatolepas Barnacle Species (Cirripedia: Balanomorpha: Coronuloidea) from Leatherback Sea Turtles SO BULLETIN OF THE PEABODY MUSEUM OF NATURAL HISTORY LA English DT Article DE Dermochelys coriacea; epibionts; leatherback sea turtle; new species ID COMMENSAL AB A new species of the commensal barnacle genus Stomatolepas has been collected from leatherback turtles in the southern Atlantic Ocean. It is described here as S. pilsbryi n. sp. and compared to its congeners S. elegans (Costa, 1838) and S. praegustator Pilsbry, 1910. A neotype is also designated for S. elegans. C1 [Frick, Michael G.] Smithsonian Natl Zool Pk, Friends Natl Zoo, Washington, DC 20013 USA. [Zardus, John D.] 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; zardusj1@citadel.edu; eric.lazo-wasem@yale.edu NR 15 TC 10 Z9 10 U1 2 U2 5 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 J9 B PEABODY MUS NAT HI JI Bull. Peabody Mus. Natl. Hist. PD APR PY 2010 VL 51 IS 1 BP 123 EP 136 DI 10.3374/014.051.0102 PG 14 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 591AE UT WOS:000277269100003 ER PT J AU Ponssa, ML Heyer, WR de Sa, R AF Laura Ponssa, Maria Heyer, W. Ronald de Sa, Rafael TI Phylogeny of the genus Leptodactylus (Anura, Leptodactylidae) based on characters of morphology and mode of life SO CLADISTICS LA English DT Meeting Abstract CT 27th Annual Meeting of the Willi-Hennig-Society/8th Argentina Meeting of Cladistics and Biogeography CY OCT 28-31, 2008 CL San Javier, ARGENTINA SP Willi Hennig Soc C1 [Laura Ponssa, Maria] Consejo Nacl Invest Cient & Tecn, Fdn Miguel Lillo, Inst Herpetol, RA-1033 Buenos Aires, DF, Argentina. [de Sa, Rafael] Univ Richmond, Dept Biol, Richmond, VA 23173 USA. [Heyer, W. Ronald] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 1 U2 3 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0748-3007 J9 CLADISTICS JI Cladistics PD APR PY 2010 VL 26 IS 2 BP 222 EP 222 PG 1 WC Evolutionary Biology SC Evolutionary Biology GA 564LD UT WOS:000275214800086 ER PT J AU Ramirez, MJ Maddison, W Coddington, JA AF Ramirez, Martin J. Maddison, Wayne Coddington, Jonathan A. TI Use of ontologies to document characters SO CLADISTICS LA English DT Meeting Abstract CT 27th Annual Meeting of the Willi-Hennig-Society/8th Argentina Meeting of Cladistics and Biogeography CY OCT 28-31, 2008 CL San Javier, ARGENTINA SP Willi Hennig Soc C1 [Ramirez, Martin J.] Consejo Nacl Invest Cient & Tecn, Museo Argentino Ciencias Nat Bernardino Rivadavia, RA-1033 Buenos Aires, DF, Argentina. [Maddison, Wayne] Univ British Columbia, Dept Zool, Vancouver, BC V6T 1Z4, Canada. [Coddington, Jonathan A.] Smithsonian Inst, Washington, DC 20013 USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0748-3007 J9 CLADISTICS JI Cladistics PD APR PY 2010 VL 26 IS 2 BP 223 EP 223 PG 1 WC Evolutionary Biology SC Evolutionary Biology GA 564LD UT WOS:000275214800088 ER PT J AU Laurance, WF Koh, LP Butler, R Sodhi, NS Bradshaw, CJA Neidel, JD Consunji, H Vega, JM AF Laurance, William F. Koh, Lian P. Butler, Rhett Sodhi, Navjot S. Bradshaw, Corey J. A. Neidel, J. David Consunji, Hazel Mateo Vega, Javier TI Improving the Performance of the Roundtable on Sustainable Palm Oil for Nature Conservation SO CONSERVATION BIOLOGY LA English DT Article ID BIODIVERSITY; DEFORESTATION; CLIMATE C1 [Laurance, William F.] James Cook Univ, Sch Marine & Trop Biol, Cairns, Qld 4870, Australia. [Laurance, William F.; Mateo Vega, Javier] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Koh, Lian P.] ETH, Inst Terr Ecosyst, CHN G 74 2, CH-8092 Zurich, Switzerland. [Butler, Rhett] Mongabay Com, Menlo Pk, CA 94026 USA. [Sodhi, Navjot S.; Neidel, J. David; Consunji, Hazel] Natl Univ Singapore, Dept Biol Sci, Singapore 117543, Singapore. [Bradshaw, Corey J. A.] Univ Adelaide, Inst Environm, Adelaide, SA 5005, Australia. [Bradshaw, Corey J. A.] Univ Adelaide, Sch Earth & Environm Sci, Adelaide, SA 5005, Australia. [Bradshaw, Corey J. A.] S Australian Res & Dev Inst, Henley Beach, SA 5022, Australia. [Neidel, J. David; Consunji, Hazel; Mateo Vega, Javier] Yale Univ, Sch Forestry & Environm Studies, Environm Leadership & Training Initiat, New Haven, CT 06511 USA. RP Laurance, WF (reprint author), James Cook Univ, Sch Marine & Trop Biol, Cairns, Qld 4870, Australia. EM bill.laurance@jcu.edu.au RI Bradshaw, Corey/A-1311-2008; Koh, Lian Pin/A-5794-2010; Laurance, William/B-2709-2012 OI Bradshaw, Corey/0000-0002-5328-7741; Koh, Lian Pin/0000-0001-8152-3871; FU Environmental Leadership and Training Initiative (ELTI); ETH Fellowship; Swiss National Science Foundation FX This paper was stimulated by a multistakeholder conference on oil palm and biofuels in Singapore (May 2009) sponsored by the Environmental Leadership and Training Initiative (ELTI), a cooperative venture of the Yale School of Forestry and Environmental Studies and the Smithsonian Tropical Research Institute. L. P. K. was supported by an ETH Fellowship and the Swiss National Science Foundation. We thank A. Rante, D. Gilbert, and E. Pumomo for use of photographs and T. Gardner, R. Ewers, WWF-International, and three anonymous referees for helpful comments on the manuscript. NR 22 TC 53 Z9 54 U1 5 U2 60 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0888-8892 J9 CONSERV BIOL JI Conserv. Biol. PD APR PY 2010 VL 24 IS 2 BP 377 EP 381 DI 10.1111/j.1523-1739.2010.01448.x PG 5 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 572ZM UT WOS:000275877600007 PM 20184655 ER PT J AU Boyer, AG AF Boyer, Alison G. TI Consistent Ecological Selectivity through Time in Pacific Island Avian Extinctions SO CONSERVATION BIOLOGY LA English DT Article DE body size; conservation paleobiology; decision tree; extinction risk; fossil birds; Red List ID NEW-ZEALAND AVIFAUNA; BIRD EXTINCTIONS; HAWAIIAN-ISLANDS; OCEANIC ISLANDS; PATTERNS; CONTACT; RISK AB Understanding the ecological mechanisms that lead to extinction is a central goal of conservation. Can understanding ancient avian extinctions help to predict extinction risk in modern birds? I used classification trees trained on both paleoecological and historical data from islands across the Pacific to determine the ecological traits associated with extinction risk. Intrinsic traits, including endemism, large body size, and certain feeding guilds, were tightly linked with avian extinction over the past 3500 years. Species ecology and phylogeny were better predictors of extinction risk through time than extrinsic or abiotic factors. Although human impacts on birds and their habitats have changed over time, modern endangered birds share many of the same ecological characteristics as victims of previous extinction waves. My use of detailed predictions of extinction risk to identify species potentially in need of conservation attention demonstrates the utility of paleoecological knowledge for modern conservation biology. C1 [Boyer, Alison G.] Smithsonian Inst, Natl Museum Nat Hist, MRC 116, Div Birds, Washington, DC 20013 USA. [Boyer, Alison G.] Univ Calif San Diego, Div Biol Sci, Ecol Behav & Evolut Sect, La Jolla, CA 92093 USA. RP Boyer, AG (reprint author), Smithsonian Inst, Natl Museum Nat Hist, MRC 116, Div Birds, POB 37012, Washington, DC 20013 USA. EM agboyer@ucsd.edu OI Boyer, Alison/0000-0002-4252-9725 FU Smithsonian Institution Postdoctoral Fellowship; National Science Foundation Postdoctoral Research Fellowship in Biological Informatics [DBI-0805669]; University of New Mexico; American Museum of Natural History FX T. Blackburn, J. H. Brown, W. Jetz, T. M. Lee, F. A. Smith, and D. W. Steadman provided comments that improved the manuscript. A. G. B. was supported by a Smithsonian Institution Postdoctoral Fellowship and a National Science Foundation Postdoctoral Research Fellowship in Biological Informatics (DBI-0805669). Data collection was made possible by grants from the University of New Mexico and the Frank M. Chapman Fund of the American Museum of Natural History. NR 34 TC 22 Z9 22 U1 1 U2 23 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0888-8892 J9 CONSERV BIOL JI Conserv. Biol. PD APR PY 2010 VL 24 IS 2 BP 511 EP 519 DI 10.1111/j.1523-1739.2009.01341.x PG 9 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 572ZM UT WOS:000275877600021 PM 19843128 ER PT J AU Lepczyk, CA Dauphine, N Bird, DM Conant, S Cooper, RJ Duffy, DC Hatley, PJ Marra, PP Stone, E Temple, SA AF Lepczyk, Christopher A. Dauphine, Nico Bird, David M. Conant, Sheila Cooper, Robert J. Duffy, David C. Hatley, Pamela Jo Marra, Peter P. Stone, Elizabeth Temple, Stanley A. TI What Conservation Biologists Can Do to Counter Trap-Neuter-Return: Response to Longcore et al. SO CONSERVATION BIOLOGY LA English DT Editorial Material ID FERAL CATS C1 [Lepczyk, Christopher A.] Univ Hawaii Manoa, Dept Nat Resources & Environm Management, Honolulu, HI 96822 USA. [Dauphine, Nico] Zool Soc London, London NW1 4RY, England. [Bird, David M.] McGill Univ, Avian Sci & Conservat Ctr, Quebec City, PQ H9X 3V9, Canada. [Conant, Sheila] Univ Hawaii Manoa, Dept Zool, Honolulu, HI 96822 USA. [Cooper, Robert J.] Univ Georgia, Warnell Sch Forestry & Nat Resources, Athens, GA 30602 USA. [Duffy, David C.] Univ Hawaii Manoa, Dept Bot, Pacific Cooperat Studies Unit, Honolulu, HI 96822 USA. [Hatley, Pamela Jo] Pamela Jo Hatley PA, Tampa, FL 33646 USA. [Marra, Peter P.] Smithsonian Inst, Natl Zool Pk, Smithsonian Migratory Bird Ctr, Washington, DC 20008 USA. [Stone, Elizabeth] Ctr Wildlife Hlth Res, Pownal, ME 04069 USA. [Temple, Stanley A.] Univ Wisconsin, Dept Forest & Wildlife Ecol, Madison, WI 53706 USA. [Temple, Stanley A.] Univ Wisconsin, Gaylord Nelson Inst Environm Studies, Madison, WI 53706 USA. RP Lepczyk, CA (reprint author), Univ Hawaii Manoa, Dept Nat Resources & Environm Management, Honolulu, HI 96822 USA. EM lepczyk@hawaii.edu OI Duffy, David/0000-0002-0498-9632 NR 7 TC 15 Z9 15 U1 6 U2 22 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0888-8892 J9 CONSERV BIOL JI Conserv. Biol. PD APR PY 2010 VL 24 IS 2 BP 627 EP 629 DI 10.1111/j.1523-1739.2009.01426.x PG 3 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 572ZM UT WOS:000275877600033 PM 20088960 ER PT J AU Munoz-Fuentes, V Darimont, CT Paquet, PC Leonard, JA AF Munoz-Fuentes, Violeta Darimont, Chris T. Paquet, Paul C. Leonard, Jennifer A. TI The genetic legacy of extirpation and re-colonization in Vancouver Island wolves SO CONSERVATION GENETICS LA English DT Article; Proceedings Paper CT ESF-ConGen Meeting on Integrating Population Genetics and Conservation Biology CY MAY 23-27, 2009 CL Trondheim, NORWAY SP European Sci Fdn Res Network DE Allee effect; Canada; Canis; Domestic dog; Historical DNA; Hybridization; Introgression; Microsatellites; mtDNA; Museum specimens; Wolf ID WOLF CANIS-LUPUS; GENOTYPING ERRORS; DOMESTIC DOG; COMPUTER-PROGRAM; HYBRIDIZATION; POPULATION; MITOCHONDRIAL; MARKERS; IDENTIFICATION; MULTIPLE AB Hybridization between wild and domestic species is of conservation concern because it can result in the loss of adaptations and/or disappearance of a distinct taxon. Wolves from Vancouver Island, British Columbia (Canada), have been subject to several eradication campaigns during the twentieth century and were considered virtually extirpated between 1950 and 1970. In this study, we use control region mitochondrial DNA sequences and 13 autosomal microsatellite loci to characterize Vancouver Island wolves as well as dogs from British Columbia. We observe a turnover in the haplotypes of wolves sampled before and after the 1950-1970 period, when there was no permanent wolf population on the island, supporting the probable local extinction of wolves on Vancouver Island during this time, followed by re-colonization of the island by wolves from mainland British Columbia. In addition, we report the presence of a domestic dog mtDNA haplotype in three individuals eliminated in 1986 that were morphologically identified as wolves. Here we show that Vancouver Island wolves were also identified as wolves based on autosomal microsatellite data. We attribute the hybridization event to the episodically small size of this population during the re-colonization event. Our results demonstrate that at least one female hybrid offspring, resulting from a cross of a male wolf and a female dog or a female hybrid pet with dog mtDNA, successfully introgressed into the wolf population. No dog mtDNA has been previously reported in a population of wild wolves. Genetic data show that Vancouver Island wolves are distinct from dogs and thus should be recognized as a population of wild wolves. We suggest that the introgression took place due to the Allee effect, specifically a lack of mates when population size was low. Our findings exemplify how small populations are at risk of hybridization. C1 [Munoz-Fuentes, Violeta; Leonard, Jennifer A.] Uppsala Univ, Dept Evolutionary Biol, S-75236 Uppsala, Sweden. [Darimont, Chris T.] Univ Calif Santa Cruz, Dept Environm Studies, Santa Cruz, CA 95064 USA. [Darimont, Chris T.; Paquet, Paul C.] Raincoast Conservat Fdn, Denny Isl, BC V0T 1B0, Canada. [Paquet, Paul C.] Univ Calgary, Fac Environm Design, Calgary, AB T2N 1N4, Canada. [Leonard, Jennifer A.] Smithsonian Inst, Natl Zool Pk, Ctr Conservat & Evolutionary Genet, Washington, DC 20008 USA. [Leonard, Jennifer A.] CSIC, Estac Biol Donana, Seville 41092, Spain. RP Munoz-Fuentes, V (reprint author), Uppsala Univ, Dept Evolutionary Biol, Norbyvagen 18D, S-75236 Uppsala, Sweden. EM Violeta.Munoz@ebc.uu.se; darimont@ucsc.edu; ppaquet@baudoux.ca; Jennifer.Leonard@ebc.uu.se RI Munoz-Fuentes, Violeta/E-4218-2014; 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 NR 49 TC 34 Z9 35 U1 0 U2 28 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1566-0621 J9 CONSERV GENET JI Conserv. Genet. PD APR PY 2010 VL 11 IS 2 SI SI BP 547 EP 556 DI 10.1007/s10592-009-9974-1 PG 10 WC Biodiversity Conservation; Genetics & Heredity SC Biodiversity & Conservation; Genetics & Heredity GA 567OE UT WOS:000275455700018 ER PT J AU Hagedorn, M Carter, VL Leong, JC Kleinhans, FW AF Hagedorn, M. Carter, V. L. Leong, J. C. Kleinhans, F. W. TI Physiology and cryosensitivity of coral endosymbiotic algae (Symbiodinium) SO CRYOBIOLOGY LA English DT Article DE Coral; Symbiodinium; Algae; Zooxanthellae; Symbionts; Water and cryoprotectant permeability; Deuterium; Pulse Amplitude Fluorometer ID DIFFUSIONAL WATER PERMEABILITY; CLIMATE-CHANGE; ENCAPSULATION/DEHYDRATION PROTOCOL; HYDRAULIC CONDUCTIVITY; MEMBRANE-PERMEABILITY; MICROALGAE HELD; FUNGIA-SCUTARIA; CRYOPRESERVATION; DIVERSITY; SYMBIOSIS AB Coral throughout the world are under threat To save coral via cryopreservation methods, the Symbiodinium algae that live within many coral cells must also be considered Coral juvenile must often take up these important cells from their surrounding water and when adult coral bleach, they lose their endosymbiotic algae and will die if they are not regained The focus Of this paper was to understand some of the cryo-physiology of the endosymbiotic algae. Symbiodinium. living within three species of Hawaiian coral, Fungia scutaria. Porites compressa and Pocillopora damicornis in Kaneohe Bay, Hawaii Although cryopreservation of algae is common. the successful cryopreservation of these important coral endosymbionts is not common, and these species are often maintained in live serial Cultures within stock centers worldwide Freshly-extracted Symbiodinium were exposed to cryobiologically appropriate physiological stresses and their viability assessed with a Pulse Amplitude Fluorometer Stresses Included sensitivity to chilling temperatures, osmotic stress, and toxic effects of various concentrations and types of cryoprotectants (ie. dimethyl sulfoxide. propylene glycol, glycerol and methanol) To determine the water and cryoprotectant permeabilities of Symbiodinium, uptake of radio-labeled glycerol and heavy water (D(2)O) were measured The three different Symbiodinium subtypes studied demonstrated remarkable similarities in their morphology, sensitivity to cryoprotectants and permeability characteristics, however, they differed greatly in their sensitivity to hypo- and hyposmotic challenges and sensitivity to chilling, suggesting that standard slow freezing cryopreservation may not work well for all Symbiodinium An appendix describes our H(2)O D(2)O water exchange experiments and compares the diffusionally determined permeability with the two parameter model osmotic permeability Published by Elsevier Inc C1 [Hagedorn, M.; Carter, V. L.] Smithsonian Natl Zool Pk, Dept Reprod Sci, Washington, DC 20008 USA. [Hagedorn, M.; Carter, V. L.; Leong, J. C.] Univ Hawaii, Hawaii Inst Marine Biol, Kaneohe, HI 96744 USA. [Kleinhans, F. W.] Indiana Univ Purdue Univ, Dept Phys, Indianapolis, IN 46202 USA. RP Hagedorn, M (reprint author), Smithsonian Inst, POB 1346, Kaneohe, HI 96744 USA. FU Mrs Nancy Upp Porter; Morris Animal Foundation [13139] FX Statement of funding We would like to thank Dr Ruth Gates, and her entire laboratory. especially Jacqueline L Padilla-Gamino. for their kind assistance and loan of the PAM during these experiments Or Michael Stat kindly offered invaluable comments on this paper This work was supported by the financial assistance of Mrs Nancy Upp Porter and the Morris Animal Foundation to M H This paper has an HIMB contribution #13139 NR 56 TC 12 Z9 13 U1 6 U2 25 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0011-2240 J9 CRYOBIOLOGY JI Cryobiology PD APR PY 2010 VL 60 IS 2 BP 147 EP 158 DI 10.1016/j.cryobiol.2009.10.005 PG 12 WC Biology; Physiology SC Life Sciences & Biomedicine - Other Topics; Physiology GA 570OH UT WOS:000275687100006 PM 19857482 ER PT J AU Shik, JZ Kaspari, M AF Shik, Jonathan Z. Kaspari, Michael TI More food, less habitat: how necromass and leaf litter decomposition combine to regulate a litter ant community SO ECOLOGICAL ENTOMOLOGY LA English DT Article DE Ant colony size; decomposer food web; Pheidole; press experiment; scaling ID LOWLAND TROPICAL FOREST; WASMANNIA-AUROPUNCTATA; TOP-DOWN; RAIN-FOREST; BOTTOM-UP; POPULATION; LIMITATION; ECOLOGY; COLONY; SEX AB 2. Maximum, but not mean, colony growth rates were higher on +food plots. However, neither average colony size, nor density was higher on +food plots. In contrast, +food plots saw diminished availability of leaf litter and higher microbial decomposition of cellulose, a main component of the organic substrate that comprises litter habitat. 3. Furthermore, necromass acted as a limiting resource to the ant community only when nest sites were supplemented on +food plots in a second experiment. Many of these +food +nest plots were colonised by the weedy species Wasmannia auropunctata. 4. Combined, these results support the more food-less habitat hypothesis and highlight the importance of embedding studies of litter ant ecology within broader decomposer food web dynamics. C1 [Shik, Jonathan Z.; Kaspari, Michael] Univ Oklahoma, Dept Zool, Grad Program Ecol & Evolutionary Biol, Norman, OK 73019 USA. [Kaspari, Michael] Smithsonian Trop Res Inst, Balboa, Panama. RP Shik, JZ (reprint author), Univ Oklahoma, Dept Zool, Grad Program Ecol & Evolutionary Biol, 730 Van Vleet Oval, Norman, OK 73019 USA. EM jshik@ou.edu OI Kaspari, Michael/0000-0002-9717-5768 FU National Science Foundation [0212386]; University of Oklahoma FX N. Clay, D. Donoso, O. Fincke, J. Kelly, R. Knapp, J. Mendoza, and the members of the Zoology Journal Club provided many excellent suggestions for improving this manuscript. D. Donoso assisted with species identification and construction of litter bags. O. Acevedo and B. Jimenez of STRI provided invaluable logistical support in Panama. This project was funded by the National Science Foundation under Grant no. 0212386 to M. K., and an Adams Summer Research Fellowship and Alumni Fellowship, both from the University of Oklahoma, to J. Z. S. The experiments in this study comply with current laws of the Republic of Panama. NR 53 TC 17 Z9 18 U1 2 U2 14 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0307-6946 J9 ECOL ENTOMOL JI Ecol. Entomol. PD APR PY 2010 VL 35 IS 2 BP 158 EP 165 DI 10.1111/j.1365-2311.2009.01165.x PG 8 WC Entomology SC Entomology GA 564KP UT WOS:000275213300005 ER PT J AU Holmes, MA Ruff, CB Deleon, VB Brown, KM Frohlich, B AF Holmes, Megan A. Ruff, Christopher B. Deleon, Valerie B. Brown, Kirsten M. Frohlich, Bruno TI Scaling in the primate masticatory apparatus SO FASEB JOURNAL LA English DT Meeting Abstract C1 [Holmes, Megan A.; Ruff, Christopher B.; Deleon, Valerie B.; Brown, Kirsten M.] Johns Hopkins Univ, Sch Med, Ctr Funct Anat & Evolut, Baltimore, MD USA. [Frohlich, Bruno] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU FEDERATION AMER SOC EXP BIOL PI BETHESDA PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814-3998 USA SN 0892-6638 J9 FASEB J JI Faseb J. PD APR PY 2010 VL 24 PG 1 WC Biochemistry & Molecular Biology; Biology; Cell Biology SC Biochemistry & Molecular Biology; Life Sciences & Biomedicine - Other Topics; Cell Biology GA V28IW UT WOS:000208675507479 ER PT J AU Owsley, DW AF Owsley, Douglas W. TI The Scientists' Perspective on Kennewick Man SO FASEB JOURNAL LA English DT Meeting Abstract C1 [Owsley, Douglas W.] Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 1 U2 18 PU FEDERATION AMER SOC EXP BIOL PI BETHESDA PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814-3998 USA SN 0892-6638 J9 FASEB J JI Faseb J. PD APR PY 2010 VL 24 PG 1 WC Biochemistry & Molecular Biology; Biology; Cell Biology SC Biochemistry & Molecular Biology; Life Sciences & Biomedicine - Other Topics; Cell Biology GA V28IW UT WOS:000208675500324 ER PT J AU Clay, AM Estes, RD Thompson, KV Wildt, DE Monfort, SL AF Clay, A. Moss Estes, R. D. Thompson, K. V. Wildt, D. E. Monfort, S. L. TI Endocrine patterns of the estrous cycle and pregnancy of wildebeest in the Serengeti ecosystem SO GENERAL AND COMPARATIVE ENDOCRINOLOGY LA English DT Article DE Wildebeest; Progestagens; Seasonality; Fecal steroids; Estrous cycle ID ORYX ORYX-DAMMAH; REPRODUCTIVE SEASONALITY; OVARIAN-FUNCTION; SABLE ANTELOPE; ESTRUS; SYNCHRONIZATION; MOSCHATUS; URINARY; DEER; RAM AB Despite the importance of the western white-bearded wildebeest (Connochaetes taurinus mearnsi) to the Serengeti-Mara ecosystem, surprisingly little is known about the reproductive physiology of this keystone species. A longitudinal, non-invasive endocrine study was conducted on female wildebeest captured from the Serengeti-Mara migration and maintained for similar to 16 months in large fenced enclosures within the species' natural range. An intact bull was introduced to a female subgroup (n = 5), while remaining females (n = 10) were unexposed to a male. Fecal progestagen patterns reflected ovarian activity and pregnancy. In non-pregnant animals, luteal and inter-luteal baseline progestagen values differed (p < 0.001) over time, thereby allowing identification of recurrent estrous cycles. The average durations of the luteal phase, estrous cycle, gestation, and post-partum anestrus were 14.3 +/- 0.5, 22.6 +/- 1.0, 240.8 +/- 11.7, and 104.1 +/- 15.6 d, respectively. Annual reproductive patterns indicated a distinctive period of ovarian activity that extended from 13 May through 3 December(203.5 +/- 29.9 d) with all unmated females displaying from one to 14 estrous cycles. Progestagens were higher (p < 0.001) in pregnant (n = 4) than non-pregnant (n = 10) cows. These data (1) reveal the value of fecal hormone monitoring for establishing the first ever endocrine profiles of female wildebeest in semi-free-living conditions in their native range, and (2) indicate that the species is a seasonal breeder that is polyestrous and a spontaneous ovulator. (C) 2009 Elsevier Inc. All rights reserved. C1 [Clay, A. Moss; Estes, R. D.; Thompson, K. V.; Wildt, D. E.; Monfort, S. L.] Smithsonian Inst, Conservat & Res Ctr, Natl Zool Pk, Front Royal, VA 22630 USA. [Thompson, K. V.] Univ Maryland, Coll Chem & Life Sci, Behav Ecol Evolut & Systemat Program, College Pk, MD 20742 USA. RP Clay, AM (reprint author), 68 Foti Pitta, CY-4180 Ypsonas, Cyprus. EM amossvan@hotmail.com RI Thompson, Katerina/B-6146-2009 FU Smithsonian Institution; Abbott Endowment fund; British Airways FX We thank Nicky Jenner, Penny Spiering, Jessica Beckman, Nicole Presley and the large local staff of the nyumbu project for all their hard work in sample collection, behavioral observation, animal care, and laboratory analysis. Dr. Harald Wiik, Dr. Robert Fyumagwa and the Serengeti veterinary team oversaw the health and well-being of the study animals, and Pete Morkel provided valuable advice and assistance with animal capturing and handling. We are grateful to Simon Mduma, Rian and Lorna Labuschagne and the Singita Grumeti Reserves for essential logistical and bureaucratic support, and to COSTECH, TAWIRI and TANAPA for enabling us to undertake this project. This research was made possible by funding from: Smithsonian Institution Scholarly Studies Program, Abbott Endowment fund, Philip and Betty Reed, Paul Tudor Jones, Paul Khurana, and British Airways. NR 50 TC 0 Z9 0 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 0016-6480 J9 GEN COMP ENDOCR JI Gen. Comp. Endocrinol. PD APR 1 PY 2010 VL 166 IS 2 BP 365 EP 371 DI 10.1016/j.ygcen.2009.12.005 PG 7 WC Endocrinology & Metabolism SC Endocrinology & Metabolism GA 571UR UT WOS:000275781800019 PM 20036667 ER PT J AU Stewart, RA Pelican, KM Brown, JL Wildt, DE Ottinger, MA Howard, JG AF Stewart, R. A. Pelican, K. M. Brown, J. L. Wildt, D. E. Ottinger, M. A. Howard, J. G. TI Oral progestin induces rapid, reversible suppression of ovarian activity in the cat SO GENERAL AND COMPARATIVE ENDOCRINOLOGY LA English DT Article DE Cat; Progestin; Altrenogest; Ovarian suppression; Fecal hormone monitoring; Estrous cycle ID LAPAROSCOPIC ARTIFICIAL-INSEMINATION; FROZEN-THAWED SPERMATOZOA; EXOGENOUS GONADOTROPINS; DOMESTIC CAT; ESTROUS-CYCLE; INTRAUTERINE INSEMINATION; REPRODUCTIVE PHYSIOLOGY; CHORIONIC-GONADOTROPIN; OVULATION INDUCTION; CLOUDED LEOPARD AB The influence of oral progestin (altrenogest; ALT) on cat ovarian activity was studied using non-invasive fecal steroid monitoring. Queens were assigned to various ALT dosages: (1) 0 mg/kg (control; n = 5 cats); (2) 0.044 mg/kg (LOW: n = 5); (3) 0.088 mg/kg (MID; n = 6); or (4) 0.352 mg/kg (HIGH; n = 6). Fecal estrogen and progestagen concentrations were quantified using enzyme immunoassays for 60 days before, 38 days during and 60 days after ALT treatment. Initiation of follicular activity was suppressed in all cats during progestin treatment, whereas controls continued to cycle normally. Females (n = 6) with elevated fecal estrogens at treatment onset completed a normal follicular phase before returning to baseline and remained Suppressed until treatment withdrawal. All cats receiving oral progestin re-initiated follicular activity after treatment, although MID cats experienced the most synchronized return (within 1016 days). Mean baseline fecal estrogens and progestagens were higher (P < 0.05) after treatment in HIGH, but not in LOW or MID cats compared to pre-treatment values. The results demonstrate that: (1) oral progestin rapidly suppresses initiation of follicular activity in the cat. but does not influence a follicular phase that exists before treatment initiation; and (2) queens return to normal follicular activity after progestin withdrawal. This study provides foundational information for research aimed at using progestin priming to improve ovarian response in felids scheduled for ovulation induction and assisted breeding. (C) 2010 Elsevier Inc. All rights reserved. C1 [Stewart, R. A.; Pelican, K. M.; Brown, J. L.; Wildt, D. E.; Howard, J. G.] Smithsonians Natl Zool Pk Conservat & Res Ctr, Ctr Species Survival, Dept Reprod Sci, Front Royal, VA 22630 USA. [Stewart, R. A.; Ottinger, M. A.] Univ Maryland, Dept Anim & Avian Sci, College Pk, MD 20742 USA. RP Wildt, DE (reprint author), Smithsonians Natl Zool Pk Conservat & Res Ctr, Ctr Species Survival, Dept Reprod Sci, Front Royal, VA 22630 USA. EM wildtd@si.edu FU Smithsonian's National Zoological Park; University of Maryland Graduate School; National Institutes of Health [1KO-01-RR17310-01] FX R.A.S. was supported by a Predoctoral Research Fellowship from the Smithsonian's National Zoological Park and a Matching Tuition Scholarship from the University of Maryland Graduate School. Research was supported by a National Institutes of Health SERCA grant to K.M.P. (1KO-01-RR17310-01). We are grateful to Michele Sommers, Cathi Morrison and Stacey Wise for providing excellent animal care. We also thank Ryan Berger, David Kersey, Kate MacKinnon, Bernardo Mesa and Nicole Presley for technical assistance. Dry cat food was donated by the Purina Nestle PetCare Company. NR 54 TC 13 Z9 13 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 0016-6480 EI 1095-6840 J9 GEN COMP ENDOCR JI Gen. Comp. Endocrinol. PD APR 1 PY 2010 VL 166 IS 2 BP 409 EP 416 DI 10.1016/j.ygcen.2009.12.016 PG 8 WC Endocrinology & Metabolism SC Endocrinology & Metabolism GA 571UR UT WOS:000275781800025 PM 20051246 ER PT J AU McFadden, RR Teyssier, C Siddoway, CS Whitney, DL Fanning, CM AF McFadden, R. R. Teyssier, C. Siddoway, C. S. Whitney, D. L. Fanning, C. M. TI Oblique dilation, melt transfer, and gneiss dome emplacement SO GEOLOGY LA English DT Article ID MARIE-BYRD-LAND; ROSS SEA RIFT; SHEAR ZONE; CONVERGENT OROGEN; BRITISH-COLUMBIA; CORE COMPLEX; ANTARCTICA; GRANITE; FLOW; TRANSTENSION AB The upward transfer of partially molten crust and the formation of gneiss domes and metamorphic core complexes commonly take place by localization of normal or oblique extension in the middle and upper crust. In Marie Byrd Land, Antarctica, a transition from wrench to oblique extension occurred during oblique plate divergence along the East Gondwana margin and intracontinental crustal extension associated with the West Antarctic Rift System in mid-Cretaceous time. Migmatites in the Fosdick dome record steep fabrics formed during wrenching, and associated granite networks display crystallization ages of 117-115 Ma. These steep fabrics are overprinted by subhorizontal foliation and leucogranite sheets with crystallization ages in the 109-102 Ma range. Syntectonic emplacement of granite sheets in the South Fosdick detachment zone indicates that detachment tectonics led to rapid exhumation of the terrain by 100 Ma. This study has implications for understanding melt transport, magma accumulation, and the formation of detachments in an oblique tectonic setting. C1 [McFadden, R. R.; Teyssier, C.; Whitney, D. L.] Univ Minnesota, Minneapolis, MN 55455 USA. [Siddoway, C. S.] Colorado Coll, Dept Geol, Colorado Springs, CO 80903 USA. [Fanning, C. M.] Australian Natl Univ, Res Sch Earth Sci, Canberra, ACT 0200, Australia. RP McFadden, RR (reprint author), Smithsonian Trop Res Inst Ancon, Unit 0948, APO, AA 34002 USA. EM mcfaddenR@si.edu RI Fanning, C. Mark/I-6449-2016; OI Fanning, C. Mark/0000-0003-3331-3145; Siddoway, Christine Smith/0000-0003-0478-6138; Whitney, Donna/0000-0002-8296-4692 FU National Science Foundation [NSF-OPP 0337488, NSF-OPP 0338279]; Geological Society of America FX Work was supported by National Science Foundation Office of Polar Programs grants NSF-OPP 0337488 to Teyssier and NSF-OPP 0338279 to Siddoway, and partially supported by a Geological Society of America Bruce L. "Biff" Reed Student Scholarship awarded to McFadden. This manuscript was improved by insightful reviews by Chris Andronicos, An Yin, and Carl Stevenson. NR 40 TC 23 Z9 23 U1 0 U2 6 PU GEOLOGICAL SOC AMER, INC PI BOULDER PA PO BOX 9140, BOULDER, CO 80301-9140 USA SN 0091-7613 EI 1943-2682 J9 GEOLOGY JI Geology PD APR PY 2010 VL 38 IS 4 BP 375 EP 378 DI 10.1130/G30493.1 PG 4 WC Geology SC Geology GA 573XC UT WOS:000275947700023 ER PT J AU Li, S McShea, WJ Wang, DJ Shao, LK Shi, XG AF Li, Sheng McShea, William J. Wang, Dajun Shao, Liangkun Shi, Xiaogang TI The use of infrared-triggered cameras for surveying phasianids in Sichuan Province, China SO IBIS LA English DT Article DE adult sex ratio; daily activity pattern; detection probability; occupancy model; temperate forest ID PHOTOGRAPHIC RATES; ESTIMATE DENSITIES; CRYPTIC MAMMALS; WILDLIFE; PHEASANTS; CONSERVATION; ECOLOGY; PERIOD; TIGERS; INDIA AB We report on the use of infrared-triggered cameras as an effective tool to survey phasianid populations in Wanglang and Wolong Nature Reserves, China. Surveys at 183 camera-trapping sites recorded 30 bird species, including nine phasianids (one grouse and eight pheasant species). Blood Pheasant Ithaginis cruentus and Temminck's Tragopan Tragopan temminckii were the phasianids most often detected at both reserves and were found within the mid-elevation range (2400-3600 m asl). The occupancy rate and detection probability of both species were examined using an occupancy model relative to eight sampling covariates and three detection covariates. The model estimates of occupancy for Blood Pheasant (0.30) and Temminck's Tragopan (0.14) are close to the naive estimates based on camera detections (0.27 and 0.13, respectively). The estimated detection probability during a 5-day period was 0.36 for Blood Pheasant and 0.30 for Temminck's Tragopan. The daily activity patterns for these two species were assessed from the time/date stamps on the photographs and sex ratios calculated for Blood Pheasant (152M : 72F) and Temminck's Tragopan (48M : 21F). Infrared cameras are valuable for surveying these reclusive species and our protocol is applicable to research or monitoring of phasianids. C1 [Li, Sheng; Wang, Dajun] Peking Univ, Ctr Nat & Soc, Coll Life Sci, Beijing 100871, Peoples R China. [McShea, William J.] Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA 22630 USA. [Shao, Liangkun] Wanglang Natl Nat Reserve, Pingwu Cty 622550, Sichuan Prov, Peoples R China. [Shi, Xiaogang] Wolong Natl Nat Reserve, Wolong, Sichuan Prov, Peoples R China. RP Li, S (reprint author), Peking Univ, Ctr Nat & Soc, Coll Life Sci, Beijing 100871, Peoples R China. EM shengli@pku.edu.cn FU Smithsonian's National Zoological Park; Friends of the National Zoo; Peking University; World Wildlife Fund China; Sichuan Forestry Department; China Wildlife Conservation Association FX This work was supported by the Smithsonian's National Zoological Park, Friends of the National Zoo, Peking University, World Wildlife Fund China, Sichuan Forestry Department, and China Wildlife Conservation Association. We thank Chen Youping, Jiang Shiwei, Huang Junzhong, Xu Haibin, Zhang Qingyu, Tang Hao and all the reserve staff who assisted with data collection. We also thank John H. Rappole, Pan Wenshi, Lu Zhi, Wang Hao, Shen Xiaoli, Liu Yang, and several reviewers for fruitful discussions and valuable comments on the manuscript. NR 61 TC 11 Z9 21 U1 4 U2 25 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0019-1019 EI 1474-919X J9 IBIS JI Ibis PD APR PY 2010 VL 152 IS 2 BP 299 EP 309 PG 11 WC Ornithology SC Zoology GA 571OR UT WOS:000275764100007 ER PT J AU Berrocoso, AJ MacLeod, KG Huber, BT Lees, JA Wendler, I Bown, PR Mweneinda, AK Londono, CI Singano, JM AF Berrocoso, Alvaro Jimenez MacLeod, Kenneth G. Huber, Brian T. Lees, Jacqueline A. Wendler, Ines Bown, Paul R. Mweneinda, Amina K. Londono, Carolina Isaza Singano, Joyce M. TI Lithostratigraphy, biostratigraphy and chemostratigraphy of Upper Cretaceous sediments from southern Tanzania: Tanzania drilling project sites 21-26 SO JOURNAL OF AFRICAN EARTH SCIENCES LA English DT Article DE Tanzania drilling project; Late Cretaceous biostratigraphy; Clay-rich shelfal facies; Glassy foraminifera; Holococcoliths; OAE2 isotopic excursion ID COASTAL TANZANIA; KILWA AREA; PALEOGENE; BASIN; TEMPERATURES; SUCCESSION; MOZAMBIQUE; BOUNDARY; ZONATION; CORES AB The 2007 drilling season by the Tanzania drilling project (TOP) reveals a much more expanded Upper Cretaceous sequence than was recognized previously in the Lindi region of southern Tanzania. This TDP expedition targeted recovery of excellently preserved microfossils (foraminifera and calcareous nannofossils) for Late Cretaceous paleoclimatic, paleoceanographic and biostratigraphic studies. A total of 501.17 m of core was drilled at six Upper Cretaceous sites (TDP Sites 21, 22, 23, 24, 24B and 26) and a thin Miocene-Pleistocene section (TDP Site 25). Microfossil preservation at all these sites is good to excellent, with foraminifera often showing glassy shells and consistently good preservation of small and delicate nannofossil taxa. In addition to adding to our knowledge of the subsurface geology, new surface exposures were mapped and the geological map of the region is revised herein. TDP Sites 24, 24B and 26 collectively span the upper Albian to lower-middle Turonian (planktonic foraminiferal Planomalina buxtorfi-Whiteinella archaeocretacea Zones and calcareous nannofossil zones UC0a-UC8a). The bottom of TOP Site 21 is barren, but the rest of the section represents the uppermost Cenomanian-Coniacian (W. archaeocretacea-Dicarinella concavata Zones and nannofossil zones UC5c-UC10). Bulk organic delta C-13 data suggest recovery of part of Ocean Anoxic Event 2 (OAE2) from these four sites. In the upper part of this interval, the lower Turonian nannofossil zones UC6a-7 are characterized by a low-diversity nannoflora that may be related to OAE2 surface-water conditions. TDP Site 22 presents a 122-m-thick, lower-middle Turonian (W. archaeocretacea-Helvetoglobotruncana helvetica Zones) sequence that includes the nannofossil zones UC6a(-7?), but invariable isotopic curves. Further, a lower to upper Campanian (Globotruncana ventricosa-Radotruncana calcarata Zones and nannofossil subzones UC15b(TP)-UC15d(TP)) succession was drilled at TDP Site 23. Lithologies of the new sites include thin units of gray, medium to coarse sandstones, separating much thicker intervals of dark claystones with organic-rich laminated parts, irregular silty to fine sandstone partings, and rare inoceramid and ammonite debris. These lithofacies are interpreted to have been deposited in outer shelf and upper slope settings and indicate relatively stable sedimentary conditions during most of the Late Cretaceous on the Tanzanian margin. (C) 2009 Elsevier Ltd. All rights reserved. C1 [Berrocoso, Alvaro Jimenez; MacLeod, Kenneth G.; Londono, Carolina Isaza] Univ Missouri, Dept Geol Sci, Columbia, MO 65211 USA. [Huber, Brian T.] Smithsonian Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [Lees, Jacqueline A.; Bown, Paul R.] UCL, Dept Earth Sci, London WC1E 6BT, England. [Wendler, Ines] Univ Bremen, D-28334 Bremen, Germany. [Mweneinda, Amina K.] Cardiff Univ, Sch Earth Ocean & Planetary Sci, Cardiff CF10 3YE, S Glam, Wales. [Singano, Joyce M.] Tanzania Petr Dev Corp, Dar Es Salaam, Tanzania. RP Berrocoso, AJ (reprint author), Univ Manchester, Sch Earth Atmospher & Environm Sci, Williamson Bldg,Oxford Bldg, Manchester M13 9PL, Lancs, England. EM alvaro.jimenezberrocoso@manchester.ac.uk RI Bown, Paul/C-5235-2011; MacLeod, Kenneth/C-4042-2017; OI MacLeod, Kenneth/0000-0002-6016-0837; LEES, JACKIE/0000-0003-0737-8826; Bown, Paul/0000-0001-6777-4463 FU USA National Science Foundation [EAR 0642993]; Natural Environmental Research Council [NE/C510508/1]; UCL Graduate School FX The Tanzania Petroleum Development Corporation is gratefully acknowledged for logistical support, and the Tanzania Commission for Science and Technology is thanked for permission to carry out this research in the field. We greatly appreciate the generous hospitality and valuable technical assistance of Ephrem Mchana, Michael Mkereme and Elvis Mgaya (Mr. K). S.W. Lepley and C.A. Kelley are acknowledged for assistance with the isotopic analysis, and C.J. Nicholas and P.N. Pearson for constructive comments on the manuscript. P. Eriksson is thanked for editorial handling. Field work and drilling were funded by a USA National Science Foundation grant to KGM and BTH (EAR 0642993). Participation of JAL was funded by a Natural Environmental Research Council Grant (NE/C510508/1) and the UCL Graduate School. PRB was partly funded by the UCL Graduate School. NR 38 TC 18 Z9 20 U1 0 U2 8 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1464-343X EI 1879-1956 J9 J AFR EARTH SCI JI J. Afr. Earth Sci. PD APR PY 2010 VL 57 IS 1-2 BP 47 EP 69 DI 10.1016/j.jafrearsci.2009.07.010 PG 23 WC Geosciences, Multidisciplinary SC Geology GA 576BV UT WOS:000276119600005 ER PT J AU Neto, MAM Lobato, AKD Alves, JD Goulart, PDP Laughinghouse, HD AF Menezes Neto, Marco Antonio da Silva Lobato, Allan Klynger Alves, Jose Donizeti Pereira Goulart, Patricia de Fatima Laughinghouse, Haywood Dail TI Seed and seedling anatomy in Euterpe oleracea Mart. during the germination process SO JOURNAL OF FOOD AGRICULTURE & ENVIRONMENT LA English DT Article DE Euterpe oleracea Mart.; seed; endosperm; reserve; degradation ID PHOENIX-DACTYLIFERA L; ENDOSPERM AB The aim of the study was to investigate the seed and seedling anatomy, as well as to identify the reserve degradation pathway during the germination process in Euterpe oleracea seeds. Longitudinal and transversal sections of endosperm and embryo seeds, as well as transversal sections of different parts of the seedling were analyzed. The seeds are ruminated with the endosperm formed by cells of several sizes and forms, as well as by presenting very large walls and pits. The embryo is formed by a hypocotyl-radicle axis, procambium and parenchyma with several idioblasts composed of raphides. The seed endosperm has the hypocotyl base and haustorium as sites of starch accumulation. The results obtained by scanning and transmission electron microscopy demonstrate that the endosperm cells present several pits with plasmodesma connections and the haustorium can regulate the endosperm degradation process. Seedling sections between the endosperm and haustorium indicate that the testa projections can have the function of transport during the degradation process of the endosperm reserves. C1 [Menezes Neto, Marco Antonio] Fed Univ Para, Inst Ciencia Biol, BR-66059 Belem, Para, Brazil. [da Silva Lobato, Allan Klynger] Univ Estadual Maringa, Nucleo Pesquisa Aplicada Agr, Maringa, Parana, Brazil. [Alves, Jose Donizeti] Univ Fed Lavras, Dept Biol, Lavras, Brazil. [Pereira Goulart, Patricia de Fatima] Ctr Univ Lavras, Lavras, Brazil. [Laughinghouse, Haywood Dail] Univ Maryland, Dept Environm Sci & Technol, College Pk, MD 20742 USA. [Laughinghouse, Haywood Dail] Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Neto, MAM (reprint author), Fed Univ Para, Inst Ciencia Biol, BR-66059 Belem, Para, Brazil. EM neto@ufpa.br OI Laughinghouse, Haywood/0000-0003-1018-6948 FU Fundacao de Amparo e Desenvolvimento da Pesquisa (Fadesp/Brazil); Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior (CAPES/Brazil) FX We would like to thank the financial support from the Fundacao de Amparo e Desenvolvimento da Pesquisa (Fadesp/Brazil) to M. A. M. Neto and acknowledge the Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior (CAPES/Brazil) for the graduate fellowship supporting A. K. S. Lobato. NR 24 TC 0 Z9 0 U1 2 U2 9 PU WFL PUBL PI HELSINKI PA MERI-RASTILANTIE 3 C, HELSINKI, FI-00980, FINLAND SN 1459-0255 J9 J FOOD AGRIC ENVIRON JI J. Food Agric. Environ. PD APR PY 2010 VL 8 IS 2 BP 1147 EP 1152 PN 2 PG 6 WC Food Science & Technology SC Food Science & Technology GA 615AS UT WOS:000279103700099 ER PT J AU Sosa-Calvo, J Schultz, TR LaPolla, JS AF Sosa-Calvo, Jeffrey Schultz, Ted R. LaPolla, John S. TI A Review of the Dacetine Ants of Guyana (Formicidae: Myrmicinae) SO JOURNAL OF HYMENOPTERA RESEARCH LA English DT Review ID GENUS SMITHISTRUMA FORMICIDAE; PREDATORY BIOLOGY; HYMENOPTERA; STRUMIGENYS; BIODIVERSITY; FOREST AB The dacetine ants of Guyana are reviewed. One genus, Acanthognathus, is added to the three genera reported previously from Guyana. A total of 42 species are reported, 32 of which are new records for Guyana. Among these 32 species, the following five are new species: Pyramica dahlanae sp. n., Pyramica mariae sp. n., Strumigenys acarai sp. n., Strumigenys royi sp. n., and Strumigenys waiwai sp. n. Pyramica dahlanae is unusual for the genus because it lacks propodeal spines and possesses distinctive mandibular morphology. Pyramica mariae belongs to the gundlachi group and is apparently closely related to P. denticulata based on the length of the mandibles, the absence of spongiform tissue on the ventral margin of waist segments, general body pilosity, and general habitus. Pyramica denticulata is illustrated in order to show morphological differences from P. mariae. Strumigenys royi is a remarkable ant because its waist segments lack ventral spongiform tissue, it possesses short propodeal spines, its mandibles are long and with a minute denticle proximal to the apicodorsal tooth of the mandibular fork, and its coloration is distinctive. Strumigenys acarai is unusual because it possesses a minute denticle on the inner margin of the mandibles, distinctive rugulose sculpture on the dorsum of mesonotum that differs from sculpture found on other parts of the body, and a longitudinal median carina on the promesonotum. Strumigenys waiwai is easily recognized by the unusual multifurcate pilosity of the cephalic dorsum and small body size. Modifications of Bolton's (2000) keys to Pyramica and Strumigenys are provided to accommodate the newly described species. C1 [Sosa-Calvo, Jeffrey] Univ Maryland, Dept Entomol, Maryland Ctr Systemat Entomol, College Pk, MD 20742 USA. [Sosa-Calvo, Jeffrey; Schultz, Ted R.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, NHB, Washington, DC 20013 USA. [LaPolla, John S.] Towson Univ, Dept Biol Sci, Towson, MD 21252 USA. RP Sosa-Calvo, J (reprint author), Univ Maryland, Dept Entomol, Maryland Ctr Systemat Entomol, 4112 Plant Sci Bldg, College Pk, MD 20742 USA. FU NSF [DEB 0110073, DEB 0431330]; National Geographic Society Committee for Research and Exploration; Smithsonian Institution USS Restricted Endowment Fund; Smithsonian Institution's Biological Diversity of the Guiana FX We would like to thank Barry Bolton for confirming the new species. We thank George Else, Suzanne Lewis, Christine Taylor (BMNH), and Carlos Roberto Brandao (MZSP) for specimen loans. Ted Suman (USNM) sorted and prepared the specimens, Scott Whittaker (USNM) assisted with the scanning electronic micrographs, and Eugenia Okonski (USNM) databased and labeled the specimens. For corrections and comments on earlier versions of the manuscript we thank Matt Buffington, David Furth, Victor H. Gonzalez, Akito Kawahara, Robert Kula, and John T. Longino. Claudia M. Ortiz and Monica Pava-Ripoll read and commented on the Spanish-language abstract. We thank Brian Fisher and an anonymous reviewer for comments that greatly improved the manuscript. This project was supported in part by NSF DEB 0110073 and DEB 0431330 to TRS, by a National Geographic Society Committee for Research and Exploration grant to JSL and TRS, by the Smithsonian Institution USS Restricted Endowment Fund grant to TRS, and by the Smithsonian Institution's Biological Diversity of the Guiana Shield Program (BDG). This manuscript is number 158 in the BDG Program's publication series. NR 40 TC 1 Z9 4 U1 0 U2 4 PU PENSOFT PUBL PI SOFIA PA 12 PROF GEORGI ZLATARSKI ST, SOFIA, 1700, BULGARIA SN 1070-9428 EI 1314-2607 J9 J HYMENOPT RES JI J. Hymenopt. Res. PD APR PY 2010 VL 19 IS 1 BP 12 EP 43 PG 32 WC Entomology SC Entomology GA 700WU UT WOS:000285775800003 ER PT J AU West-Eberhard, MJ Carpenter, JM Gelin, LFF Noll, FB AF Jane West-Eberhard, Mary Carpenter, James M. Gelin, Luiz Fernando F. Noll, Fernando B. TI Chartergellus golfitensis West-Eberhard: a new species of Neotropical swarm-founding wasp (Hymenoptera: Vespidae, Polistinae) with notes on the taxonomy of Chartergellus zonatus Spinola SO JOURNAL OF HYMENOPTERA RESEARCH LA English DT Article AB Chartergellus golfitensis West-Eberhard new species, is described from Central America and compared with C. zonatus Spinola, a species heretofore inadequately described. C1 [Jane West-Eberhard, Mary] Univ Costa Rica, Escuela Biol, Smithsonian Trop Res Inst, San Jose, Costa Rica. [Carpenter, James M.] Amer Museum Nat Hist, Dept Entomol, New York, NY 10024 USA. [Gelin, Luiz Fernando F.; Noll, Fernando B.] Sao Paulo State Univ, Inst Biociencias Letras & Ciencias Exatas, Dept Bot & Zool, BR-15054000 Sao Jose Do Rio Preto, SP, Brazil. RP West-Eberhard, MJ (reprint author), Univ Costa Rica, Escuela Biol, Smithsonian Trop Res Inst, San Jose, Costa Rica. EM mjwe@sent.com; carpente@amnh.org; fernandogelin@gmail.com; noll@ibilce.unesp.br RI Gelin, Luiz Fernando/C-3301-2011; FERNANDO, NOLL/A-3606-2008 OI FERNANDO, NOLL/0000-0003-0207-1067 NR 13 TC 3 Z9 3 U1 0 U2 2 PU PENSOFT PUBLISHERS PI SOFIA PA GEO MILEV STR 13A, SOFIA, 1111, BULGARIA SN 1070-9428 J9 J HYMENOPT RES JI J. Hymenopt. Res. PD APR PY 2010 VL 19 IS 1 BP 84 EP 93 PG 10 WC Entomology SC Entomology GA 700WU UT WOS:000285775800008 ER PT J AU Buffington, ML AF Buffington, M. L. TI The Description of Banacuniculus Buffington, New Genus (Hymenoptera: Figitidae: Eucoilinae) SO JOURNAL OF HYMENOPTERA RESEARCH LA English DT Article DE Liriomyza; Agromyzidae; new species; new genus; species revision; parasitoid ID GANASPIDIUM-UTILIS HYMENOPTERA; AGROMYZIDAE; LIRIOMYZA; DIPTERA; WATERMELON; REVISION AB The new eucoiline genus Banacuniculus is described to accommodate several species previously placed in Ganaspidium: Banacuniculus hunteri (Crawford), new combination; B. merickeli (Miller), new combination; B. nigrimanus (Kieffer), new combination; B. utilis (Beardsley), new combination; these species are all redescribed. The following new species are described: Banacuniculus brautigani, B. beardsleyi, B. dis, and B. strykeri. As is the case with Ganaspidium, species of Banacuniculus are parasitoids of some of the most pestiferous species of leaf-mining Agromyzidae (Diptera) and have been investigated for use as biological control agents of Liriomyza trifolii (Burgess). Additional phylogenetic, host range, and distributional data, and a key to all species are provided. C1 USDA ARS, Systemat Entomol Lab, Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Buffington, ML (reprint author), USDA ARS, Systemat Entomol Lab, Smithsonian Inst, Natl Museum Nat Hist, 10th & Constitut Ave,POB 37012,MRC 168,NW, Washington, DC 20013 USA. EM matt.buffington@ars.usda.gov FU NSF [DEB9712543] FX Thanks are given to Smithsonian Institution intern Jaime Choi and Systematic Entomology Laboratory Museum Specialist David Adamski for entering label data and labeling specimens; Joe Cora (Ohio State University) assisted with data management and digital map generation. Ricardo Hernandez (Texas A&M University) sent specimens of Banacuniculus Mills to me for identification and allowed me to keep the specimens in the USNM; Robert Kula (Systematic Entomology Lab) and Gregory Zolnerowich (Kansas State Univeristy) assisted with obtaining specimens from the Konza Prairie Reserve; Jennifer Read (Canadian National Collection of Insects), Robert Zuparko (California Academy of Science), Doug Yanega (Entomology Research Museum, UC Riverside), Ed Riley (Texas A&M University) and Steve Heydon (Bohart Museum, UC Davis) assisted with the loans of specimens critical to the success of this research. Rich Pyle (Bishop Museum, Honolulu, HI) provided the Zoo Bank registration numbers. Smithsonian Institution interns Cristy Falcone and Nick Olson provided the environmental SEM image in Fig. 2. I also thank Robert Wharton, Jack Beardsley and Richard Brautigan for advice and positive influences over the years. Finally, I extend thanks to Michael Pogue and Thomas Henry (Systematic Entomology Laboratory) and Scott Solomon (Department of Entomology, Smithsonian Institution) for constructive and useful comments to earlier drafts of this paper. Habitat images were provided by Greg Zolnerowich (Konza Prairie, KS), Lynn Kimsey (Algodone Dunes, CA), and Steve Heydon (Cold Canyon, CA). Initial research for this project was begun under NSF PEET Grant # DEB9712543 awarded to Robert Wharton and James Woolley (Texas A&M University). NR 22 TC 6 Z9 6 U1 0 U2 2 PU PENSOFT PUBL PI SOFIA PA GEO MILEV STR 13A, SOFIA, 1111, BULGARIA SN 1070-9428 EI 1314-2607 J9 J HYMENOPT RES JI J. Hymenopt. Res. PD APR PY 2010 VL 19 IS 1 BP 94 EP 112 PG 19 WC Entomology SC Entomology GA 700WU UT WOS:000285775800009 ER PT J AU Langley, HD AF Langley, Harold D. TI Double Duty in the Civil War: Letters of Sailor and Soldier Edward W. Bacon. SO JOURNAL OF MILITARY HISTORY LA English DT Book Review C1 [Langley, Harold D.] Smithsonian Inst, Washington, DC 20560 USA. RP Langley, HD (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU SOC MILITARY HISTORY PI LEXINGTON PA C/O VIRGINIA MILITARY INST, GEORGE C MARSHALL LIBRARY, LEXINGTON, VA 24450-1600 USA SN 0899-3718 J9 J MILITARY HIST JI J. Mil. Hist. PD APR PY 2010 VL 74 IS 2 BP 593 EP 594 PG 2 WC History SC History GA 581KO UT WOS:000276521600033 ER PT J AU Neufeld, MJ AF Neufeld, Michael J. TI A Fiery Peace in a Cold War: Bernard Schriever and the Ultimate Weapon. SO JOURNAL OF MILITARY HISTORY LA English DT Book Review C1 [Neufeld, Michael J.] Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. RP Neufeld, MJ (reprint author), Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU SOC MILITARY HISTORY PI LEXINGTON PA C/O VIRGINIA MILITARY INST, GEORGE C MARSHALL LIBRARY, LEXINGTON, VA 24450-1600 USA SN 0899-3718 J9 J MILITARY HIST JI J. Mil. Hist. PD APR PY 2010 VL 74 IS 2 BP 644 EP 645 PG 2 WC History SC History GA 581KO UT WOS:000276521600069 ER PT J AU Ericson, PGP Olson, SL Irestedt, M Alvarenga, H Fjeldsa, J AF Ericson, Per G. P. Olson, Storrs L. Irestedt, Martin Alvarenga, Herculano Fjeldsa, Jon TI Circumscription of a monophyletic family for the tapaculos (Aves: Rhinocryptidae): Psiloramphus in and Melanopareia out SO JOURNAL OF ORNITHOLOGY LA English DT Article DE Melanopareia; Psiloramphus; Rhinocryptidae; Tapaculos; Molecular systematics; Taxonomy; South America ID MOLECULAR SYSTEMATICS; SUBOSCINES AVES; PHYLOGENY; PASSERIFORMES; EVOLUTION; BIRDS; GENUS; INFERENCE; NUCLEAR AB The tapaculos (Rhinocryptidae) are tracheophone, suboscine birds restricted to South and Central America. Most tapaculos share a number of internal and external characteristics that have been used to define the family taxonomically. The genera Melanopareia and Psiloramphus do not fully fit this pattern and have caused considerable dispute among taxonomists since they were first described. In this paper we delimit the systematic boundaries of the tapaculos and assess their generic relationships by analysis of molecular sequence data. The results show that whereas Psiloramphus is nested well within the Rhinocryptidae, Melanopareia falls far outside that clade. A new family is erected for Melanopareia. C1 [Ericson, Per G. P.] Swedish Museum Nat Hist, Dept Vertebrate Zool, S-10405 Stockholm, Sweden. [Olson, Storrs L.] Natl Museum Nat Hist, Div Birds, Dept Vertebrate Zool, Smithsonian Inst, Washington, DC 20013 USA. [Irestedt, Martin] Swedish Museum Nat Hist, Mol Systemat Lab, S-10405 Stockholm, Sweden. [Alvarenga, Herculano] Museu Hist Nat Taubate, BR-12070640 Taubate, SP, Brazil. [Fjeldsa, Jon] Univ Copenhagen, Zool Museum, DK-2100 Copenhagen, Denmark. RP Ericson, PGP (reprint author), Swedish Museum Nat Hist, Dept Vertebrate Zool, POB 50007, S-10405 Stockholm, Sweden. EM per.ericson@nrm.se RI Fjeldsa, Jon/A-9699-2013; Research, NRM-BIG/F-2603-2013 OI Fjeldsa, Jon/0000-0003-0790-3600; FU Swedish Research Council [621-2007-5280] FX Our thanks go especially to those researchers who, for years, and often with very small economic means, have collected the specimens and tissue samples without which studies like this could not be made. N. Krabbe is thanked for comments on the manuscript. E. Endrigo kindly provided the photograph of Psilorhamphus. The following institutions provided samples that have been included in the study: Zoological Museum of Copenhagen University, Swedish Museum of Natural History, National Museum of Natural History, American Museum of Natural History and Field Museum of Natural History. The Swedish Research Council provided financial support for the laboratory work (grant no. 621-2007-5280 to PE). NR 47 TC 7 Z9 7 U1 1 U2 2 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0021-8375 J9 J ORNITHOL JI J. Ornithol. PD APR PY 2010 VL 151 IS 2 BP 337 EP 345 DI 10.1007/s10336-009-0460-9 PG 9 WC Ornithology SC Zoology GA 576GH UT WOS:000276131900009 ER PT J AU Angelier, F Tonra, CM Holberton, RL Marra, PP AF Angelier, Frederic Tonra, Christopher M. Holberton, Rebecca L. Marra, Peter P. TI How to capture wild passerine species to study baseline corticosterone levels SO JOURNAL OF ORNITHOLOGY LA English DT Article DE Corticosterone; Capture; Stress; Field endocrinology ID STRESS-RESPONSE; MIGRATORY BIRD; ADRENOCORTICAL-RESPONSE; CHALLENGE HYPOTHESIS; HABITAT SEGREGATION; HORMONAL RESPONSES; NONBREEDING SEASON; AMERICAN REDSTARTS; GREAT TITS; SPARROWS AB Baseline corticosterone levels have been suggested to be an effective tool to assess and monitor the health status of individuals and populations of wild birds. However, measuring baseline corticosterone levels in the field is difficult because the capture protocol may affect rates of corticosterone secretion. In passerine birds, two methods of capture are widely used: (1) passive netting consisting of monitoring mist-nets frequently to check if a bird has been caught; and (2) target netting consisting of installing a conspecific decoy and/or playing a tape-recorded conspecific song in the vicinity of a mist-net until the territorial bird is captured. Our objective here was to determine whether these methods of capture are effective at achieving non-disturbed baseline corticosterone levels in American Redstarts (Setophaga ruticilla). We found that passive netting was associated with elevated corticosterone levels, suggesting that hanging in a net for several minutes activates the HPA axis and, thus, elicits an adreno-cortical stress response. In contrast, target netting was not associated with an increase in corticosterone levels, regardless of the length of time between when the target bird first approached the net and when it was captured. Therefore, we suggest that researchers interested in estimated baseline corticosterone in this species use target netting and not passive netting. C1 [Angelier, Frederic; Marra, Peter P.] Natl Zool Pk, Smithsonian Migratory Bird Ctr, Washington, DC 20008 USA. [Tonra, Christopher M.; Holberton, Rebecca L.] Univ Maine, Lab Avian Biol, Dept Biol Sci, Orono, ME 04469 USA. RP Angelier, F (reprint author), Univ Calif Davis, Dept Neurobiol Physiol & Behav, Davis, CA 95616 USA. EM fangelier@ucdavis.edu RI Tonra, Christopher/B-1620-2013 FU NSF [0649679, 0717338] FX This study was supported by an NSF grant (0649679) to P. P. Marra and R. L. Holberton and an NSF grant (0717338) to P. P. Marra. We thank E. Corliss, J. L. Dowling, J. H. Junda, S. R. Sult and M. A. Thomas for their assistance in the field. We thank the Petroleum Corporation of Hill Nature Preserve, and Yvette Strong and Andrea Donaldson of the Jamaica National Environmental Planning Agency for their cooperation. NR 43 TC 21 Z9 21 U1 1 U2 31 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0021-8375 J9 J ORNITHOL JI J. Ornithol. PD APR PY 2010 VL 151 IS 2 BP 415 EP 422 DI 10.1007/s10336-009-0471-6 PG 8 WC Ornithology SC Zoology GA 576GH UT WOS:000276131900018 ER PT J AU Tamura, Y Ishizuka, O Aoike, K Kawate, S Kawabata, H Chang, Q Saito, S Tatsumi, Y Arima, M Takahashi, M Kanamaru, T Kodaira, S Fiske, RS AF Tamura, Yoshihiko Ishizuka, Osamu Aoike, Kan Kawate, Shinichi Kawabata, Hiroshi Chang, Qing Saito, Satoshi Tatsumi, Yoshiyuki Arima, Makoto Takahashi, Masaki Kanamaru, Tatsuo Kodaira, Shuichi Fiske, Richard S. TI Missing Oligocene Crust of the Izu-Bonin Arc: Consumed or Rejuvenated During Collision? SO JOURNAL OF PETROLOGY LA English DT Article DE collision zone; granite; IBM arc; Oligocene; remobilization; tonalite ID UPPER-MANTLE BENEATH; CENTRAL JAPAN; CONTINENTAL-CRUST; PHILIPPINE-SEA; MARIANA ARC; SUBDUCTION ZONES; VOLCANIC-ROCKS; SILICIC MAGMAS; EVOLUTION; CONSTRAINTS AB The similar to 50 Myr old Izu-Bonin-Mariana (IBM) arc consists mostly of Oligocene middle and lower crust that underlies the upper crust; these units are in turn covered by Quaternary volcanic rocks. Seismic imaging, forearc geology, Ocean Drilling Program drilling and magnetic anomalies suggest that most IBM arc crust was created in Eocene-Oligocene times. However, remnants of this old crust have never been found at the northern end of the arc, where it is colliding with the Honshu arc (Izu collision zone). Two batholiths in this collision zone (the Tanzawa tonalites and the Kofu Granitic Complex) were emplaced during the Miocene (4-17 Ma). Major elements, Zr/Y, rare earth element ratios and normalized abundance patterns, and Sr-Nd isotopic data indicate that these plutonic bodies are compositionally similar to the Oligocene IBM volcanic rocks, and that they are dissimilar to the Miocene, Pliocene and Quaternary IBM lavas and volcaniclastic rocks. We suggest that the Miocene plutonic rocks in the Izu collision zone were derived from partially melted Oligocene middle crust. A model is proposed in which IBM arc middle crust in the collision zone was partially melted during the collision and then intruded into the overlying upper crust of the Honshu and IBM arcs. This resulted in the complete loss of chronological information related to their original source. C1 [Tamura, Yoshihiko; Kawabata, Hiroshi; Chang, Qing; Saito, Satoshi; Tatsumi, Yoshiyuki; Kodaira, Shuichi] Japan Agcy Marine Earth Sci & Technol, Inst Res Earth Evolut, Yokosuka, Kanagawa 2370061, Japan. [Ishizuka, Osamu] Geol Survey Japan AIST, Inst Geosci, Tsukuba, Ibaraki 3058567, Japan. [Aoike, Kan] Japan Agcy Marine Earth Sci & Technol, Ctr Deep Earth Explorat, Yokohama, Kanagawa 2360001, Japan. [Kawate, Shinichi] Musashi High Sch, Tokyo 1768535, Japan. [Arima, Makoto] Yokohama Natl Univ, Grad Sch Environm & Informat Sci, Yokohama, Kanagawa 2408501, Japan. [Takahashi, Masaki; Kanamaru, Tatsuo] Nihon Univ, Inst Nat Sci, Tokyo 1568550, Japan. [Fiske, Richard S.] Smithsonian Inst, Washington, DC 20013 USA. RP Tamura, Y (reprint author), Japan Agcy Marine Earth Sci & Technol, Inst Res Earth Evolut, 2-15 Natsushimacho, Yokosuka, Kanagawa 2370061, Japan. EM tamuray@jamstec.go.jp NR 72 TC 22 Z9 22 U1 2 U2 12 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0022-3530 J9 J PETROL JI J. Petrol. PD APR PY 2010 VL 51 IS 4 BP 823 EP 846 DI 10.1093/petrology/egq002 PG 24 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 587LC UT WOS:000276992800002 ER PT J AU Park, MG Kim, M Kim, S Yih, W AF Park, Myung Gil Kim, Miran Kim, Sunju Yih, Wonho TI DOES DINOPHYSIS CAUDATA (DINOPHYCEAE) HAVE PERMANENT PLASTIDS? SO JOURNAL OF PHYCOLOGY LA English DT Article DE Dinophysis; kleptoplastids; permanent plastids; plastid preference; restriction fragment length polymorphism ID CILIATE MYRIONECTA-RUBRA; MOLECULAR EVIDENCE; DINOFLAGELLATE; ACUMINATA; GROWTH; KLEPTOPLASTIDY; CHLOROPLASTS; ORIGIN; EVOLUTIONARY; PHYLOGENY AB The marine photosynthetic dinoflagellates Dinophysis Ehrenb. species are obligate mixotrophs that require both light and the ciliate prey Myrionecta rubra (= Mesodinium rubrum) for long-term survival. Despite rapid progress on the study of Dinophysis using laboratory cultures, however, whether it has its own permanent plastids or kleptoplastids (i.e., stolen plastids from its ciliate prey) is not fully resolved. Here, we addressed this issue using established cultures of D. caudata Saville-Kent strain DC-LOHABE01 and cross-feeding/starvation experiments encompassing the prey M. rubra strain MR-MAL01 cultures grown on two different cryptophytes (strains CR-MAL01 and CR-MAL11). To follow the fate of prey plastids, psbA gene as a tracer was amplified from individually isolated D. caudata cells, and the PCR products were digested with a restriction enzyme, SfaNI. The RFLP pattern of the PCR products digested by SfaNI revealed that D. caudata continued to keep CR-MAL01-type plastids, while it lost CR-MAL11-type plastids with increasing starvation time. Our results suggest that Dinophysis treats in different ways plastids taken up from different cryptophytes via its ciliate prey M. rubra. Alternatively, D. caudata may already have its own CR-MAL01-type permanent plastid, with two types of plastids (CR-MAL01 and CR-MAL11) obtained from M. rubra being lost within 1 month. This result highlights the need to identify more accurately the origin of plastids in newly isolated photosynthetic Dinophysis species to resolve the issue of plastid permanence. C1 [Park, Myung Gil; Kim, Miran] Chonnam Natl Univ, Dept Oceanog, LOHABE, Kwangju 500757, South Korea. [Kim, Sunju; Yih, Wonho] Kunsan Natl Univ, Dept Oceanog, Gunsan 573701, South Korea. RP Park, MG (reprint author), Smithsonian Environm Res Ctr, POB 28,647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM kimsu@si.edu FU Korean Government (MOEHRD) [KRF-2006-312-C00698]; Korea Ministry of Land, Transport and Maritime Affairs FX This work was supported by the Korea Research Foundation Grant funded by the Korean Government (MOEHRD, Basic Research Promotion Fund) (KRF-2006-312-C00698) (M. G. P.) and a grant from Marine Biotechnology Program funded by Korea Ministry of Land, Transport and Maritime Affairs (W. Y.). We thank J. S. Park for his assistance during the early stage of this work. M. G. P. is grateful to D. Wayne Coats (SERC) who provided valuable comments on the early version of the manuscript. NR 27 TC 20 Z9 20 U1 0 U2 8 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0022-3646 J9 J PHYCOL JI J. Phycol. PD APR PY 2010 VL 46 IS 2 BP 236 EP 242 DI 10.1111/j.1529-8817.2009.00777.x PG 7 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA 577LZ UT WOS:000276226100002 ER PT J AU Centeno, SA Ropret, P Del Federico, E Shamir, J Itin, B Jerschow, A AF Centeno, Silvia A. Ropret, Polonca Del Federico, Eleonora Shamir, Jacob Itin, Boris Jerschow, Alexej TI Characterization of Al(III) complexes with hematein in artistic alum logwood inks SO JOURNAL OF RAMAN SPECTROSCOPY LA English DT Article DE logwood; hematein; ink; Raman spectroscopy; NMR ID NUCLEAR MAGNETIC-RESONANCE; ALUMINATE SOLUTIONS; NATURAL DYES; 2,5-DIHYDROXY-1,4-BENZOQUINONE; SPECTROSCOPY; HEMATOXYLIN; FIELD AB The complexes between Al(III) and hematein, the main coloring matter in alum logwood inks, were characterized by Raman and (27)Al NMR (nuclear magnetic resonance) spectroscopies. Raman spectra of the crystallized complexes and of the compounds applied on a paper substrate are presented and assigned based on published data for the parent compounds. These Raman spectra show that the coordination of the hematein to the Al(III) ions takes place in both cases through the carbonyl and hydroxyl groups in the molecule, and that the aromatic rings are also involved in the interaction. The Raman spectra of the pure hematein -Al(III) complexes were found to be consistent with those recorded for a logwood ink prepared following a late 19th century recipe, using logwood chips instead of pure hematein, and applied on a paper substrate. These spectra can be used as references for the noninvasive identification of the compounds in works of art. (27)Al solid-state NMR showed that the coordination of the Al(III) atoms in the crystallized powder is predominantly octahedral, while when applied on a paper substrate the colorant is present mainly as a tetrahedral complex, with an octahedral coordination also present in a smaller proportion. The fact that the predominant coordinations for the complexes in the crystallized material and for the ones present on the paper substrate are different is relevant for the study of the lightfastness and thermal stability of works of art bearing these media. Copyright (C) 2009 John Wiley & Sons, Ltd. C1 [Centeno, Silvia A.] Metropolitan Museum Art, New York, NY 10028 USA. [Ropret, Polonca] Inst Protect Cultural Heritage Slovenia, Restorat Ctr, Ljubljana 1000, Slovenia. [Ropret, Polonca] Smithsonian Inst, Museum Conservat Inst, Suitland, MD 20746 USA. [Del Federico, Eleonora] Pratt Inst, Dept Math & Sci, Brooklyn, NY 11205 USA. [Shamir, Jacob] Hebrew Univ Jerusalem, Dept Inorgan & Analyt Chem, IL-91904 Jerusalem, Israel. [Itin, Boris] New York Struct Biol Ctr, New York, NY 10027 USA. [Jerschow, Alexej] New York Univ, Dept Chem, New York, NY 10003 USA. RP Centeno, SA (reprint author), Metropolitan Museum Art, 1000 5th Ave, New York, NY 10028 USA. EM silvia.centeno@metmuseum.org OI Jerschow, Alexej/0000-0003-1521-9219; Centeno, Silvia/0000-0002-8496-4426 NR 43 TC 7 Z9 7 U1 3 U2 14 PU JOHN WILEY & SONS LTD PI CHICHESTER PA THE ATRIUM, SOUTHERN GATE, CHICHESTER PO19 8SQ, W SUSSEX, ENGLAND SN 0377-0486 J9 J RAMAN SPECTROSC JI J. Raman Spectrosc. PD APR PY 2010 VL 41 IS 4 BP 445 EP 451 DI 10.1002/jrs.2455 PG 7 WC Spectroscopy SC Spectroscopy GA 591ZM UT WOS:000277344100013 ER PT J AU Mastin, LG Guffanti, M Servranckx, R Webley, P Barsotti, S Dean, K Durant, A Ewert, JW Neri, A Rose, WI Schneider, D Siebert, L Stunder, B Swanson, G Tupper, A Volentik, A Waythomas, CF AF Mastin, L. G. Guffanti, M. Servranckx, R. Webley, P. Barsotti, S. Dean, K. Durant, A. Ewert, J. W. Neri, A. Rose, W. I. Schneider, D. Siebert, L. Stunder, B. Swanson, G. Tupper, A. Volentik, A. Waythomas, C. F. TI A multidisciplinary effort to assign realistic source parameters to models of volcanic ash-cloud transport and dispersion during eruptions (vol 188, pg 1, 2009) SO JOURNAL OF VOLCANOLOGY AND GEOTHERMAL RESEARCH LA English DT Correction C1 [Mastin, L. G.; Ewert, J. W.] US Geol Survey, Cascades Volcano Observ, Vancouver, WA 98683 USA. [Guffanti, M.] US Geol Survey Reston, Reston, VA USA. [Servranckx, R.] Canadian Meteorol Ctr, Quebec City, PQ, Canada. [Webley, P.; Dean, K.] Univ Alaska Fairbanks, Inst Geophys, Fairbanks, AK USA. [Barsotti, S.; Neri, A.] Ist Nazl Geofis & Vulcanol, Sez Pisa, Pisa, Italy. [Durant, A.] Univ Bristol, Dept Earth Sci, Bristol BS8 1TH, Avon, England. [Rose, W. I.] Michigan Technol Univ, Dept Geol & Engn Sci, Houghton, MI 49931 USA. [Schneider, D.; Waythomas, C. F.] USGS Alaska Volcano Observ, Anchorage, AK USA. [Siebert, L.] Smithsonian Inst, Washington, DC 20560 USA. [Stunder, B.] NOAA, Air Resources Lab, Silver Spring, MD 20910 USA. [Swanson, G.] NOAA, Camp Springs, MD USA. [Volentik, A.] Univ S Florida, Dept Geol, Tampa, FL 33620 USA. [Tupper, A.] Bur Meteorol, Casuarina, NT, Australia. RP Mastin, LG (reprint author), US Geol Survey, Cascades Volcano Observ, 1300 SE Cardinal Court,Bldg 10,Suite 100, Vancouver, WA 98683 USA. EM lgmastin@usgs.gov RI Neri, Augusto/A-1623-2009; Durant, Adam/C-7883-2014; Webley, Peter/F-8238-2015; Stunder, Barbara/C-3106-2016 OI Neri, Augusto/0000-0002-3536-3624; Durant, Adam/0000-0002-0198-7332; Webley, Peter/0000-0001-5327-8151; NR 1 TC 0 Z9 0 U1 0 U2 15 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0377-0273 J9 J VOLCANOL GEOTH RES JI J. Volcanol. Geotherm. Res. PD APR 1 PY 2010 VL 191 IS 3-4 BP 245 EP 245 DI 10.1016/j.jvolgeores.2009.10.013 PG 1 WC Geosciences, Multidisciplinary SC Geology GA 583CS UT WOS:000276651100008 ER PT J AU Riley, S AF Riley, Sheila TI As Husbands Go 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 APR 1 PY 2010 VL 135 IS 6 BP 68 EP 69 PG 2 WC Information Science & Library Science SC Information Science & Library Science GA 576KE UT WOS:000276142400058 ER PT J AU Guz, SS AF Guz, Savannah Schroll TI It's All Chinese to Me: An Overview of Culture and Etiquette in China, 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 3 PU REED BUSINESS INFORMATION PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD APR 1 PY 2010 VL 135 IS 6 BP 98 EP 98 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 576KE UT WOS:000276142400189 ER PT J AU Guz, SS AF Guz, Savannah Schroll TI Icons of Beauty: Art, Culure, and the Image of Women 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 APR 1 PY 2010 VL 135 IS 6 BP 98 EP 98 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 576KE UT WOS:000276142400188 ER PT J AU Guz, SS AF Guz, Savannah Schroll TI The Second 100 Japanese Kanji: The Quick and Easy Way To Learn the Basic Japanese Kanji 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 APR 1 PY 2010 VL 135 IS 6 BP 98 EP 98 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 576KE UT WOS:000276142400190 ER PT J AU Guz, SS AF Guz, Savannah Schroll TI Elementary Korean, 2d 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 APR 1 PY 2010 VL 135 IS 6 BP 98 EP 98 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 576KE UT WOS:000276142400185 ER PT J AU Guz, SS AF Guz, Savannah Schroll TI Historical Dictionary of Modern Chinese Literature 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 APR 1 PY 2010 VL 135 IS 6 BP 98 EP 98 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 576KE UT WOS:000276142400187 ER PT J AU Guz, SS AF Guz, Savannah Schroll TI 250 Essential Chinese Characters, vol 1, 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 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 APR 1 PY 2010 VL 135 IS 6 BP 98 EP 98 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 576KE UT WOS:000276142400186 ER PT J AU Guz, SS AF Guz, Savannah Schroll TI Women in the Age of Shakespeare 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 2 PU REED BUSINESS INFORMATION PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD APR 1 PY 2010 VL 135 IS 6 BP 98 EP 98 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 576KE UT WOS:000276142400184 ER PT J AU Guz, SS AF Guz, Savannah Schroll TI Everyday Balinese: Your Guide to Speaking Balinese Quickly and Effortlessly in a Few Hours 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 APR 1 PY 2010 VL 135 IS 6 BP 98 EP 98 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 576KE UT WOS:000276142400191 ER PT J AU Herrera, S Baco, A Sanchez, JA AF Herrera, Santiago Baco, Amy Sanchez, Juan A. TI Molecular systematics of the bubblegum coral genera (Paragorgiidae, Octocorallia) and description of a new deep-sea species SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Bubblegum octocoral; Paragorgia; Sibogagorgia; Deep-sea coral; Seamount; Phylogeny ID WATER GORGONIAN CORALS; RIBOSOMAL-RNA; PHYLOGENETIC INFERENCE; PHENOTYPIC PLASTICITY; MITOCHONDRIAL-DNA; CNIDARIA; TREES; SEQUENCES; ANTHOZOA; IMPACTS AB Bubblegum octocorals (Paragorgia and Sibogagorgia) play an important ecological role in many deep-sea ecosystems. However, these organisms are currently threatened by destructive fishing methods such as bottom trawling. Taxonomic knowledge of conservation targets is necessary for the creation and implementation of efficient conservation strategies. However, for most deep-sea coral groups this knowledge remains incomplete. For instance, despite its similarities with Paragorgia, Sibogagorgia is particular in lacking polyp sclerites, which are present in groups like Paragorgia and the Coralliidae. Although two kinds of sclerites are very similar between Paragorgia and Sibogagorgia, other characters challenge the monophyly of these genera. Here we help to clarify the taxonomy and evolutionary relationships of the bubblegum octocorals and related taxa by examining molecular data. We employed nucleotide sequences of mitochondrial (ND6, ND6-ND3 intergenic spacer, ND3, ND2, CO1, msh1 and 16S) and nuclear (28S and ITS2) genomic regions from several taxa to infer molecular phylogenetics and to examine the correspondence of morphological features with the underlying genetic information. Our data strongly supported the monophyly of the genus Paragorgia, the family Coralliidae (precious corals), and a group of undescribed specimens resembling Sibogagorgia. Further morphological observations were congruent regarding the uniqueness of the undescribed specimens, here defined as a new species, Sibogagorgia cauliflora sp. nov., which occurs in both sides of the North American landmass at depths below 1700 m. This new species resembles S. dennisgordoni with branching in one plane but has fairly different radiate sclerites and significantly divergent DNA sequences. The existence of several diagnostic characters of Sibogagorgia in S. cauliflora indicates that they indeed belong to this genus. It is however remarkable that a small number of medullar canals are also found in this species; medullar canals have been considered as the main diagnostic character of Paragorgia. Thus, the evidence generated here indicates that tire presence or absence of these canals per se is not a conclusively diagnostic character for either genus. The lack of internal-node resolution in the inferred phylogenetic hypotheses of these genera does not allow us to propose a clear scenario regarding the evolution of these traits. (C) 2009 Elsevier Inc. All rights reserved. C1 [Herrera, Santiago; Sanchez, Juan A.] Univ Los Andes, Fac Ciencias, Dept Ciencias Biol, Lab Biol Mol Marina BIOMMAR, Bogota, Colombia. [Herrera, Santiago] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA. [Baco, Amy] Florida State Univ, Dept Oceanog, Tallahassee, FL 32306 USA. RP Sanchez, JA (reprint author), Univ Los Andes, Fac Ciencias, Dept Ciencias Biol, Lab Biol Mol Marina BIOMMAR, Carrera 1E 18A-10,J 409,J309 Lab, Bogota, Colombia. EM sherrera@mit.edu; juansanc@uniandes.edu.co RI Herrera, Santiago/E-5953-2011 OI Herrera, Santiago/0000-0001-7204-9434 FU Global Census of Marine Life on Seamounts Project (CenSeam); Facultad de Ciencias, Department of Biological Sciences of the Universidad de los Andes; NOAA's National Marine Fisheries Service [NA04OAR4600051, UAF-040118]; Smithsonian Graduate Student Fellowship; Systematics Association and the Linnean Society of London; Sigma Xi Research Society; NOAA [NA07OAR4600292]; National Museum of Natural History of the Smithsonian Institution, USA (NMNH-SI); National Institute of Water and Atmospheric Research, New Zealand; Pratt Seamount [NA03OAR4600108, NA04OAR4600071] FX Support for this study was generously provided by a minigrant from the Global Census of Marine Life on Seamounts Project (CenSeam) to J.A.S. and S.H., a grant from the Facultad de Ciencias, Department of Biological Sciences of the Universidad de los Andes to J.A.S, the National Systematics Laboratory of NOAA's National Marine Fisheries Service, a Smithsonian Graduate Student Fellowship to S.H., an award from the Systematics Research Fund of the Systematics Association and the Linnean Society of London to S.H., and a Grant-in-Aid of Research from the Sigma Xi Research Society to S.H. A.B.T. was supported by grant No. NA07OAR4600292 from the NOAA Office of Ocean Exploration. We are especially thankful to S.D. Cairns, A.G. Collins, M. Consalvey, A. Rowden, M. Clark, D. Tracey, K. Schnabel, S. Mills, C.L. Agudelo, L.F. Duenas, N. Ardila, C.S. McFadden, M. Taylor, A. Ormos, J. Hunt, L. Weigt, S. Whittaker, L. Monroy, M. Herrera, M. Simpson, C.D. Cadena, S. Alvarado, J. Cortes, M. Sangrey, and B. Stone for their generous support and assistance. Samples were provided by the National Museum of Natural History of the Smithsonian Institution, USA (NMNH-SI) and the National Institute of Water and Atmospheric Research, New Zealand (NIWA Invertebrate Collection). Coralliid and Paragorgia specimens from Hawaii (except C. secundum and P. regalis) were collected by A.B.T. through grants Nos. NA03OAR4600108 and NA04OAR4600071 and from Pratt Seamount through grant No. NA04OAR4600051 from the NOAA Office of Ocean Exploration. Sibogagorgia cauliflora from Derickson Seamount was collected by A.B.T. through Grant No, UAF-040118 from the NOAA West Coast and Polar Region NURP Center. Specimens of Sibogagorgia cauliflora from Davidson Seamount were provided by Lonny Lundsten of MBARI. C.S. McFadden and N. Ardila kindly contributed additional sequences for the analyses. Molecular work was performed at the Laboratories of Analytical Biology NMNH, Smithsonian Institution. Image from Fig. 7 was taken by M. Taylor. NR 80 TC 23 Z9 23 U1 1 U2 12 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 APR PY 2010 VL 55 IS 1 BP 123 EP 135 DI 10.1016/j.ympev.2009.12.007 PG 13 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 565PI UT WOS:000275306000010 PM 20025983 ER PT J AU Braun, MJ Huddleston, CJ AF Braun, Michael J. Huddleston, Christopher J. TI Comment on Braun and Huddleston "A molecular phylogenetic survey of caprimulgiform nightbirds illustrates the utility of non-coding sequences" Response SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Letter ID AVIAN ORDER CAPRIMULGIFORMES; MODERN BIRDS; AVES; FOSSILS C1 [Braun, Michael J.; Huddleston, Christopher J.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Suitland, MD 20746 USA. [Braun, Michael J.] Univ Maryland, Behav Ecol Evolut & Systemat Program, College Pk, MD 20742 USA. RP Braun, MJ (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, 4210 Silver Hill Rd, Suitland, MD 20746 USA. EM braunm@si.edu NR 23 TC 1 Z9 1 U1 0 U2 1 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 APR PY 2010 VL 55 IS 1 BP 345 EP 346 DI 10.1016/j.ympev.2009.12.014 PG 2 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 565PI UT WOS:000275306000031 ER PT J AU Mehdiabadi, NJ Schultz, TR AF Mehdiabadi, Natasha J. Schultz, Ted R. TI Natural history and phylogeny of the fungus-farming ants (Hymenoptera: Formicidae: Myrmicinae: Attini) SO MYRMECOLOGICAL NEWS LA English DT Article DE Hymenoptera; Formicidae; fungus-growing ants; leafcutter ants; colony life; natural history; evolution; mating; agriculture; review ID LEAF-CUTTING ANTS; GENUS TRACHYMYRMEX FOREL; ACROMYRMEX-OCTOSPINOSUS HYMENOPTERA; MYCOCEPURUS-SMITHII HYMENOPTERA; ATTA-CEPHALOTES L; GROWING ANTS; GARDENING ANT; MICROBE SYMBIOSIS; NEST ARCHITECTURE; COLONY FOUNDATION AB Ants of the tribe Attini comprise a monophyletic group of approximately 230 described and many more undescribed species that obligately depend on the cultivation of fungus for food. In return, the ants nourish, protect, and disperse their fungal cultivars. Although all members of this tribe cultivate fungi, attine ants are surprisingly heterogeneous with regard to symbiont associations and agricultural system, colony size and social structure, nesting behavior, and mating system. This variation is a key reason that the Attini have become a model system for understanding the evolution of complex symbioses. Here, we review the natural-history traits of fungus-growing ants in the context of a recently published phylogeny, collating patterns of evolution and symbiotic coadaptation in a variety of colony and fungus-gardening traits in a number of major lineages. We discuss the implications of these patterns and suggest future research directions. C1 [Mehdiabadi, Natasha J.; Schultz, Ted R.] Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, Washington, DC 20013 USA. [Mehdiabadi, Natasha J.; Schultz, Ted R.] Smithsonian Inst, Labs Analyt Biol, NHB, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Mehdiabadi, NJ (reprint author), Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, POB 37012,CE518,MRC 188, Washington, DC 20013 USA. EM mehdiabadi@si.edu; schultzt@si.edu FU National Science Foundation [DEB 0110073, 0431330]; Smithsonian FX We thank Eugenia Okonski for the beautiful ant images used to create Figure 1; Rachelle Adams, Leeanne Alonso, Jacques Delabie, Ulrich Mueller, Christian Rabeling, Scott Solomon, and Jeffrey Sosa-Calvo for permission to cite unpublished data; and Rachelle Adams, Matthew Kweskin, Jessica Louton, Ulrich Mueller, Scott Solomon, two anonymous reviewers, and the editors for many helpful comments on earlier drafts of the manuscript. This work was supported by National Science Foundation grants DEB 0110073 and 0431330 to TRS and a Smithsonian Post-doctoral Fellowship to NJM. NR 198 TC 53 Z9 56 U1 4 U2 55 PU OESTERREICHISCHE GESELL ENTOMOFAUNISTIK, C/O NATURHISTOR MUSEUM WIEN PI WIEN PA ZWEITE ZOOLOGISCHE ABTEILUNG (INSEKTEN), BURGRING 7, WIEN, AUSTRIA SN 1994-4136 J9 MYRMECOL NEWS JI Myrmecol. News PD APR PY 2010 VL 13 BP 37 EP 55 PG 19 WC Entomology SC Entomology GA 592ZS UT WOS:000277421300006 ER PT J AU Swinbank, AM Smail, I Longmore, S Harris, AI Baker, AJ De Breuck, C Richard, J Edge, AC Ivison, RJ Blundell, R Coppin, KEK Cox, P Gurwell, M Hainline, LJ Krips, M Lundgren, A Neri, R Siana, B Siringo, G Stark, DP Wilner, D Younger, JD AF Swinbank, A. M. Smail, I. Longmore, S. Harris, A. I. Baker, A. J. De Breuck, C. Richard, J. Edge, A. C. Ivison, R. J. Blundell, R. Coppin, K. E. K. Cox, P. Gurwell, M. Hainline, L. J. Krips, M. Lundgren, A. Neri, R. Siana, B. Siringo, G. Stark, D. P. Wilner, D. Younger, J. D. TI Intense star formation within resolved compact regions in a galaxy at z=2.3 SO NATURE LA English DT Article ID SUBMILLIMETER GALAXIES; HIGH-REDSHIFT; MOLECULAR CLOUDS; BIG-BANG; RESOLUTION; POPULATION; LUMINOSITY; CONTINUUM; STARBURST; EMISSION AB Massive galaxies in the early Universe have been shown to be forming stars at surprisingly high rates(1-3). Prominent examples are dust-obscured galaxies which are luminous when observed at sub-millimetre wavelengths and which may be forming stars at a rate of 1,000 solar masses (M(circle dot)) per year(4-7). These intense bursts of star formation are believed to be driven by mergers between gas-rich galaxies(8-9). Probing the properties of individual star-forming regions within these galaxies, however, is beyond the spatial resolution and sensitivity of even the largest telescopes at present. Here we report observations of the sub-millimetre galaxy SMMJ2135-0102 at redshift z = 2.3259, which has been gravitationally magnified by a factor of 32 by a massive foreground galaxy cluster lens. This magnification, when combined with high-resolution sub-millimetre imaging, resolves the star-forming regions at a linear scale of only 100 parsecs. We find that the luminosity densities of these star-forming regions are comparable to the dense cores of giant molecular clouds in the local Universe, but they are about a hundred times larger and 10(7) times more luminous. Although vigorously star-forming, the underlying physics of the star-formation processes at z approximate to 2 appears to be similar to that seen in local galaxies, although the energetics are unlike anything found in the present-day Universe. C1 [Swinbank, A. M.; Smail, I.; Richard, J.; Edge, A. C.; Coppin, K. E. K.] Univ Durham, Inst Computat Cosmol, Durham DH1 3LE, England. [Longmore, S.; Blundell, R.; Gurwell, M.; Wilner, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Harris, A. I.; Hainline, L. J.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Baker, A. J.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [De Breuck, C.] European So Observ, D-85748 Garching, Germany. [Ivison, R. J.] Royal Observ, Sci & Technol Facil Council, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Ivison, R. J.] Royal Observ Edinburgh, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Cox, P.; Krips, M.; Neri, R.] Inst Radio Astron Millimetr, F-38406 St Martin Dheres, France. [Lundgren, A.; Siringo, G.] European So Observ, Santiago 19, Chile. [Siana, B.] CALTECH, Pasadena, CA 91125 USA. [Stark, D. P.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Younger, J. D.] Inst Adv Study, Princeton, NJ 08540 USA. RP Swinbank, AM (reprint author), Univ Durham, Inst Computat Cosmol, South Rd, Durham DH1 3LE, England. EM a.m.swinbank@dur.ac.uk RI Ivison, R./G-4450-2011; Smail, Ian/M-5161-2013 OI Ivison, R./0000-0001-5118-1313; Edge, Alastair/0000-0002-3398-6916; De Breuck, Carlos/0000-0002-6637-3315; /0000-0002-0729-2988; Smail, Ian/0000-0003-3037-257X FU Royal Astronomical Society Sir Norman Lockyer Fellowship; Marie Curie fellowship; Science Technology and Facilities Council fellowship; NASA through a Hubble Fellowship; Smithsonian Institution; Academia Sinica; INSU/CNRS (France); Max Planck Gesellschaft (MPG; Germany); Instituto Geografico Nacional (IGN; Spain) FX We thank the staff at Green Bank Telescope for scheduling the Zpectrometer observations at short notice, and the ESO director for granting director's discretionary time observations with SABOCA. A. M. S. gratefully acknowledges a Royal Astronomical Society Sir Norman Lockyer Fellowship, and J. R. and D. P. S. acknowledge a Marie Curie fellowship and a Science Technology and Facilities Council fellowship respectively. J. D. Y. acknowledges support from NASA through a Hubble Fellowship. The Zpectrometer observations were carried out on the Robert C. Byrd Green Bank Telescope, which is operated by the National Radio Astronomy Observatory, a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. The APEX observations were carried out with ESO Telescopes. The 870 mm interferometric observations were carried out with the Sub-Millimeter Array, which is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. The CO(3-2) observations were carried out with the Plateau de Bure Interferometer, which is supported by INSU/CNRS (France), Max Planck Gesellschaft (MPG; Germany), and Instituto Geografico Nacional (IGN; Spain). J. D. Y. is a Hubble Fellow. NR 28 TC 180 Z9 181 U1 0 U2 5 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD APR 1 PY 2010 VL 464 IS 7289 BP 733 EP 736 DI 10.1038/nature08880 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 577EO UT WOS:000276205000039 PM 20305639 ER PT J AU Gorshkov, AV Hermele, M Gurarie, V Xu, C Julienne, PS Ye, J Zoller, P Demler, E Lukin, MD Rey, AM AF Gorshkov, A. V. Hermele, M. Gurarie, V. Xu, C. Julienne, P. S. Ye, J. Zoller, P. Demler, E. Lukin, M. D. Rey, A. M. TI Two-orbital SU(N) magnetism with ultracold alkaline-earth atoms SO NATURE PHYSICS LA English DT Article ID KONDO-LATTICE MODEL; QUANTUM ANTIFERROMAGNETS; EXCHANGE INTERACTION; OPTICAL LATTICES; GROUND-STATES; SPIN; SUPEREXCHANGE; FERMIONS; SYSTEMS; PHYSICS AB Fermionic alkaline-earth atoms have unique properties that make them attractive candidates for the realization of atomic clocks and degenerate quantum gases. At the same time, they are attracting considerable theoretical attention in the context of quantum information processing. Here we demonstrate that when such atoms are loaded in optical lattices, they can be used as quantum simulators of unique many-body phenomena. In particular, we show that the decoupling of the nuclear spin from the electronic angular momentum can be used to implement many-body systems with an unprecedented degree of symmetry, characterized by the SU(N) group with N as large as 10. Moreover, the interplay of the nuclear spin with the electronic degree of freedom provided by a stable optically excited state should enable the study of physics governed by the spin-orbital interaction. Such systems may provide valuable insights into the physics of strongly correlated transition-metal oxides, heavy-fermion materials and spin-liquid phases. C1 [Gorshkov, A. V.; Xu, C.; Demler, E.; Lukin, M. D.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Hermele, M.; Gurarie, V.; Ye, J.; Rey, A. M.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA. [Julienne, P. S.] NIST, Joint Quantum Inst, Gaithersburg, MD 20899 USA. [Julienne, P. S.] Univ Maryland, Gaithersburg, MD 20899 USA. [Ye, J.; Rey, A. M.] NIST, JILA, Boulder, CO 80309 USA. [Zoller, P.] Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria. [Zoller, P.] Austrian Acad Sci, Inst Quantum Opt & Quantum Informat, A-6020 Innsbruck, Austria. [Demler, E.; Lukin, M. D.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys, Cambridge, MA 02138 USA. RP Gorshkov, AV (reprint author), Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. EM gorshkov@post.harvard.edu RI Ye, Jun/C-3312-2011; Zoller, Peter/O-1639-2014; Julienne, Paul/E-9378-2012; Gorshkov, Alexey/A-9848-2008; Hermele, Michael/B-9424-2009 OI Zoller, Peter/0000-0003-4014-1505; Julienne, Paul/0000-0002-5494-1442; Hermele, Michael/0000-0003-2594-1176; Gorshkov, Alexey/0000-0003-0509-3421; FU NSF; CUA; DARPA; Packard Foundation; AFOSR MURI; NIST FX We gratefully acknowledge conversations with M. M. Boyd, A. J. Daley, S. Folling, W. S. Bakr, J. I. Gillen, L. Jiang, G. K. Campbell, Y. Qi and N. Blumer. This work was supported by NSF, CUA, DARPA, the Packard Foundation, AFOSR MURI and NIST. NR 50 TC 271 Z9 272 U1 6 U2 38 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 APR PY 2010 VL 6 IS 4 BP 289 EP 295 DI 10.1038/NPHYS1535 PG 7 WC Physics, Multidisciplinary SC Physics GA 591EI UT WOS:000277281600023 ER PT J AU Capogrosso-Sansone, B Giorgini, S Pilati, S Pollet, L Prokof'ev, N Svistunov, B Troyer, M AF Capogrosso-Sansone, B. Giorgini, S. Pilati, S. Pollet, L. Prokof'ev, N. Svistunov, B. Troyer, M. TI The Beliaev technique for a weakly interacting Bose gas SO NEW JOURNAL OF PHYSICS LA English DT Article ID EINSTEIN CONDENSATION; ZERO-TEMPERATURE; FLUCTUATIONS; SYMMETRY; BOSONS; SYSTEM AB Aiming at simplicity of explicit equations and, at the same time, controllable accuracy of the theory, we present our results for all the thermodynamic quantities and correlation functions for a weakly interacting Bose gas at short-to-intermediate distances obtained within an improved version of Beliaev's diagrammatic technique. With a controllably small (but essentially finite) Bogoliubov's symmetry-breaking term, Beliaev's diagrammatic technique becomes regular in the infrared limit. Up to higher-order terms (for which we present parametric order-of-magnitude estimates), the partition function and entropy of the system formally correspond to those of a non-interacting bosonic (pseudo-) Hamiltonian with a temperature-dependent Bogoliubov-type dispersion relation. Away from the fluctuation region, this approach provides the most accurate-in fact, the best possible within the Bogoliubov-type pseudo-Hamiltonian framework-description of the system with controlled accuracy. It produces accurate answers for the off-diagonal correlation functions up to distances where the behavior of correlators is controlled by generic hydrodynamic relations and, thus, can be accurately extrapolated to arbitrarily large scales. In the fluctuation region, the non-perturbative contributions are given by universal (for all weakly interacting U(1) systems) constants and scaling functions, which can be obtained separately-by simulating classical U(1) models-and then used to extend the description of the weakly interacting Bose gas to the fluctuation region. The technique works in all spatial dimensions, and we explicitly checked the validity of this technique against first-principle Monte Carlo simulations for various thermodynamic properties and the single-particle density matrix. C1 [Capogrosso-Sansone, B.; Pollet, L.; Prokof'ev, N.; Svistunov, B.] Univ Massachusetts, Dept Phys, Amherst, MA 01003 USA. [Capogrosso-Sansone, B.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys, Cambridge, MA 02138 USA. [Giorgini, S.; Pilati, S.] Univ Trent, Dipartimento Fis, I-38050 Trento, Italy. [Giorgini, S.; Pilati, S.] CNR, INFM, BEC Ctr, I-38050 Trento, Italy. [Pilati, S.; Svistunov, B.] ETH, CH-8093 Zurich, Switzerland. [Pollet, L.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Prokof'ev, N.; Svistunov, B.] IV Kurchatov Atom Energy Inst, Russian Res Ctr, Moscow 123182, Russia. RP Svistunov, B (reprint author), Univ Massachusetts, Dept Phys, Amherst, MA 01003 USA. EM svistunov@physics.umass.edu RI Troyer, Matthias/B-7826-2008; Pollet, Lode/F-6845-2010; PROKOFIEV, NIKOLAY/F-6865-2010; Pilati, Sebastiano/L-4485-2013 OI Troyer, Matthias/0000-0002-1469-9444; Pollet, Lode/0000-0002-7274-2842; NR 43 TC 22 Z9 22 U1 0 U2 5 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 APR 1 PY 2010 VL 12 AR 043010 DI 10.1088/1367-2630/12/4/043010 PG 47 WC Physics, Multidisciplinary SC Physics GA 579EG UT WOS:000276349800010 ER PT J AU Watling, D Wynn, A Zug, GR AF Watling, Dick Wynn, Addison Zug, George R. TI Rediscovery of the Taveuni blind snake SO ORYX LA English DT News Item C1 [Wynn, Addison; Zug, George R.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. NR 0 TC 1 Z9 1 U1 0 U2 0 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0030-6053 J9 ORYX JI Oryx PD APR PY 2010 VL 44 IS 2 BP 165 EP 166 PG 2 WC Ecology SC Environmental Sciences & Ecology GA 599YX UT WOS:000277951400003 ER PT J AU Kornicker, LS Harrison-Nelson, E Coles, SL AF Kornicker, Louis S. Harrison-Nelson, Elizabeth Coles, S. L. TI Ostracoda (Myodocopina) of the Hawaiian Islands SO PACIFIC SCIENCE LA English DT Article AB Ostracoda (Myodocopina) from four of the Hawaiian Islands (Kana'i, Moloka'i, Maui, and Hawai'i) are identified, and a new species, Pterocypridina colesi Kornicker & Harrison-Nelson, that was present on all the Islands is described and illustrated, including all five instars and the adult male and female. The genus was not previously known from the area, and its ontogeny had not been described. The number of species collected on the Islands varied from two on Moloka'i to six on Kaua'i. C1 [Kornicker, Louis S.; Harrison-Nelson, Elizabeth] Smithsonian Inst, Dept Invertebrate Zool, Natl Museum Nat Hist, Washington, DC 20013 USA. [Coles, S. L.] Bernice P Bishop Museum, Dept Nat Sci, Honolulu, HI USA. RP Kornicker, LS (reprint author), Smithsonian Inst, Dept Invertebrate Zool, Natl Museum Nat Hist, Washington, DC 20013 USA. EM kornickl@si.edu FU U.S. Fish and Wildlife Service FX We thank Ralph DeFelice and P. Reath, Bishop Museum, for collecting the specimens upon which this paper is based. All collecting was funded and given logistical support by the U.S. Fish and Wildlife Service. Alps supplied by S.L.C. were modified by Molly Kelly Ryan, Smithsonian Institution. Camera lucida drawings by L.S.K. were inked by Mary Ellen Didion-Carsley of Media Art and Design. NR 25 TC 0 Z9 0 U1 0 U2 1 PU UNIV HAWAII PRESS PI HONOLULU PA 2840 KOLOWALU ST, HONOLULU, HI 96822 USA SN 0030-8870 J9 PAC SCI JI Pac. Sci. PD APR PY 2010 VL 64 IS 2 BP 233 EP 283 DI 10.2984/64.2.233 PG 51 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA 580WV UT WOS:000276482200007 ER PT J AU Burrows, BL Dalgarno, A Cohen, M AF Burrows, B. L. Dalgarno, A. Cohen, M. TI Calculation of exchange energies using algebraic perturbation theory SO PHYSICAL REVIEW A LA English DT Article ID FORCES; H-2+ AB An algebraic perturbation theory is presented for efficient calculations of localized states and hence of exchange energies, which are the differences between low-lying states of the valence electron of a molecule, formed by the collision of an ion Y(+) with an atom X. For the case of a homonuclear molecule these are the gerade and ungerade states and the exchange energy is an exponentially decreasing function of the internuclear distance. For such homonuclear systems the theory is used in conjunction with the Herring-Holstein technique to give accurate exchange energies for a range of intermolecular separations R. Since the perturbation parameter is essentially 1/R, this method is suitable for large R. In particular, exchange energies are calculated for X(2)(+) systems, where X is H, Li, Na, K, Rb, or Cs. C1 [Burrows, B. L.] Staffordshire Univ, Math Sect, Fac Comp Engn & Technol, Stafford ST18 0DG, Staffs, England. [Dalgarno, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Cohen, M.] Hebrew Univ Jerusalem, Dept Phys Chem, IL-91904 Jerusalem, Israel. RP Burrows, BL (reprint author), Staffordshire Univ, Math Sect, Fac Comp Engn & Technol, Stafford ST18 0DG, Staffs, England. EM B.L.Burrows@staffs.ac.uk; adalgarno@cfa.harvard.edu; maurice@fh.huji.ac.il FU Physical Chemistry Department at the Hebrew University of Jerusalem; Institute of Atomic and Molecular Physics at Harvard; EPSRC [EP/F005199/1] FX One of us (B.L.B.) thanks the Physical Chemistry Department at the Hebrew University of Jerusalem and the Institute of Atomic and Molecular Physics at Harvard for their hospitality and support and the EPSRC for the provision of Grant No. EP/F005199/1. NR 17 TC 5 Z9 5 U1 0 U2 5 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD APR PY 2010 VL 81 IS 4 AR 042508 DI 10.1103/PhysRevA.81.042508 PG 8 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 590LJ UT WOS:000277227300075 ER PT J AU Rittenhouse, ST AF Rittenhouse, Seth T. TI Magnetic-field dependence and Efimov resonance broadening in ultracold three-body recombination SO PHYSICAL REVIEW A LA English DT Article ID LARGE SCATTERING LENGTH; ENERGY-LEVELS; UNIVERSALITY; SYSTEM; ATOMS AB We derive an analytic formula which describes the final bound state dependence in ultracold three-body recombination. Using an energy-dependent loss parameter, the recently observed broad resonance in an ultracold gas of (6)Li atoms [T. B. Ottenstein, T. Lompe, M. Kohnen, A. N. Wenz, and S. Jochim, Phys. Rev. Lett. 101, 203202 (2008); J. H. Huckans, J. R. Williams, E. L. Hazlett, R. W. Stites, and K. M. O'Hara, Phys. Rev. Lett. 102, 165302 (2009)] is described quantitatively. We also provide an analytic and approximation for the three-body recombination rate which encapsulates the underlying physics of the universal three-body recombination process. C1 Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Rittenhouse, ST (reprint author), Harvard Smithsonian Ctr Astrophys, ITAMP, 60 Garden St, Cambridge, MA 02138 USA. EM srittenhouse@cfa.harvard.edu RI Rittenhouse, Seth/E-7688-2011 FU NSF through ITAMP at Harvard University; Smithsonian Astrophysical Observatory FX The author would like to thank S. Jochim and H. R. Sadeghpour for useful discussions. Funding for this work was provided by an NSF grant through ITAMP at Harvard University and Smithsonian Astrophysical Observatory. NR 25 TC 4 Z9 4 U1 0 U2 0 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 APR PY 2010 VL 81 IS 4 AR 040701 DI 10.1103/PhysRevA.81.040701 PG 4 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 590LJ UT WOS:000277227300008 ER PT J AU Ticknor, C AF Ticknor, Christopher TI Quasi-two-dimensional dipolar scattering SO PHYSICAL REVIEW A LA English DT Article ID MOLECULES; ATOMS; GAS AB We study two-body dipolar scattering with one dimension of confinement. We include the effects of confinement by expanding this degree of freedom in harmonic oscillator states. We then study the properties of the resulting multichannel system. We study the adiabatic curves as a function of D/l, the ratio of the dipolar and confinement length scales. There is no dipolar barrier for this system when D/l < 0.34. We also study the WKB tunneling probability as a function of D/l and scattering energy. This can be used to estimate the character of the scattering. C1 [Ticknor, Christopher] 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. RP Ticknor, C (reprint author), Los Alamos Natl Lab, Div Theoret, Los Alamos, NM 87545 USA. RI Ticknor, Christopher/B-8651-2014 FU Australian Research Council; NSF; Smithsonian Astrophysical Observatory FX The author thanks S. Rittenhouse, S. Ronen, and E. Kuznetsova for discussions and gratefully acknowledges support from the Australian Research Council and partial support from NSF through ITAMP at Harvard University and the Smithsonian Astrophysical Observatory. NR 33 TC 25 Z9 25 U1 1 U2 3 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 APR PY 2010 VL 81 IS 4 AR 042708 DI 10.1103/PhysRevA.81.042708 PG 6 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 590LJ UT WOS:000277227300103 ER PT J AU Fiske, IJ Bruna, EM AF Fiske, Ian J. Bruna, Emilio M. TI Alternative spatial sampling in studies of plant demography: consequences for estimates of population growth rate SO PLANT ECOLOGY LA English DT Article DE Lambda; Matrix models; Plot; Population dynamics; Sampling; Vital rates ID PROJECTION MATRIX ANALYSIS; PLOT SIZE; UNDERSTORY HERB; DYNAMICS; COMMUNITY; DENSITY; MODELS; FOREST; FIELD; AUTOCORRELATION AB Ecologists commonly use matrix models to study the population dynamics of plants. Most studies of plant demography use plot-based methods to collect data, in part, because mapped individuals are easier to relocate in subsequent surveys and survey methods can be standardized among sites. However, there is tremendous variation among studies, both in terms of plot arrangement and the total area sampled. In addition, there has been little discussion of how alternative sampling arrangements influence estimates of population growth rates (lambda) calculated with matrix models. We surveyed the literature to determine what sampling designs are most used in studies of plant demography using matrix models. We then used simulations of three common sampling techniques-using a single randomly placed plot, multiple randomly placed plots, and systematically distributed plots-to evaluate how these alternative strategies influenced the precision of estimates of lambda. These simulations were based on long-term demographic data collected on 13 populations of the Amazonian understory herb Heliconia acuminate (Heliconiaceae). We found that the method used to collect data did not affect the bias or precision of estimates in our system-a surprising result, since the advantage in efficiency that is gained from systematic sampling is a well-known result from sampling theory. Because the statistical advantage of systematic sampling is most evident when there is spatial structure in demographic vital rates, we attribute this result to the lack of spatially structured vital rates in our focal populations. Given the likelihood of spatial autocorrelation in most ecological systems, we advocate sampling with a systematic grid of plots in each study site, as well as that researchers ensure that enough area is sampled-both within and across sites-to encompass the range of spatial variation in plant survival, growth, and reproduction. C1 [Fiske, Ian J.; Bruna, Emilio M.] Univ Florida, Dept Wildlife Ecol & Conservat, Gainesville, FL 32611 USA. [Bruna, Emilio M.] Univ Florida, Ctr Latin Amer Studies, Gainesville, FL 32611 USA. [Bruna, Emilio M.] Inst Nacl de Pesquisas da Amazonia, Biol Dynam Forest Fragments Project, BR-69011970 Manaus, AM, Brazil. [Bruna, Emilio M.] Smithsonian Trop Res Inst, BR-69011970 Manaus, AM, Brazil. RP Bruna, EM (reprint author), Univ Florida, Dept Wildlife Ecol & Conservat, POB 110430, Gainesville, FL 32611 USA. EM embruna@ufl.edu RI Bruna, Emilio/H-2769-2012 OI Bruna, Emilio/0000-0003-3381-8477 NR 49 TC 2 Z9 2 U1 3 U2 15 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1385-0237 J9 PLANT ECOL JI Plant Ecol. PD APR PY 2010 VL 207 IS 2 BP 213 EP 225 DI 10.1007/s11258-009-9666-4 PG 13 WC Plant Sciences; Ecology; Forestry SC Plant Sciences; Environmental Sciences & Ecology; Forestry GA 563JC UT WOS:000275123700003 ER PT J AU Salazar, C Baxter, SW Pardo-Diaz, C Wu, G Surridge, A Linares, M Bermingham, E Jiggins, CD AF Salazar, Camilo Baxter, Simon W. Pardo-Diaz, Carolina Wu, Grace Surridge, Alison Linares, Mauricio Bermingham, Eldredge Jiggins, Chris D. TI Genetic Evidence for Hybrid Trait Speciation in Heliconius Butterflies SO PLOS GENETICS LA English DT Article ID REPRODUCTIVE ISOLATION; SYMPATRIC SPECIATION; COLOR PATTERN; ECOLOGICAL SPECIATION; DNA; EVOLUTION; HYBRIDIZATION; SELECTION; MODEL; LEPIDOPTERA AB Homoploid hybrid speciation is the formation of a new hybrid species without change in chromosome number. So far, there has been a lack of direct molecular evidence for hybridization generating novel traits directly involved in animal speciation. Heliconius butterflies exhibit bright aposematic color patterns that also act as cues in assortative mating. Heliconius heurippa has been proposed as a hybrid species, and its color pattern can be recreated by introgression of the H. m. melpomene red band into the genetic background of the yellow banded H. cydno cordula. This hybrid color pattern is also involved in mate choice and leads to reproductive isolation between H. heurippa and its close relatives. Here, we provide molecular evidence for adaptive introgression by sequencing genes across the Heliconius red band locus and comparing them to unlinked wing patterning genes in H. melpomene, H. cydno, and H. heurippa. 670 SNPs distributed among 29 unlinked coding genes (25,847bp) showed H. heurippa was related to H. c. cordula or the three species were intermixed. In contrast, among 344 SNPs distributed among 13 genes in the red band region (18,629bp), most showed H. heurippa related with H. c. cordula, but a block of around 6,5kb located in the 39 of a putative kinesin gene grouped H. heurippa with H. m. melpomene, supporting the hybrid introgression hypothesis. Genealogical reconstruction showed that this introgression occurred after divergence of the parental species, perhaps around 0.43Mya. Expression of the kinesin gene is spatially restricted to the distal region of the forewing, suggesting a mechanism for pattern regulation. This gene therefore constitutes the first molecular evidence for adaptive introgression during hybrid speciation and is the first clear candidate for a Heliconius wing patterning locus. C1 [Salazar, Camilo; Baxter, Simon W.; Pardo-Diaz, Carolina; Wu, Grace; Surridge, Alison; Jiggins, Chris D.] Univ Cambridge, Dept Zool, Cambridge, England. [Salazar, Camilo; Pardo-Diaz, Carolina; Bermingham, Eldredge] Smithsonian Trop Res Inst, Balboa, Panama. [Salazar, Camilo; Linares, Mauricio] Univ Los Andes, Inst Genet, Bogota, Colombia. RP Salazar, C (reprint author), Univ Cambridge, Dept Zool, Cambridge, England. EM salazar.camilo@gmail.com RI Jiggins, Chris/B-9960-2008; Salazar, camilo/A-1647-2010; Linares, Mauricio/I-3509-2016; Pardo-Diaz, Carolina/C-7936-2016 OI Jiggins, Chris/0000-0002-7809-062X; Salazar, camilo/0000-0001-9217-6588; Linares, Mauricio/0000-0002-1021-0226; Wu, Grace C./0000-0002-8290-119X; Pardo-Diaz, Carolina/0000-0002-7259-1183 FU Royal Society; Leverhulme Trust; BBSRC; Smithsonian Tropical Research Institute (STRI)-Academic Programs Office; COLCIENCIAS FX CDJ and SWB were supported by the Royal Society, Leverhulme Trust, and the BBSRC. CS was supported by the Smithsonian Tropical Research Institute (STRI)-Academic Programs Office and a Leverhulme Trust grant to CDJ. CP-D was supported by a STRI internship. ML was funded by COLCIENCIAS. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 71 TC 40 Z9 43 U1 4 U2 39 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 185 BERRY ST, STE 1300, SAN FRANCISCO, CA 94107 USA SN 1553-7390 J9 PLOS GENET JI PLoS Genet. PD APR PY 2010 VL 6 IS 4 AR e1000930 DI 10.1371/journal.pgen.1000930 PG 12 WC Genetics & Heredity SC Genetics & Heredity GA 592CY UT WOS:000277354200046 PM 20442862 ER PT J AU Adamski, D Landry, JF Passoa, S Tracy, RA AF Adamski, D. Landry, J. -F. Passoa, S. Tracy, R. A. TI HISTORY, DISTRIBUTION, AND IDENTIFICATION OF EXOTELEIA DODECELLA (L.) (LEPIDOPTERA: GELECHIIDAE) IN NORTH AMERICA, WITH INSIGHTS INTO THE SYSTEMATICS OF EXOTELEIA WALLENGREN USING CHARACTERS OF THE ADULT, IMMATURES, BIONOMICS, AND DNA BARCODES SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE bud-miner; chaetotaxy; DNA barcode; Europe; Exoteleia pinifoliella; invasive species; life cycle; morphology; needle-miner; North America; parasitoids; pine AB Exoteleia dodecella (L.) (Lepidoptera: Gelechiidae), a native of Europe, was first documented from North America at several locations in eastern Canada. Additional records indicate this moth has now spread throughout New England and west to northern Pennsylvania, New York, and possibly into Michigan in the United States. A second introduction of E. dodecella has occurred near the Vancouver area of British Columbia in Canada. To help with the identification of E. dodecella, morphological, biological, and molecular evidence are presented. Key features of the adult, larval, and pupal morphology are compared to other species of Exoteleia and illustrated with line drawings or scanning electron micrographs. The high sequence divergence (>7%) of E. dodecella compared to samples of related native North American species demonstrates that DNA barcodes are a useful identification tool for this pest. A summary of the biology of E. dodecella, including 12 species of larval and pupal parasitoids (most representing new host records), is also included. C1 [Adamski, D.] Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, Washington, DC 20013 USA. [Landry, J. -F.] Agr & Agri Food Canada, Ottawa, ON K1A 0C6, Canada. [Passoa, S.] USDA Forest Serv, APHIS, PPQ, USDA,No Res Stn, Columbus, OH 43212 USA. [Passoa, S.] Ohio State Univ, Museum Biodivers, Columbus, OH 43212 USA. [Tracy, R. A.] USDA, APHIS, PPQ, Linden, NJ 07036 USA. RP Adamski, D (reprint author), Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, POB 37012,NHB-E523, Washington, DC 20013 USA. EM adamskid@si.edu; landryjf@agr.gc.ca; steven.c.passoa@usda.gov; robert.a.tracy@aphis.usda.gov FU Genome Canada through the Ontario Genomics Institute, NSERC FX We thank the following staff, formerly of the Systematic Entomology Laboratory, Smithsonian Institution National Museum of Natural History, Washington, DC, for identifications of parasitoids: R. W. Carlson (Ichneumonidae), E. E. Grissell (Eulophidae), P. M. Marsh (Braconidae), A. S. Menke (Bethylidae), and C. W. Sabrosky (Diptera). We are grateful to Scott Whittaker, Lab Manager, Scanning Electron Microscopy Laboratory, Smithsonian Institution, Washington, DC, for the suggestions on larval fixation prior to SEM analysis and scheduling time on the SEM. Diana Marques, Lisboa, Portugal, constructed the fine computer generated illustrations of the male and female genitalia and produced the plates. We also thank J. R. deWaard, D. Handfield, P. D. N. Hebert, and D. Holden for supplying some barcoded specimens. Support for DNA barcoding was provided by the Canadian Barcode of Life Network from Genome Canada through the Ontario Genomics Institute, NSERC (to JFL), and other sponsors listed at www.BOLDNET.ca. NR 53 TC 2 Z9 4 U1 0 U2 2 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD APR PY 2010 VL 112 IS 2 BP 183 EP 206 DI 10.4289/0013-8797.112.2.183 PG 24 WC Entomology SC Entomology GA 610EL UT WOS:000278713900001 ER PT J AU Kula, RR Knight, KS Rebbeck, J Bauer, LS Cappaert, DL Gandhi, KJK AF Kula, Robert R. Knight, Kathleen S. Rebbeck, Joanne Bauer, Leah S. Cappaert, David L. Gandhi, Kamal J. K. TI LELUTHIA ASTIGMA (ASHMEAD) (HYMENOPTERA: BRACONIDAE: DORYCTINAE) AS A PARASITOID OF AGRILUS PLANIPENNIS FAIRMAIRE (COLEOPTERA: BUPRESTIDAE: AGRILINAE), WITH AN ASSESSMENT OF HOST ASSOCIATIONS FOR NEARCTIC SPECIES OF LELUTHIA CAMERON SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE ash; biological control; emerald ash borer; exotic; Fraxinus; invasive; natural enemies; Nearctic AB Published host associations are assessed for Leluthia astigma (Ashmead), Leluthia floridensis Marsh, and Leluthia mexicana Cameron, the three known species of Leluthia Cameron in the Nearctic Region. Leluthia astigma is reported as a parasitoid of Agrilus planipennis Fairmaire, emerald ash borer (EAB), infesting Fraxinus americana L., white ash, in Delaware County, Ohio. It is the first species of Leluthia for which a determined species of Agrilus Curtis has been confirmed as a host and the association vouchered. All other hosts reported in the literature for L. astigma require confirmation through rearing from an isolated host or documentation of an unequivocal host-parasitoid association. Leluthia astigma adults reared from parasitoid cocoons collected in Delaware County, Ohio parasitized and produced F(1) adults in the laboratory on last-instar EAB larvae collected in County, Michigan. Parasitism of EAB and other natural history data are reported for L. astigma, including the first records of L. astigma from Kansas and New York. C1 [Kula, Robert R.] ARS, Systemat Entomol Lab, Inst Plant Sci, US Dept Agr,Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA. [Knight, Kathleen S.; Rebbeck, Joanne] US Forest Serv, No Res Stn, US Dept Agr, Delaware, OH 43015 USA. [Bauer, Leah S.] Michigan State Univ, US Forest Serv, No Res Stn, US Dept Agr, E Lansing, MI 48823 USA. [Cappaert, David L.] Michigan State Univ, Dept Entomol, E Lansing, MI 48824 USA. [Gandhi, Kamal J. K.] Univ Georgia, Daniel B Warnell Sch Forestry & Nat Resources, Athens, GA 30602 USA. RP Kula, RR (reprint author), ARS, Systemat Entomol Lab, Inst Plant Sci, US Dept Agr,Natl Museum Nat Hist,Smithsonian Inst, POB 37012,MRC 168, Washington, DC 20013 USA. EM Robert.Kula@ars.usda.gov FU USDA FX We thank Dempsey Middle School 7th and 8th grade science students and their teacher, Mrs. Deborah Bogard, for dissecting logs and collecting specimens and data. We are grateful to Delaware City Schools for their cooperation. We acknowledge Robert Ford, Tim Fox, Lawrence Long, Kyle Costilow, Joan Jolliff, and Stan McDonald for cutting and hauling ash trees; Joan Jolliff, Deborah Miller, and Bill Morgan for laboratory work; Deborah McCullough and Andrew Tluczek for advice on peeling ash logs; Annemarie Smith, Charles Flower, and Lisa Tabak for helping supervise in the classroom; and the Ohio Department of Agriculture for lending drawknives. We appreciate Natalia J. Vandenberg (Systematic Entomology Laboratory [SEL]) and Norman E. Wood ley (SEL) for their efforts in identifying a buprestid cadaver associated with a L. astigma cocoon and adult in the USNM. We are grateful to John S. Strazanac (West Virginia University-Morgantown) for examining specimens of L. astigma in the WVUC. We thank Thomas J. Henry (SEL), John W. Brown (SEL), and Jeffrey Sosa-Calvo (University of Maryland-College Park) for reviewing the manuscript. The USDA Forest Service Civil Rights Diversity Special Projects Fund provided funding for this project. NR 20 TC 13 Z9 13 U1 2 U2 5 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD APR PY 2010 VL 112 IS 2 BP 246 EP 257 DI 10.4289/0013-8797.112.2.246 PG 12 WC Entomology SC Entomology GA 610EL UT WOS:000278713900006 ER PT J AU Pogue, MG Honey, M Zilli, A AF Pogue, Michael G. Honey, Martin Zilli, Alberto TI NEW SYNONYMY IN A NORTH AMERICAN SPECIES OF PYRRHIA HUBNER, [1821] (LEPIDOPTERA: NOCTUIDAE) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Heliothinae; new synonym; New World; Old World; Pyrrhia umbra AB The nomenclatural history for Pyrrhia aurantiago (Guenee 1852), Pyrrhia cilisca (Guenee 1852), and Pyrrhia exprimens (Walker 1857) is detailed to resolve confusion over the last 150 years concerning those names. Based on characters of the male and female genitalia and coloration and pattern of the fore- and hind wing, Pyrrhia adela Lafontaine and Mikkola 1996 is proposed as a new synonym of Pyrrhia cilisca (Guenee 1852). C1 [Pogue, Michael G.] ARS, Systemat Entomol Lab, PSI, USDA,Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA. [Honey, Martin] Nat Hist Museum, Dept Entomol, London SW7 5BD, England. [Zilli, Alberto] Museum Zool, I-00197 Rome, Italy. RP Pogue, MG (reprint author), ARS, Systemat Entomol Lab, PSI, USDA,Natl Museum Nat Hist,Smithsonian Inst, POB 37012,MRC 168, Washington, DC 20013 USA. EM michael.pogue@ars.usda.gov; m.honey@nhm.ac.uk; a.zilli@comune.roma.it NR 35 TC 0 Z9 0 U1 0 U2 1 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD APR PY 2010 VL 112 IS 2 BP 274 EP 280 DI 10.4289/0013-8797.112.2.274 PG 7 WC Entomology SC Entomology GA 610EL UT WOS:000278713900008 ER PT J AU Wei, MC Smith, DR AF Wei, Meicai Smith, David R. TI REVIEW OF SYRISTA KONOW (HYMENOPTERA: CEPHIDAE) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Review DE Rosa; shoot borer; new combinations; China; Japan AB Syrista Konow includes five species: S. parreyssii (Spinola 1843) from the Mediterranean Region and Near East; S. similis Mocsary 1904, from Japan and China; and S. xiaoi Wei 2008, S. rufiabdominalis (Wei and Nie 1996), n. comb., and S. incisa (Wei and Nie 1996), n. comb., from China. The lectotype of Syrista similis and holotypes of S. incisa and S. rufiabdominalis are redescribed, and the male of S. xiaoi is described. A key to the five species is presented. Species are shoot borers in Rosa spp. (Rosaceae). C1 [Wei, Meicai] Cent S Univ Forestry & Technol, Lab Insect Systemat & Evolutionary Biol, Changsha 410004, Hunan, Peoples R China. [Smith, David R.] ARS, Systemat Entomol Lab, PSI, USDA,Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA. RP Wei, MC (reprint author), Cent S Univ Forestry & Technol, Lab Insect Systemat & Evolutionary Biol, Changsha 410004, Hunan, Peoples R China. EM weimc@126.com; dave.smith@ars.usda.gov FU National Natural Science Foundation of China [30571504, 30771741] FX We extend thanks to the following for allowing examination of specimens: Andreas Taeger and Stephan Blank during our 2008 visit to DEI; Tosio Kumata, during DRS's 1979 visit to Hokkaido University, Sapporo (HU), Sandor Csosz (HNHM); Akihiko Shinohara (NSMT); E. Richard Hoebeke (CUIC); Henri Goulet (CNC); John Quinlan, during DRS's 1978 visit to The Natural History Museum, UK (BMNH). Thanks are also due to Gengyun Niu (CSUFT) and Michele Touchet (Systematic Entomology Laboratory, U.S. Department of Agriculture [SETA) for preparing some figures. We appreciate the reviews of H. Goulet, Agriculture and Agri-Food Canada, Ottawa, and S. J. Scheffer and T. J. Henry, SEL, Beltsville, MD, and Washington, DC, respectively. The research was supported by the National Natural Science Foundation of China (No. 30571504 and 30771741). NR 24 TC 2 Z9 4 U1 0 U2 0 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD APR PY 2010 VL 112 IS 2 BP 302 EP 316 DI 10.4289/0013-8797.112.2.302 PG 15 WC Entomology SC Entomology GA 610EL UT WOS:000278713900011 ER PT J AU Kruse, JJ Smith, DR Schiff, NM AF Kruse, James J. Smith, David R. Schiff, Nathan M. TI Monsoma pulveratum (Retzius) (Hymenoptera: Tenthredinidae: Allantinae), A Palaearctic Sawfly Defoliator of Alder in Alaska and New to the United States SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Editorial Material C1 [Kruse, James J.] US Forest Serv, Forest Hlth Protect, State & Private Forestry, USDA, Fairbanks, AK 99709 USA. [Smith, David R.] ARS, Systemat Entomol Lab, PSI, USDA,Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20560 USA. [Schiff, Nathan M.] US Forest Serv, Ctr Bottomland Hardwoods Res, So Res Stn, USDA, Stoneville, MS 38776 USA. RP Kruse, JJ (reprint author), US Forest Serv, Forest Hlth Protect, State & Private Forestry, USDA, 3700 Airport Way, Fairbanks, AK 99709 USA. EM jkruse@fs.fed.us; dave.smith@ars.usda.gov; nschiff@fs.fed.us NR 7 TC 5 Z9 5 U1 0 U2 6 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD APR PY 2010 VL 112 IS 2 BP 332 EP 335 DI 10.4289/0013-8797-112.2.332 PG 4 WC Entomology SC Entomology GA 610EL UT WOS:000278713900014 ER PT J AU Santos, LM Tierney, SM Wcislo, WT AF Santos, Leandro M. Tierney, Simon M. Wcislo, William T. TI Nest descriptions of Megalopta aegis (Vachal) and M. guimaraesi Santos & Silveira (Hymenoptera, Halictidae) from the Brazilian Cerrado SO REVISTA BRASILEIRA DE ENTOMOLOGIA LA English DT Article DE Augochlorini; bees; nesting biology; nocturnal ID TRIBE AUGOCHLORINI HYMENOPTERA; ECUADORIA HYMENOPTERA; SOCIAL-BEHAVIOR; SWEAT BEES; BIOLOGY; GENALIS; CLASSIFICATION; EVOLUTION AB Nest descriptions of Megalopta aegis (Vachal) and M. guimaraesi Santos & Silveira (Hymenoptera, Halictidae) from the Brazilian Cerrado. We present the first data on the nesting biology of Megalopta aegis and M. guimaraesi from southeastern Brazil. Nests were collected in the Area de Protecao Ambiental Agua Limpa, Bauru, Sao Paulo state. Our data suggest that nest architecture is conserved throughout all species of Megalopta. Two nests of M. guimaraesi consisted of a single female with brood. Of three M. aegis nests, two contained single females with brood and the third nest contained three adult females, with three times more brood than any single female nest. This observation suggests that social behavior in M. aegis is facultative, as known for other Megalopta species. C1 [Santos, Leandro M.] Univ Fed Parana, Dept Zool, Lab Biol Comparada Hymenoptera, BR-81531980 Curitiba, Parana, Brazil. [Tierney, Simon M.; Wcislo, William T.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Santos, Leandro M.] Univ Fed Parana, Dept Zool, Programa Posgrad Entomol, BR-81531980 Curitiba, Parana, Brazil. RP Santos, LM (reprint author), Univ Fed Parana, Dept Zool, Lab Biol Comparada Hymenoptera, Caixa Postal 19020, BR-81531980 Curitiba, Parana, Brazil. EM megalopta@gmail.com; tierneys@si.edu; wcislow@si.edu RI Santos, Leandro/H-4364-2012; Tierney, Simon/H-2410-2015 OI Tierney, Simon/0000-0002-8812-6753 FU Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq); Ministerio da Ciencia e Tecnologia, Brazil; Smithsonian Tropical Research Institute (STRI); National Geographic Society Research and Exploration FX We are most grateful to Fatima Knoll, Gabriel A. R. Melo for their hospitality and assistance with fieldwork and Vitor A. Nardino (Taxon line - UFPR) for taking photographs. This work was supported by Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq), Ministerio da Ciencia e Tecnologia, Brazil by Masters Fellowship to LMS, an Earl S. Tupper Postdoctoral Fellowship from the Smithsonian Tropical Research Institute (STRI) awarded to SMT and a National Geographic Society Research and Exploration Grant to WTW and SMT, and general research funds from STRI to WTW. NR 17 TC 5 Z9 5 U1 0 U2 1 PU SOC BRASILEIRA ENTOMOLOGIA PI CURITIBA PA CAIXA POSTAL 19030, CURITIBA, PR 81531-980, BRAZIL SN 0085-5626 EI 1806-9665 J9 REV BRAS ENTOMOL JI Rev. Bras. Entomol. PD APR-JUN PY 2010 VL 54 IS 2 BP 332 EP 334 PG 3 WC Entomology SC Entomology GA 618UE UT WOS:000279380400018 ER PT J AU Clough, W AF Clough, Wayne TI Bi-Centennial SO SMITHSONIAN LA English DT Editorial Material C1 Smithsonian Inst, Washington, DC 20560 USA. RP Clough, W (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 APR PY 2010 VL 41 IS 1 BP 20 EP 20 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 573SK UT WOS:000275934900008 ER PT J AU Attrill, GDR Wills-Davey, MJ AF Attrill, G. D. R. Wills-Davey, M. J. TI Automatic Detection and Extraction of Coronal Dimmings from SDO/AIA Data SO SOLAR PHYSICS LA English DT Article DE Corona, quiet; Coronal mass ejections, low coronal signatures; Instrumentation and data management ID CME-RELATED DIMMINGS; 1997 MAGNETIC CLOUD; MASS EJECTION; EIT WAVES; SOLAR; EVENT; FLARE; RECONNECTION; SIGNATURE; REGIONS AB The volume of data anticipated from the Solar Dynamics Observatory/Atmospheric Imaging Assembly (SDO/AIA) highlights the necessity for the development of automatic-detection methods for various types of solar activity. Initially recognized in the 1970s, it is now well established that coronal dimmings are closely associated with coronal mass ejections (CMEs), and they are particularly noted as a reliable indicator of front-side (halo) CMEs, which can be difficult to detect in white-light coronagraph data. Existing work clearly demonstrates that several properties derived from the analysis of coronal dimmings can give useful information about the associated CME. The development and implementation of an automated coronal-dimming region detection and extraction algorithm removes visual observer bias, however unintentional, from the determination of physical quantities such as spatial location, area, and volume. This allows for reproducible, quantifiable results to be mined from very large data sets. The information derived may facilitate more reliable early space-weather detection, as well as offering the potential for conducting large-sample studies focused on determining the geo-effectiveness of CMEs, coupled with analysis of their associated coronal dimming signatures. In this paper we present examples of both simple and complex dimming events extracted using our algorithm, which will be run as a module for the SDO/Computer Vision Centre. Contrasting and well-studied events at both the minimum and maximum of solar cycle 23 are identified in Solar and Heliospheric Observatory/Extreme ultra-violet Imaging Telescope (SOHO/EIT) data. A more recent example extracted from Solar and Terrestrial Relations Observatory/Extreme Ultra-Violet Imager (STEREO/EUVI) data is also presented, demonstrating the potential for the anticipated application to SDO/AIA data. The detection part of our algorithm is based largely on the principle of operation of the NEMO software, namely the detection of significant variation in the statistics of the EUV image pixels (Podladchikova and Berghmans in Solar Phys. 228, 265 -aEuro parts per thousand 284, 2005). As well as running on historic data sets, the presented algorithm is capable of detecting and extracting coronal dimmings in near real-time. C1 [Attrill, G. D. R.; Wills-Davey, M. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Attrill, GDR (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM gattrill@cfa.harvard.edu FU NASA [NNX08BA97G] FX We sincerely thank the anonymous referee for suggestions that improved the description of the work presented here, as well as for helpful comments pertinent to the next phase of testing and development. We are grateful to E. Podladchikova, D. Bewsher, S. Saar, P. Grigis, and A. Davey for helpful discussions. We acknowledge NASA grant NNX08BA97G, which supported this work. NR 37 TC 12 Z9 13 U1 0 U2 2 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD APR PY 2010 VL 262 IS 2 BP 461 EP 480 DI 10.1007/s11207-009-9444-4 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 573JC UT WOS:000275908300015 ER PT J AU Liu, Q Zhang, DX Peterson, PM AF Liu, Q. Zhang, D. X. Peterson, P. M. TI Lemma micromorphological characters in the Chloridoideae (Poaceae) optimized on a molecular phylogeny SO SOUTH AFRICAN JOURNAL OF BOTANY LA English DT Article DE Character; Chloridoideae; Lemma micromorphology; Poaceae; Synapomorphies ID GRASS FAMILY POACEAE; EPIDERMAL FEATURES; GRAMINEAE; SEQUENCES; EVOLUTION; MELICA AB Eight lemma micromorphological characters of 83 taxa representing 61 genera in the Chloridoideae have been investigated using Scanning Electron Microscopy, including long cells, cork cells, stomata, bicellular microhairs, papillae, silica cells, microprickles, and macrohairs. Five new types of lemma micromorphological characters were reported here. Data for 27 taxa representing 19 genera from previous publications were also supplied to access the homology of lemma micromorphological characters for different groups through optimization onto a molecular cladogram. Given the optimization, five characters including long cells, cork cells, stomata, papillae, microprickles are of phylogenetic significance for supra-generic groups. Seven characters including straight outline long cells, crescent-shaped cork cells, absent stomata, absent papillae, dumb-bell-shaped silica cells, c-type microprickles, and papillate-base macrohairs may not be homologous, however, the enneapogonoid-type bicellular microhairs appeared as a synapomorphy for the Chloridoideae. (C) 2009 SAAB. Published by Elsevier B.V. All rights reserved. C1 [Liu, Q.; Zhang, D. X.] Chinese Acad Sci, S China Bot Garden, Key Lab Plant Resources Conservat & Sustainable U, Guangzhou 510650, Guangdong, Peoples R China. [Liu, Q.; Peterson, P. M.] Smithsonian Inst, Dept Bot, Washington, DC 20013 USA. RP Liu, Q (reprint author), Chinese Acad Sci, S China Bot Garden, Key Lab Plant Resources Conservat & Sustainable U, Guangzhou 510650, Guangdong, Peoples R China. EM liuqing@scib.ac.cn FU National Natural Science Foundation of China [30700043]; Key Laboratory of Plant Resources Conservation and Sustainable Utilization; Chinese Academy of Sciences [200922]; Smithsonian Institution by Chinese Government Scholarships [2008491004] FX This study was supported by the National Natural Science Foundation of China (30700043), Q. Liu was supported to visit to the Department of Botany, Key Laboratory of Plant Resources Conservation and Sustainable Utilization, Chinese Academy of Sciences (200922), and Smithsonian Institution by Chinese Government Scholarships (2008491004). We are indebted to staff of B, IBSC, K, KUN, LINN, P, PE, and US for loan specimens, to H.L. Bell and G. Hao for the discussion, and to Ms. X.Y. Hu for her help with SEM. The authors also thank two anonymous reviewers and editor Trevor Edwards for their valuable comments. NR 37 TC 9 Z9 12 U1 0 U2 8 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0254-6299 J9 S AFR J BOT JI S. Afr. J. Bot. PD APR PY 2010 VL 76 IS 2 BP 196 EP 209 DI 10.1016/j.sajb.2009.10.006 PG 14 WC Plant Sciences SC Plant Sciences GA 599HP UT WOS:000277902300004 ER PT J AU Wang, J Chaney, D AF Wang, Jun Chaney, Dan TI A re-examination of the type specimens of Yuania HC Sze 1953 and its junior synonym Russellites Mamay 1968 (Noeggerathiales) SO TAXON LA English DT Article DE Noeggerathiales; Permian; Russellites Mamay; synonym; Yuania Sze ID DISCINITES NOEGGERATHIALES; CHINA AB The noeggerathialean fossil names Yuania H.C. Sze and Russellites Mamay are shown to be synonymous, with the latter being the junior synonym of the former. Examination and re-illustration of the type material of both Yuania and Russellites shows that they are indistinguishable taxonomically. Both sets of material have pinnules with clasping bases and concave apices in which the veins converge but do not anastomose. Sze's original description of Yuania was incorrect in indicating that the leaves were petiolate and that the veins converged. Yuania may be the first plant taxon identified in the Permian floras of China and North America with vegetative and reproductive organs represented on both continents. C1 [Wang, Jun] Chinese Acad Sci, LPS, Nanjing Inst Geol & Palaeontol, Nanjing 210008, Peoples R China. [Chaney, Dan] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20506 USA. RP Wang, J (reprint author), Chinese Acad Sci, LPS, Nanjing Inst Geol & Palaeontol, Nanjing 210008, Peoples R China. EM jun.wang@nigpas.ac.cn FU Chinese Academy of Sciences [KZCX2-YW-105]; Chinese Natural Science Foundation [40572008, 40621062]; Ministry of Science and Technology of China [2006CB806400] FX We would like to acknowledge the Chinese Academy of Sciences (Project No. KZCX2-YW-105), Chinese Natural Science Foundation (Gr. No. 40572008,40621062), and the Major Basic Research Project (Grant No. 2006CB806400) of the Ministry of Science and Technology of China, for financial support. J. Wang would like to thank Dr. E.M. Friis for her kind help in checking the specimens housed in the Swedish Museum of Natural History, and Dr. John McNeill for his kind help with the terminology of nomenclature. NR 26 TC 5 Z9 5 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 APR PY 2010 VL 59 IS 2 BP 517 EP 524 PG 8 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA 582RW UT WOS:000276617400017 ER PT J AU Dorr, LJ AF Dorr, Laurence J. TI IN MEMORIAM ARMAND RAKOTOZAFY (1932-2009): MALAGASY BOTANIST AND HERBARIUM CURATOR SO TAXON LA English DT Biographical-Item C1 Smithsonian Inst, Washington, DC 20560 USA. RP Dorr, LJ (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 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 APR PY 2010 VL 59 IS 2 BP 670 EP 671 PG 2 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA 582RW UT WOS:000276617400033 ER PT J AU Derryberry, E Claramunt, S Chesser, RT Aleixo, A Cracraft, J Moyle, RG Brumfield, RT AF Derryberry, Elizabeth Claramunt, Santiago Chesser, R. Terry Aleixo, Alexandre Cracraft, Joel Moyle, Robert G. Brumfield, Robb T. TI Certhiasomus, a new genus of woodcreeper (Aves: Passeriformes: Dendrocolaptidae) SO ZOOTAXA LA English DT Article DE Deconychura longicauda; Deconychura stictolaema; Certhiasomus stictolaemus; morphometric heterogeneity; phylogeny; ranking criteria ID MODEL SELECTION; PHYLOGENETICS; BIOGEOGRAPHY; SYSTEMATICS; ALLOMETRY; INFERENCE; EVOLUTION; SHAPE AB Phylogenetic analysis of the family Dendrocolaptidae (Aves: Passeriformes) indicates that the two species traditionally placed in the genus Deconychura are not sister taxa. Certhiasomus, a new genus of woodcreeper, is described for one of these species, C. stictolaemus. C1 [Derryberry, Elizabeth; Claramunt, Santiago; Brumfield, Robb T.] Louisiana State Univ, Museum Nat Sci, Baton Rouge, LA 70803 USA. [Derryberry, Elizabeth; Claramunt, Santiago; Brumfield, Robb T.] Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA. [Chesser, R. Terry] Smithsonian Inst, USGS Patuxent Wildlife Res Ctr, Natl Museum Nat Hist, Washington, DC 20013 USA. [Aleixo, Alexandre] Museu Paraense Emilio Goeldi, BR-66040170 Belem, Para, Brazil. [Cracraft, Joel] Amer Museum Nat Hist, Dept Ornithol, New York, NY 10024 USA. [Moyle, Robert G.] Biodivers Res Ctr, Lawrence, KS 66045 USA. [Moyle, Robert G.] Dept Ecol & Evolutionary Biol, Lawrence, KS 66045 USA. RP Derryberry, E (reprint author), Louisiana State Univ, Museum Nat Sci, Baton Rouge, LA 70803 USA. RI Aleixo, Alexandre/L-3135-2013; Derryberry, Elizabeth/C-2396-2011; OI Brumfield, Robb/0000-0003-2307-0688 FU NSF [DBI-0400797, DEB-0543562]; AToL [EAR-0228693]; CNPq (Brazil) [476212/2007-3] FX We are grateful to the following people and institutions for providing tissue samples: John Bates and David Willard, Bird Division, Field Museum of Natural History; and Nate Rice, Ornithology, The Academy of Natural Sciences of Philadelphia. We thank Donna Dittmann, George Barrowclough and Paul Sweet for assistance in acquiring tissues. We are also grateful to Richard Banks, Al Gardner, Roy McDiarmid, and the LSU bird group for comments and discussion concerning the manuscript. This research was supported in part by NSF grants DBI-0400797 and DEB-0543562 to RTB, AToL EAR-0228693 to JC, and CNPq (Brazil) grant 476212/2007-3 to AA. NR 30 TC 5 Z9 6 U1 0 U2 0 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD APR 1 PY 2010 IS 2416 BP 44 EP 50 PG 7 WC Zoology SC Zoology GA 576PZ UT WOS:000276159300002 ER PT J AU Derryberry, E Claramunt, S O'Quin, KE Aleixo, A Chesser, RT Remsen, JV Brumfield, RT AF Derryberry, Elizabeth Claramunt, Santiago O'Quin, Kelly E. Aleixo, Alexandre Chesser, R. Terry Remsen, J. V., Jr. Brumfield, Robb T. TI Pseudasthenes, a new genus of ovenbird (Aves: Passeriformes: Furnariidae) SO ZOOTAXA LA English DT Article DE Asthenes; Oreophylax; Schizoeaca; phylogeny; taxonomy ID BAYESIAN PHYLOGENETIC INFERENCE; NEST ARCHITECTURE; EVOLUTION; SYSTEMATICS; SELECTION; MRBAYES AB Phylogenetic analysis of the family Furnariidae (Aves: Passeriformes) indicates that the genus Asthenes is polyphyletic, consisting of two groups that are not sister taxa. Pseudasthenes, a new genus of ovenbird, is described for one of these groups. The four species included in the new genus, formerly placed in Asthenes, are P. humicola, P. patagonica, P. steinbachi, and P. cactorum. C1 [Derryberry, Elizabeth; Claramunt, Santiago; O'Quin, Kelly E.; Remsen, J. V., Jr.; Brumfield, Robb T.] Louisiana State Univ, Museum Nat Sci, Baton Rouge, LA 70803 USA. [Derryberry, Elizabeth; Claramunt, Santiago; O'Quin, Kelly E.; Remsen, J. V., Jr.; Brumfield, Robb T.] Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA. [O'Quin, Kelly E.] Univ Maryland, Behav Ecol Evolut Systemat Program, College Pk, MD 20742 USA. [Aleixo, Alexandre] Museu Paraense Emilio Goeldi, BR-66040170 Belem, Para, Brazil. [Chesser, R. Terry] Smithsonian Inst, USGS Patuxent Wildlife Res Ctr, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Derryberry, E (reprint author), Louisiana State Univ, Museum Nat Sci, Baton Rouge, LA 70803 USA. RI Aleixo, Alexandre/L-3135-2013; Derryberry, Elizabeth/C-2396-2011; OI Brumfield, Robb/0000-0003-2307-0688 FU NSF [DBI-0400797, DEB-0543562] FX We are grateful to the following people and institutions for providing tissue samples: George Barrowclough and Paul Sweet, Department of Ornithology, American Museum of Natural History; Colecao Ornitologica do Departamento de Zoologia da Universidade Federal de Minas Gerais; John Bates and David Willard, Bird Division, Field Museum of Natural History; Instituto de Ciencias Naturales, Universidad Nacional de Colombia; C. Daniel Cadena, Universidad de los Andes, Bogota; Fabricio Santos, Laboratorio de Biodiversidade e Evolucao Molecular da Universidade Federal de Minas Gerais. We thank Donna Dittmann and James Dean for assistance in acquiring tissues, Andres Cuervo for making a special effort to collect sequences of Schizoeaca perijana, and Richard Banks and Storrs Olson for taxonomic advice. Brett Whitney, Neal Woodman, and Richard Banks made many helpful comments on an earlier draft of this manuscript. This research was supported in part by NSF grants DBI-0400797 and DEB-0543562 to RTB. Any use of trade, product, or firm names is for descriptive purposes only and does not imply endorsement by the U.S. Government. NR 30 TC 7 Z9 8 U1 0 U2 0 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD APR 1 PY 2010 IS 2416 BP 61 EP 68 PG 8 WC Zoology SC Zoology GA 576PZ UT WOS:000276159300004 ER PT J AU Spudis, PD Bussey, DBJ Baloga, SM Butler, BJ Carl, D Carter, LM Chakraborty, M Elphic, RC Gillis-Davis, JJ Goswami, JN Heggy, E Hillyard, M Jensen, R Kirk, RL LaVallee, D McKerracher, P Neish, CD Nozette, S Nylund, S Palsetia, M Patterson, W Robinson, MS Raney, RK Schulze, RC Sequeira, H Skura, J Thompson, TW Thomson, BJ Ustinov, EA Winters, HL AF Spudis, P. D. Bussey, D. B. J. Baloga, S. M. Butler, B. J. Carl, D. Carter, L. M. Chakraborty, M. Elphic, R. C. Gillis-Davis, J. J. Goswami, J. N. Heggy, E. Hillyard, M. Jensen, R. Kirk, R. L. LaVallee, D. McKerracher, P. Neish, C. D. Nozette, S. Nylund, S. Palsetia, M. Patterson, W. Robinson, M. S. Raney, R. K. Schulze, R. C. Sequeira, H. Skura, J. Thompson, T. W. Thomson, B. J. Ustinov, E. A. Winters, H. L. TI Initial results for the north pole of the Moon from Mini-SAR, Chandrayaan-1 mission SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID LUNAR SOUTH-POLE; RADAR EXPERIMENT; ICE DEPOSITS; MERCURY; SURFACE; IMAGES AB We present new polarimetric radar data for the sur face of the north pole of the Moon acquired with the Mini-SAR experiment onboard India's Chandrayaan-1 spacecraft. Between mid-February and mid-April, 2009, Mini-SAR mapped more than 95% of the areas polewards of 80 latitude at a resolution of 150 meters. The north polar region displays backscatter properties typical for the Moon, with circular polarization ratio (CPR) values in the range of 0.1-0.3, increasing to over 1.0 for young primary impact craters. These higher CPR values likely reflect surface roughness associated with these fresh features. In contrast, some craters in this region show elevated CPR in their interiors, but not exterior to their rims. Almost all of these features are in permanent sun shadow and correlate with proposed locations of polar ice modeled on the basis of Lunar Prospector neutron data. These relations are consistent with deposits of water ice in these craters. Citation: Spudis, P. D., et al. (2010), Initial results for the north pole of the Moon from Mini-SAR, Chandrayaan-1 mission, Geophys. Res. Lett., 37, L06204, doi: 10.10292009GL042259. C1 [Spudis, P. D.; Nozette, S.] Lunar & Planetary Inst, Houston, TX 77058 USA. [Bussey, D. B. J.; Carl, D.; Hillyard, M.; Jensen, R.; LaVallee, D.; McKerracher, P.; Neish, C. D.; Nylund, S.; Patterson, W.; Raney, R. K.; Schulze, R. C.; Sequeira, H.; Skura, J.; Thomson, B. J.; Winters, H. L.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Baloga, S. M.] Proxemy Res Inc, Laytonville, MD 20882 USA. [Butler, B. J.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Carter, L. M.] Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. [Chakraborty, M.] ISRO, Ctr Space Applicat, Ahmadabad 380015, Gujarat, India. [Elphic, R. C.] NASA, Ames Res Ctr, Planetary Syst Branch, Moffett Field, CA 94035 USA. [Gillis-Davis, J. J.] Univ Hawaii, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. [Goswami, J. N.] Phys Res Lab, Ahmadabad 380009, Gujarat, India. [Heggy, E.; Thompson, T. W.; Ustinov, E. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Kirk, R. L.] US Geol Survey, Astrogeol Program, Flagstaff, AZ 86001 USA. [Palsetia, M.] Vexcel Inc, Boulder, CO 80301 USA. [Robinson, M. S.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. RP Spudis, PD (reprint author), Lunar & Planetary Inst, 3600 Bay Area Blvd, Houston, TX 77058 USA. EM spudis@lpi.usra.edu RI Carter, Lynn/D-2937-2012; Neish, Catherine/G-6321-2012; Heggy, Essam/E-8250-2013; Ustinov, Eugene/D-1350-2015 OI Heggy, Essam/0000-0001-7476-2735; Ustinov, Eugene/0000-0003-0227-4286 NR 27 TC 74 Z9 78 U1 2 U2 24 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD MAR 31 PY 2010 VL 37 AR L06204 DI 10.1029/2009GL042259 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 578SB UT WOS:000276314400002 ER PT J AU Collin, R Rolan, E AF Collin, Rachel Rolan, Emilio TI Bostrycapulus heteropoma n. sp and Bostrycapulus tegulicius (Gastropoda: Calyptraeidae) from Western Africa SO VELIGER LA English DT Article ID MARINE GASTROPOD; CREPIDULA; PHYLOGENY; RADIATION; CONUS AB Spiny slipper shells in the genus Bostrycapulus range worldwide in tropical and temperate oceans. Owing to the scarcity of samples that retain the defining characteristics of the genus, the species from tropical Africa and the Indo-Pacific are poorly known. Here we present data showing that samples of Bostrycapulus from the Cape Verde Islands and Senegal are distinct from each other and distinct from other known Bostrycapulus species. These two species can be distinguished from each other by the unique caplike protoconch found on the shells from Senegal and the coiled globose protoconchs typical of direct-developing species on the shells from the Cape Verde Islands. Genetically, samples from Senegal and the Cape Verde Islands are distinct. DNA sequences from Senegal are very similar to those of Bostrycapulus odites, which occurs in the South Atlantic (South Africa, Argentina, and Brazil) while those from Cape Verde are closest to Bostrycapulus aculeatus from Florida. The name Bostrycapulus tegulicius is available, and the single existing protoconch on the types in the Museum National d'Histoire Naturelle, Paris, appears to match those from the Cape Verde Islands. Subtle variation in protoconch size and shape throughout the Cape Verde Islands suggests that there may be more than a single species in the archipelago. Unfortunately, too little material is available to rule out intraspecific variation or to support the description of additional new species from the Cape Verde Islands. Here, we augment the original description of B. tegulicius and describe the unique new species Bostrycapulus heteropoma n. sp. from Senegal. C1 [Collin, Rachel] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Rolan, Emilio] Museo Hist Nat, Santiago De Compostela 17582, Spain. RP Collin, R (reprint author), STRI, MRC 0580 08, Unit 9100, Box 0948, Dpo, AA 34002 USA. EM collinr@si.edu RI Collin, Rachel/G-2001-2010 NR 18 TC 0 Z9 0 U1 1 U2 2 PU CALIFORNIA MALACOZOOLOGICAL SOC INC PI SANTA BARBARA PA SANTA BARBARA MUSEUM NATURAL HISTORY, 2559 PUESTA DEL SOL RD, SANTA BARBARA, CA 93105 USA SN 0042-3211 J9 VELIGER JI Veliger PD MAR 31 PY 2010 VL 51 IS 1 BP 8 EP 14 PG 7 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA 581JY UT WOS:000276519900002 ER PT J AU Harasewych, MG Pastorino, G AF Harasewych, M. G. Pastorino, Guido TI Trophonella (Gastropoda: Muricidae), a New Genus from Antarctic Waters, with the Description of a New Species SO VELIGER LA English DT Article ID PHYLOGENETIC ANALYSIS; NEOGASTROPODA AB The new genus Trophonella is described from the outer shelf and upper continental slope of Antarctica and islands within the Antarctic Convergence. Four previously known species that had been attributed to the genus Trophon (Trophon scotianus Powell, 1951; T echinolamellatus Powell, 1951; T enderbyensis Powell, 1958; and T eversoni Houart, 1997) are included in Trophonella, as is one new species (Trophonella rugosolamellata) described herein. Trophonella resembles Trophon in gross shell morphology: the members of both genera have large, globose shells, paucispiral protoconchs, prominent axial lamellae, and short siphonal canals. Trophonella differs from Trophon in having shells with evenly rounded whorls that lack a well-defined shoulder; rachidian teeth with distinctive, broadly triangular central cusps, but that lack the marginal cusps of Trophon; characteristic spherical accessory salivary glands; and a circumpapillar fold on the penis that is absent in Trophon. Relationships of the genera Trophon and Trophonella, as well as of the subfamily Trophoninae are reexamined by supplementing the data matrix of Kool (1993b, Table 3) with data for additional taxa. Results support the segregation of Trophonella from Trophon at the generic level. Based on the relationships of the type species of their respective nominotypical genera, Trophoninae is either the sister taxon of a narrowly circumscribed Ocenebrinae, or both are part of a larger clade. A better resolved phylogeny containing a much broader sampling of the more than 50 genus-level taxa that have been attributed to these two subfamilies will be required in order to delineate more precisely the membership of the clade and to identify its diagnostic synapomorphies. C1 [Harasewych, M. G.] Smithsonian Inst, Dept Invertebrate Zool, Natl Museum Nat Hist, MRC 163, Washington, DC 20013 USA. [Pastorino, Guido] Museo Argentino Ciencias Nat Bernardino Rivadavia, Buenos Aires, DF, Argentina. RP Harasewych, MG (reprint author), Smithsonian Inst, Dept Invertebrate Zool, Natl Museum Nat Hist, MRC 163, POB 37012, Washington, DC 20013 USA. EM Harasewych@si.edu; gpastorino@macn.gov.ar FU Consejo Nacional de Investigaciones Cientificas y Tecnicas (CONICET), Argentina; NSF-USAP United States Antarctic [ANTO636408]; Conchologists of America; Walter E. Sage Memorial Award FX We thank the following curators and collection managers for access to specimens in their collections: K. Way (NHM); A. Waren (NHRM); P. Bouchet and V. Heros (MNHN); P. Mikelsen (AMNH); B. Hausdorf (ZMH), A. Tablado (MACN); C. Ituarte; (MLP) and R. Janssen (SM); P. Arnaud, Endoume, France. This work was supported by a grant from the Consejo Nacional de Investigaciones Cientificas y Tecnicas (CONICET), Argentina, which enabled the junior author to work in the Division of Mollusks, United States National Museum of Natural History, Smithsonian Institution. Additional support was provided in part by a Research Award from the NSF-USAP United States Antarctic Program Grant [ANTO636408] and a grant-in-aid from the Conchologists of America and the Walter E. Sage Memorial Award. We are grateful to Dr. Yu. Kantor for his many helpful and insightful comments during the course of this research, and to Roland Houart and Dr. Geerat Vermeij for their helpful reviews. NR 23 TC 4 Z9 5 U1 1 U2 1 PU CALIFORNIA MALACOZOOLOGICAL SOC INC PI SANTA BARBARA PA SANTA BARBARA MUSEUM NATURAL HISTORY, 2559 PUESTA DEL SOL RD, SANTA BARBARA, CA 93105 USA SN 0042-3211 J9 VELIGER JI Veliger PD MAR 31 PY 2010 VL 51 IS 1 BP 85 EP 103 PG 19 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA 581JY UT WOS:000276519900008 ER PT J AU Suutari, M Majaneva, M Fewer, DP Voirin, B Aiello, A Friedl, T Chiarello, AG Blomster, J AF Suutari, Milla Majaneva, Markus Fewer, David P. Voirin, Bryson Aiello, Annette Friedl, Thomas Chiarello, Adriano G. Blomster, Jaanika TI Molecular evidence for a diverse green algal community growing in the hair of sloths and a specific association with Trichophilus welckeri (Chlorophyta, Ulvophyceae) SO BMC EVOLUTIONARY BIOLOGY LA English DT Article ID PHYLOGENETIC TREES; TREBOUXIOPHYCEAE; INFERENCE; MRBAYES; CLOCK; DNA AB Background: Sloths are slow-moving arboreal mammals inhabiting tropical rainforests in Central and South America. The six living species of sloths are occasionally reported to display a greenish discoloration of their pelage. Trichophilus welckeri, a green algal species first described more than a century ago, is widely believed to discolor the animals fur and provide the sloth with effective camouflage. However, this phenomenon has not been explored in any detail and there is little evidence to substantiate this widely held opinion. Results: Here we investigate the genetic diversity of the eukaryotic community present in fur of all six extant species of sloth. Analysis of 71 sloth hair samples yielding 426 partial 18S rRNA gene sequences demonstrates a diverse eukaryotic microbial assemblage. Phylogenetic analysis reveals that sloth fur hosts a number of green algal species and suggests that acquisition of these organisms from the surrounding rainforest plays an important role in the discoloration of sloth fur. However, an alga corresponding to the morphological description of Trichophilus welckeri was found to be frequent and abundant on sloth fur. Phylogenetic analysis demonstrated the retention of this alga on the fur of sloths independent of geographic location. Conclusions: These results demonstrate a unique diverse microbial eukaryotic community in the fur of sloths from Central and South America. Our analysis streghtens the case for symbiosis between sloths and Trichophilus welckeri. C1 [Suutari, Milla; Blomster, Jaanika] Univ Helsinki, Dept Environm Sci, FIN-00014 Helsinki, Finland. [Majaneva, Markus] Tvarminne Zool Stn, FIN-10900 Hango, Finland. [Fewer, David P.] Univ Helsinki, Dept Food & Environm Sci, FIN-00014 Helsinki, Finland. [Voirin, Bryson] Max Planck Inst Ornithol, D-78315 Radolfzell am Bodensee, Germany. [Aiello, Annette] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Friedl, Thomas] Univ Gottingen, Abt Expt Phykol & Sammlung Algenkulturen, Albrecht von Haller Inst Pflanzenwissensch, D-37073 Gottingen, Germany. [Chiarello, Adriano G.] Pontificia Univ Catolica Minas Gerais, Programa Posgrad Zool Vertebrados, BR-30535610 Belo Horizonte, MG, Brazil. RP Blomster, J (reprint author), Univ Helsinki, Dept Environm Sci, POB 65, FIN-00014 Helsinki, Finland. EM jaanika.blomster@helsinki.fi RI Fewer, David/A-8704-2008; OI Fewer, David/0000-0003-3978-4845; Chiarello, Adriano/0000-0003-1914-5480 FU Linnean Society of London; University of Helsinki; Emil Aaltonen Foundation FX We are grateful to Roland Kays (New York State Museum) for his help, encouragement and advice at the start of the project. We also thank him for his help in sample collection. The following people helped us with searching for sloths, catching them or provided sloth hair samples: Ingrun Vogel (Association Kwata, French Guiana), Jennifer and Jeanine Licare (Organization Kids Saving the Rainforest, Costa Rica), Kirsi Pynnonen (Helsinki Zoo), Bernardo B. Dias, Bonifacio De Leon, Luis A. Dias, Christie Riehl and Marcus Martinez. Tatyana Darienko and Nataliya Rybalka performed microscopic analyses on many hair samples. We are very grateful for their help. The Museu de Biologia Mello Leitao and Instituto de Pesquisas da Mata Atlantica helped with logistics in collecting the samples in Brazil. The Brazilian sloth hair samples were exported with the permission number 0131864 BR and the samples from Panama were exported with Autoridad Nacional del Ambiente (ANAM) permits DNPN-01-2001 and SEX/A-73-06. This work was supported by the Linnean Society of London, the University of Helsinki Chancellors Travel Grants and Emil Aaltonen Foundation. NR 36 TC 23 Z9 23 U1 11 U2 73 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 MAR 30 PY 2010 VL 10 AR 86 DI 10.1186/1471-2148-10-86 PG 12 WC Evolutionary Biology; Genetics & Heredity SC Evolutionary Biology; Genetics & Heredity GA 588CS UT WOS:000277045100001 PM 20353556 ER PT J AU Diefendorf, AF Mueller, KE Wing, SL Koch, PL Freeman, KH AF Diefendorf, Aaron F. Mueller, Kevin E. Wing, Scott. L. Koch, Paul L. Freeman, Katherine H. TI Global patterns in leaf C-13 discrimination and implications for studies of past and future climate SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE biogeochemistry; ecophysiology; fractionation; PETM ID CARBON-ISOTOPE DISCRIMINATION; THERMAL MAXIMUM; STABLE-ISOTOPES; ORGANIC-MATTER; PLANTS; PHOTOSYNTHESIS; TERRESTRIAL; BOUNDARY; WATER AB Fractionation of carbon isotopes by plants during CO2 uptake and fixation (Delta(leaf)) varies with environmental conditions, but quantitative patterns of Delta(leaf) across environmental gradients at the global scale are lacking. This impedes interpretation of variability in ancient terrestrial organic matter, which encodes climatic and ecological signals. To address this problem, we converted 3,310 published leaf Alpha values into mean Delta(leaf) values for 334 woody plant species at 105 locations (yielding 570 species-site combinations) representing a wide range of environmental conditions. Our analyses reveal a strong positive correlation between Delta(leaf) and mean annual precipitation (MAP; R-2 = 0.55), mirroring global trends in gross primary production and indicating stomatal constraints on leaf gas-exchange, mediated by water supply, are the dominant control of Delta(leaf) at large spatial scales. Independent of MAP, we show a lesser, negative effect of altitude on Delta(leaf) and minor effects of temperature and latitude. After accounting for these factors, mean Delta(leaf) of evergreen gymnosperms is lower (by 1-2.7%) than for other woody plant functional types (PFT), likely due to greater leaf-level water-use efficiency. Together, environmental and PFT effects contribute to differences in mean Delta(leaf) of up to 6% between biomes. Coupling geologic indicators of ancient precipitation and PFT (or biome) with modern Delta(leaf) patterns has potential to yield more robust reconstructions of atmospheric delta C-13 values, leading to better constraints on past greenhouse-gas perturbations. Accordingly, we estimate a 4.6% decline in the delta C-13 of atmospheric CO2 at the onset of the Paleocene-Eocene Thermal Maximum, an abrupt global warming event similar to 55.8 Ma. C1 [Diefendorf, Aaron F.; Freeman, Katherine H.] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. [Mueller, Kevin E.] Penn State Univ, Intercoll Degree Program Ecol, University Pk, PA 16802 USA. [Wing, Scott. L.] Natl Museum Nat Hist, Dept Paleobiol, Smithsonian Inst, Washington, DC 20013 USA. [Koch, Paul L.] Univ Calif Santa Cruz, Dept Earth & Planetary Sci, Santa Cruz, CA 95064 USA. RP Diefendorf, AF (reprint author), Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. EM aaron.diefendorf@gmail.com RI Freeman, Katherine/H-5140-2011; OI Freeman, Katherine/0000-0002-3350-7671; Mueller, Kevin/0000-0002-0739-7472; Wing, Scott/0000-0002-2954-8905 FU National Science Foundation [EAR-0844212, DGE-9972759]; Penn State Biogeochemical Research Initiative for Education (BRIE); Department of Energy Graduate Research Environmental Fellowship (GREF) FX We thank the editors and reviewers for helpful comments. We thank Josh Dorin, Heather Graham, and Clayton Magill for data collection assistance. We also thank David Williams for providing data. This research was supported by the National Science Foundation Grant EAR-0844212 (to K. H. F.), fellowship awards from the Penn State Biogeochemical Research Initiative for Education (BRIE) funded by National Science Foundation Integrative Graduate Education and Research Traineeship (IGERT) Grant DGE-9972759 (to A. F. D. and K. E. M.), and a Department of Energy Graduate Research Environmental Fellowship (GREF) award (to K. E. M.). NR 25 TC 211 Z9 225 U1 15 U2 137 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD MAR 30 PY 2010 VL 107 IS 13 BP 5738 EP 5743 DI 10.1073/pnas.0910513107 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 576QA UT WOS:000276159500011 PM 20231481 ER PT J AU Scott, JJ Budsberg, KJ Suen, G Wixon, DL Balser, TC Currie, CR AF Scott, Jarrod J. Budsberg, Kevin J. Suen, Garret Wixon, Devin L. Balser, Teri C. Currie, Cameron R. TI Microbial Community Structure of Leaf-Cutter Ant Fungus Gardens and Refuse Dumps SO PLOS ONE LA English DT Article ID PHOSPHOLIPID FATTY-ACID; ATTA SEXDENS RUBROPILOSA; CUTTING ANTS; GROWING ANTS; SOIL; BACTERIA; FOREST; NESTS; POPULATION; COLOMBICA AB Background: Leaf-cutter ants use fresh plant material to grow a mutualistic fungus that serves as the ants' primary food source. Within fungus gardens, various plant compounds are metabolized and transformed into nutrients suitable for ant consumption. This symbiotic association produces a large amount of refuse consisting primarily of partly degraded plant material. A leaf-cutter ant colony is thus divided into two spatially and chemically distinct environments that together represent a plant biomass degradation gradient. Little is known about the microbial community structure in gardens and dumps or variation between lab and field colonies. Methodology/Principal Findings: Using microbial membrane lipid analysis and a variety of community metrics, we assessed and compared the microbiota of fungus gardens and refuse dumps from both laboratory-maintained and field-collected colonies. We found that gardens contained a diverse and consistent community of microbes, dominated by Gram-negative bacteria, particularly gamma-Proteobacteria and Bacteroidetes. These findings were consistent across lab and field gardens, as well as host ant taxa. In contrast, dumps were enriched for Gram-positive and anaerobic bacteria. Broad-scale clustering analyses revealed that community relatedness between samples reflected system component (gardens/dumps) rather than colony source (lab/field). At finer scales samples clustered according to colony source. Conclusions/Significance: Here we report the first comparative analysis of the microbiota from leaf-cutter ant colonies. Our work reveals the presence of two distinct communities: one in the fungus garden and the other in the refuse dump. Though we find some effect of colony source on community structure, our data indicate the presence of consistently associated microbes within gardens and dumps. Substrate composition and system component appear to be the most important factor in structuring the microbial communities. These results thus suggest that resident communities are shaped by the plant degradation gradient created by ant behavior, specifically their fungiculture and waste management. C1 [Scott, Jarrod J.; Budsberg, Kevin J.; Suen, Garret; Balser, Teri C.; Currie, Cameron R.] Univ Wisconsin, US DOE, Great Lakes Bioenergy Res Ctr, Madison, WI 53706 USA. [Scott, Jarrod J.; Suen, Garret; Currie, Cameron R.] Univ Wisconsin, Dept Bacteriol, Madison, WI 53706 USA. [Scott, Jarrod J.; Currie, Cameron R.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Budsberg, Kevin J.; Balser, Teri C.] Univ Wisconsin, Dept Soil Sci, Madison, WI 53706 USA. [Wixon, Devin L.] Univ Wisconsin, Dept Bot, Madison, WI 53706 USA. RP Scott, JJ (reprint author), Univ Wisconsin, US DOE, Great Lakes Bioenergy Res Ctr, Madison, WI 53706 USA. EM currie@bact.wisc.edu OI Suen, Garret/0000-0002-6170-711X FU National Science Foundation [DEB-0747002, MCB-0702025, MCB-0731822]; DOE Great Lakes Bioenergy Research Center [DE-FC02-07ER64494] FX This work was funded by the National Science Foundation [grants DEB-0747002 (to CRC), MCB-0702025 (to CRC and TCB), and MCB-0731822 (to CRC)] and the DOE Great Lakes Bioenergy Research Center (DOE BER Office of Science DE-FC02-07ER64494, to (CRC)). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 61 TC 26 Z9 27 U1 2 U2 60 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 MAR 29 PY 2010 VL 5 IS 3 AR e9922 DI 10.1371/journal.pone.0009922 PG 12 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 576QZ UT WOS:000276163100015 PM 20360970 ER PT J AU Capogrosso-Sansone, B Trefzger, C Lewenstein, M Zoller, P Pupillo, G AF Capogrosso-Sansone, B. Trefzger, C. Lewenstein, M. Zoller, P. Pupillo, G. TI Quantum Phases of Cold Polar Molecules in 2D Optical Lattices SO PHYSICAL REVIEW LETTERS LA English DT Article ID ISING-MODEL; GAS AB We study the quantum phases of hard-core bosonic polar molecules on a two-dimensional square lattice interacting via repulsive dipole-dipole interactions. In the limit of small tunneling, we find evidence for a devil's staircase, where Mott solids appear at rational fillings of the lattice. For finite tunneling, we establish the existence of extended regions of parameters where the ground state is a supersolid, obtained by doping the solids either with particles or vacancies. We discuss the effects of finite temperature and finite-size confining potentials as relevant to experiments. C1 [Capogrosso-Sansone, B.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. [Trefzger, C.; Lewenstein, M.] ICREA, Barcelona 08860, Spain. [Trefzger, C.; Lewenstein, M.] ICFO, Barcelona 08860, Spain. [Zoller, P.; Pupillo, G.] Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria. [Zoller, P.; Pupillo, G.] IQOQI, A-6020 Innsbruck, Austria. RP Capogrosso-Sansone, B (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RI Zoller, Peter/O-1639-2014; Lewenstein, Maciej/I-1337-2014 OI Zoller, Peter/0000-0003-4014-1505; Lewenstein, Maciej/0000-0002-0210-7800 FU EU [STREP FP7-ICT-2007-C]; Spanish MEC [FIS2008-00784] FX EU (STREP FP7-ICT-2007-C, NAME-QUAM), and the Spanish MEC (FIS2008-00784, QOIT). NR 39 TC 139 Z9 139 U1 1 U2 15 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 EI 1079-7114 J9 PHYS REV LETT JI Phys. Rev. Lett. PD MAR 26 PY 2010 VL 104 IS 12 AR 125301 DI 10.1103/PhysRevLett.104.125301 PG 4 WC Physics, Multidisciplinary SC Physics GA 575MY UT WOS:000276072400025 PM 20366541 ER PT J AU Akre, KL Ryan, MJ AF Akre, Karin L. Ryan, Michael J. TI Complexity Increases Working Memory for Mating Signals SO CURRENT BIOLOGY LA English DT Article ID FEMALE MATE CHOICE; TUNGARA FROGS; PHYSALAEMUS-PUSTULOSUS; RECEIVER PSYCHOLOGY; ADVERTISEMENT CALLS; EXPERIENCE; SONG; INFORMATION; RESPONSES; BEHAVIOR AB Females often prefer to mate with males who produce complex signals [1-3]. It is not clear why they do so. Females might prefer complexity if it predicts mate quality [4-6], or signals might evolve complexity to exploit females' sensory or cognitive biases [6-9]. We tested whether complexity increases active time, the period over which a signal influences a receiver's response to that signal. Mating signals are often ephemeral, yet their active time has largely been ignored. Here we demonstrate that signal complexity influences active time in tungara frogs. Male advertisement calls consist of frequency sweeps (whines) followed by 0-7 high-frequency bursts (chucks). Females preferentially approach complex (whines with chucks) over simple (whines alone) calls but do not consistently prefer greater complexity [10], so the function of multiple chucks has been uncertain. We found that females remember which speaker previously broadcast complex calls when choosing between simple calls broadcast after a delay. This effect occurred for calls with multiple chucks, but not with single chucks. Neither motivation nor orientation behavior differed with chuck number, suggesting that results are due to differential memory. Thus, female memory could favor the evolution of increasing signal complexity through sexual selection. C1 [Akre, Karin L.; Ryan, Michael J.] Univ Texas Austin, Sect Integrat Biol, Austin, TX 78712 USA. [Ryan, Michael J.] Smithsonian Trop Res Inst, Balboa, Panama. RP Akre, KL (reprint author), Univ Texas Austin, Sect Integrat Biol, 1 Univ Stn C0930, Austin, TX 78712 USA. EM kakre@mail.utexas.edu FU STRI Short-Term A. Stanley Rand Memorial Fellowship; National Science Foundation [NSF IOB 0544096] FX We thank S. Rand, X. Bernal, W. Wilczynski, W. Wcislo, M.J. West-Eberhard, K. Hoke, H. Farris, M. Bee, J. Schwartz, and M. Domjan for valuable conversation regarding this research. We are grateful to L. Bonachea, R. Taylor, A. Baugh, and I. Chiver for help with fieldwork and to STRI for logistical support. Funding was provided to K.L.A. by a STRI Short-Term A. Stanley Rand Memorial Fellowship and a National Science Foundation Graduate Research Fellowship. Other funding was provided by a National Science Foundation grant to M.J.R. (NSF IOB 0544096). This manuscript was greatly improved by comments from J. Hutchinson and five anonymous reviewers. NR 32 TC 25 Z9 25 U1 3 U2 14 PU CELL PRESS PI CAMBRIDGE PA 600 TECHNOLOGY SQUARE, 5TH FLOOR, CAMBRIDGE, MA 02139 USA SN 0960-9822 EI 1879-0445 J9 CURR BIOL JI Curr. Biol. PD MAR 23 PY 2010 VL 20 IS 6 BP 502 EP 505 DI 10.1016/j.cub.2010.01.021 PG 4 WC Biochemistry & Molecular Biology; Cell Biology SC Biochemistry & Molecular Biology; Cell Biology GA 574TT UT WOS:000276017300023 PM 20206525 ER PT J AU Oberg, KI Garrod, RT Fayolle, EC van Dishoeck, EF Linnartz, H AF Oberg, Karin I. Garrod, Robin T. Fayolle, Edith C. van Dishoeck, Ewine F. Linnartz, Harold TI Ice photochemistry revisited: Complex molecule formation during UV irradiation of ices SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. NR 0 TC 0 Z9 0 U1 1 U2 8 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD MAR 21 PY 2010 VL 239 MA 278-PHYS PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA V21DW UT WOS:000208189304276 ER PT J AU Jonsson, P Groves, BA Cox, TJ AF Jonsson, Patrik Groves, Brent A. Cox, T. J. TI High-resolution panchromatic spectral models of galaxies including photoionization and dust SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE radiative transfer; methods: numerical; dust; extinction; galaxies: spiral; infrared: galaxies; ultraviolet: galaxies ID PARTICLE HYDRODYNAMICS SIMULATIONS; CONTINUUM RADIATIVE-TRANSFER; STARBURST GALAXIES; STAR-FORMATION; ENERGY-DISTRIBUTION; INFRARED-EMISSION; SPIRAL GALAXIES; MULTIPLE-SCATTERING; INTERSTELLAR DUST; TRANSFER CODE AB An updated version of the dust radiation-transfer code sunrise, including models for star-forming regions and a self-consistent calculation of the spatially dependent dust and PAH emission, is presented. Given a hydrodynamic simulation of a galaxy, this model can calculate a realistic 2D ultraviolet-submillimetre spectral energy distribution of the galaxy, including emission lines from H ii regions, from any viewpoint. To model the emission from star-forming regions, the mappingsiii photoionization code is used. The high wavelength resolution (similar to 1000 wavelengths) is made possible by the polychromatic Monte Carlo algorithm employed by sunrise. From the 2D spectral energy distributions (SEDs), images in any filter bands or integrated galaxy SEDs can be created. Using a suite of hydrodynamic simulations of disc galaxies, the output broad-band images and SEDs are compared with observed galaxies from the multiwavelength SINGS and SLUGS galaxy surveys. Overall, the output SEDs show a good match with observed galaxies in colours ranging from far-UV to submillimetre wavelengths. The only possible exception is the 160/850 mu m colour, which the simulations underestimate by a factor of similar to 5 compared to the SINGS sample. However, the simulations here agree with the SLUGS galaxies, which consistently have significantly larger amounts of cold dust than the SINGS galaxies. The sunrise model can be used to generate simulated observations of arbitrary hydrodynamic galaxy simulations. In this way, predictions of galaxy formation theories can be directly tested against observations of galaxies. C1 [Jonsson, Patrik; Cox, T. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Groves, Brent A.] Leiden Univ, Sterrewacht Leiden, NL-2333 CA Leiden, Netherlands. [Jonsson, Patrik] 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 FU Jet Propulsion Laboratory [30183]; NASA through grants from the Space Telescope Science Institute [HST-AR-10678/10958/11758]; NASA [NAS5-26555]; Office of Science of the US Department of Energy FX The authors are grateful for the hospitality of the Max-Planck Institut fur Astrophysik in Garching, where part of this paper was written. We also thank Tom Abel, Fabio Governato, Chris Hayward, Desika Narayanan, Jennifer Lotz, Yuexing Li, Greg Novak and Joel Primack for enduring long discussions about various aspects of our model, and Chris Willmer for providing an electronic sample of the SLUGS galaxies. The comments by the anonymous referee were also helpful in finding mistakes and improving the clarity of the paper. PJ was supported by Spitzer Theory Grant 30183 from the Jet Propulsion Laboratory and by programme HST-AR-10678/10958/11758, 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. This research used computational resources of the NASA Advanced Supercomputing Division (NAS) and the National Energy Research Scientific Supercomputing Center (NERSC), which is supported by the Office of Science of the US Department of Energy. NR 68 TC 90 Z9 90 U1 0 U2 2 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 MAR 21 PY 2010 VL 403 IS 1 BP 17 EP 44 DI 10.1111/j.1365-2966.2009.16087.x PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 579EW UT WOS:000276351600022 ER PT J AU Zhuravleva, IV Churazov, EM Sazonov, SY Sunyaev, RA Forman, W Dolag, K AF Zhuravleva, I. V. Churazov, E. M. Sazonov, S. Yu. Sunyaev, R. A. Forman, W. Dolag, K. TI Polarization of X-ray lines from galaxy clusters and elliptical galaxies - a way to measure the tangential component of gas velocity SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE polarization; radiative transfer; scattering; methods: numerical; X-rays: galaxies: clusters ID ADAPTIVE MESH REFINEMENT; XMM-NEWTON OBSERVATIONS; HELIUM-LIKE IONS; COSMOLOGICAL SIMULATIONS; GASEOUS ATMOSPHERE; PERSEUS CLUSTER; PROFILES; MOTIONS; FLOWS; M87 AB We study the impact of gas motions on the polarization of bright X-ray emission lines from the hot intercluster medium. The polarization naturally arises from resonant scattering of emission lines owing to a quadrupole component in the radiation field produced by a centrally peaked gas density distribution. If differential gas motions are present, then a photon emitted in one region of the cluster will be scattered in another region only if their relative velocities are small enough and the Doppler shift of the photon energy does not exceed the linewidth. This affects both the degree and the direction of polarization. The changes in the polarization signal are in particular sensitive to the gas motions perpendicular to the line of sight. We calculate the expected degree of polarization for several patterns of gas motions, including a slow inflow expected in a simple cooling flow model and a fast outflow in an expanding spherical shock wave. In both cases, the effect of non-zero gas velocities is found to be minor. We also calculate the polarization signal for a set of clusters, taken from large-scale structure simulations and evaluate the impact of the gas bulk motions on the polarization signal. We argue that the expected degree of polarization is within reach of the next generation of space X-ray polarimeters. C1 [Zhuravleva, I. V.; Churazov, E. M.; Sazonov, S. Yu.; Sunyaev, R. A.; Dolag, K.] MPI Astrophys, D-85741 Garching, Germany. [Churazov, E. M.; Sazonov, S. Yu.; Sunyaev, R. A.] Space Res Inst, Moscow 117997, Russia. [Forman, W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Zhuravleva, IV (reprint author), MPI Astrophys, Karl Schwarzschild Str 1, D-85741 Garching, Germany. EM izhur@mpa-garching.mpg.de RI Churazov, Eugene/A-7783-2013 FU DFG [CH389/3-2]; NASA [NAS8-38248, NAS8-01130, NAS8-03060]; Division of Physical Sciences of the RAS; Chandra Science Center; Smithsonian Institution; MPI fur Astrophysik; MPI fur Extrater-restrische Physik FX IVZ and EMC are grateful to Professor Dmitry Nagirner for numerous useful discussions. EMC and WF thank Eric Silver for helpful comments and discussions about polarimeters. RAS thanks Kevin Black for demonstration of the Bragg polarimeter. IVZ thanks Fabio Muleri for important comments and corrections about future polarimeters. This work was supported by the DFG grant CH389/3-2, NASA contracts NAS8-38248, NAS8-01130, NAS8-03060, the programme 'Extended objects in the Universe' of the Division of Physical Sciences of the RAS, the Chandra Science Center, the Smithsonian Institution, MPI fur Astrophysik and MPI fur Extrater-restrische Physik. NR 47 TC 16 Z9 16 U1 0 U2 3 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 MAR 21 PY 2010 VL 403 IS 1 BP 129 EP 150 DI 10.1111/j.1365-2966.2009.16148.x PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 579EW UT WOS:000276351600028 ER PT J AU Forbes, DA Spitler, LR Harris, WE Bailin, J Strader, J Brodie, JP Larsen, SS AF Forbes, Duncan A. Spitler, Lee R. Harris, W. E. Bailin, Jeremy Strader, Jay Brodie, Jean P. Larsen, S. S. TI A blue tilt in the globular cluster system of the Milky Way-like galaxy NGC 5170 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE globular clusters: general; galaxies: individual: NGC 5170; galaxies: star clusters ID SPIRAL GALAXIES; WIDE-FIELD; GIANT ELLIPTICALS; ADVANCED CAMERA; STAR-CLUSTERS; ORIGIN; M87; METALLICITIES; PARAMETERS; SOFTWARE AB Here, we present Hubble Space Telescope/Advanced Camera for Surveys (ACS) imaging, in the B and I bands, of the edge-on Sb/Sc galaxy NGC 5170. Excluding the central disc region, we detect 142 objects with colours and sizes typical of globular clusters (GCs). Our main result is the discovery of a 'blue tilt' (a mass-metallicity relation), at the 3 Sigma level, in the metal-poor GC subpopulation of this Milky Way like galaxy. The tilt is consistent with that seen in massive elliptical galaxies and with the self-enrichment model of Bailin & Harris. For a linear mass-metallicity relation, the tilt has the form Z similar to L0.42 +/- 0.13. We derive a total GC system population of 600 +/- 100, making it much richer than the Milky Way. However, when this number is normalized by the host galaxy luminosity or stellar mass it is similar to that of M31. Finally, we report the presence of a potential Ultra Compact Dwarf of size similar to 6 pc and luminosity M(I) similar to -12.5, assuming it is physically associated with NGC 5170. C1 [Forbes, Duncan A.; Spitler, Lee R.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Harris, W. E.; Bailin, Jeremy] McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1, Canada. [Strader, Jay] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Brodie, Jean P.] Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA. [Larsen, S. S.] Univ Utrecht, Astron Inst, NL-3584 Utrecht, Netherlands. RP Forbes, DA (reprint author), Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. EM dforbes@swin.edu.au RI Spitler, Lee/A-9867-2013 OI Spitler, Lee/0000-0001-5185-9876 FU ARC; NSF [AST-0507729] FX We would like to thank K. Forde for his work performing the initial data reduction. DF and LS thank the ARC for financial support. We thank C. Foster for useful comments on this work. This material is based on the work supported by NSF grant AST-0507729. We acknowledge the usage of HyperLeda andNED data bases. Finally, we thank the referee for several useful suggestions that have improved the paper. NR 47 TC 14 Z9 14 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 MAR 21 PY 2010 VL 403 IS 1 BP 429 EP 438 DI 10.1111/j.1365-2966.2009.16130.x PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 579EW UT WOS:000276351600054 ER PT J AU Di Stefano, R Howell, SB Kawaler, SD AF Di Stefano, Rosanne Howell, Steve B. Kawaler, Steven D. TI A SEARCH FOR ASTEROIDS, MOONS, AND RINGS ORBITING WHITE DWARFS SO ASTROPHYSICAL JOURNAL LA English DT Article DE minor planets, asteroids: general; planetary systems; white dwarfs ID PLANET; SIGNATURES; ACCRETION; TRANSIT; COMETS; SYSTEM; NUMBER; STARS AB Do white dwarfs host asteroid systems? Although several lines of argument suggest that white dwarfs may be orbited by large populations of asteroids, transits would provide the most direct evidence. We demonstrate that the Kepler mission has the capability to detect transits of white dwarfs by asteroids. Because white-dwarf asteroid systems, if they exist, are likely to contain many asteroids orbiting in a spatially extended distribution, discoveries of asteroid transits can be made by monitoring only a small number of white dwarfs, compatible with Kepler's primary mission, which is to monitor stars with potentially habitable planets. Possible future missions that survey 10 times as many stars with similar sensitivity and minute-cadence monitoring can establish the characteristics of asteroid systems around white dwarfs, such as the distribution of asteroid sizes and semimajor axes. Transits by planets would be more dramatic, but the probability that they will occur is lower. Ensembles of planetary moons and/or the presence of rings around planets can also produce transits detectable by Kepler. The presence of moons and rings can significantly increase the probability that Kepler will discover planets orbiting white dwarfs, even while monitoring only a small number of them. C1 [Di Stefano, Rosanne] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Howell, Steve B.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Kawaler, Steven D.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. RP Di Stefano, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Kawaler, Steven/0000-0002-6536-6367 NR 21 TC 12 Z9 12 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 MAR 20 PY 2010 VL 712 IS 1 BP 142 EP 146 DI 10.1088/0004-637X/712/1/142 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 564NX UT WOS:000275222900012 ER PT J AU Ellison, DC Patnaude, DJ Slane, P Raymond, J AF Ellison, Donald C. Patnaude, Daniel J. Slane, Patrick Raymond, John TI EFFICIENT COSMIC RAY ACCELERATION, HYDRODYNAMICS, AND SELF-CONSISTENT THERMAL X-RAY EMISSION APPLIED TO SUPERNOVA REMNANT RX J1713.7-3946 SO ASTROPHYSICAL JOURNAL LA English DT Article DE acceleration of particles; cosmic rays; magnetic fields; shock waves; ISM: supernova remnants; turbulence ID DIFFUSIVE SHOCK ACCELERATION; NONLINEAR PARTICLE-ACCELERATION; NONTHERMAL RADIATION; MAGNETIC-FIELDS; INJECTION; ORIGIN; STARS; AMPLIFICATION; TEMPERATURE; INSTABILITY AB We model the broadband emission from supernova remnant (SNR) RX J1713.7-3946 including, for the first time, a consistent calculation of thermal X-ray emission together with non-thermal emission in a nonlinear diffusive shock acceleration model. Our model tracks the evolution of the SNR including the plasma ionization state between the forward shock and the contact discontinuity. We use a plasma emissivity code to predict the thermal X-ray emission spectrum assuming the initially cold electrons are heated either by Coulomb collisions with the shock-heated protons (the slowest possible heating), or come into instant equilibration with the protons. For either electron heating model, electrons reach greater than or similar to 10(7) K rapidly and the X-ray line emission near 1 keV is more than 10 times as luminous as the underlying thermal bremsstrahlung continuum. Since recent Suzaku observations show no detectable line emission, this places strong constraints on the unshocked ambient medium density and on the relativistic electron-to-proton ratio. For the uniform circumstellar medium (CSM) models that we consider, the low densities and high relativistic electron-to-proton ratios required to match the Suzaku X-ray observations definitively rule out pion decay as the emission process producing GeV-TeV photons. We show that leptonic models, where inverse-Compton scattering against the cosmic background radiation dominates the GeV-TeV emission, produce better fits to the broadband thermal and non-thermal observations in a uniform CSM. C1 [Ellison, Donald C.] N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA. [Patnaude, Daniel J.; Slane, Patrick; Raymond, John] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Ellison, DC (reprint author), N Carolina State Univ, Dept Phys, Box 8202, Raleigh, NC 27695 USA. EM don_ellison@ncsu.edu RI XRAY, SUZAKU/A-1808-2009 FU NASA [ATP02-0042-0006, NNH04Zss001N-LTSA, 06-ATP06-21, NAS8-03060, NNX09AT68G]; SI Endowment Grant FX We thank Matthew Baring, Roger Blandford, Andrei Bykov, Stefan Funk, Matthieu Renaud, and Andrey Vladimirov for helpful discussions on this work. We thank Yasunobu Uchiyama for furnishing the Suzaku data and Stefan Funk for furnishing the Fermi-LAT and HESS data. D. C. E acknowledges support from NASA grants ATP02-0042-0006, NNH04Zss001N-LTSA, and 06-ATP06-21. P.O.S. and D.J.P. acknowledge support from NASA Contract NAS8-03060. P.O.S. and D. C. E. acknowledge support from NASA grant NNX09AT68G. The authors are grateful to the KITP in Santa Barbara where part of this work was done when the authors were participating in a KITP program. D. C. E. also thanks KIPAC and D.J.P. acknowledges travel support from a SI Endowment Grant. NR 37 TC 107 Z9 107 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 MAR 20 PY 2010 VL 712 IS 1 BP 287 EP 293 DI 10.1088/0004-637X/712/1/287 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 564NX UT WOS:000275222900026 ER PT J AU Vercellone, S D'Ammando, F Vittorini, V Donnarumma, I Pucella, G Tavani, M Ferrari, A Raiteri, CM Villata, M Romano, P Krimm, H Tiengo, A Chen, AW Giovannini, G Venturi, T Giroletti, M Kovalev, YY Sokolovsky, K Pushkarev, AB Lister, ML Argan, A Barbiellini, G Bulgarelli, A Caraveo, P Cattaneo, PW Cocco, V Costa, E Del Monte, E De Paris, G Di Cocco, G Evangelista, Y Feroci, M Fiorini, M Fornari, F Froysland, T Fuschino, F Galli, M Gianotti, F Labanti, C Lapshov, I Lazzarotto, F Lipari, P Longo, F Giuliani, A Marisaldi, M Mereghetti, S Morselli, A Pellizzoni, A Pacciani, L Perotti, F Piano, G Picozza, P Pilia, M Prest, M Rapisarda, M Rappoldi, A Sabatini, S Soffitta, P Striani, E Trifoglio, M Trois, A Vallazza, E Zambra, A Zanello, D Pittori, C Verrecchia, F Santolamazza, P Giommi, P Colafrancesco, S Salotti, L Agudo, I Aller, HD Aller, MF Arkharov, AA Bach, U Bachev, R Beltrame, P Benitez, E Bottcher, M Buemi, CS Calcidese, P Capezzali, D Carosati, D Chen, WP Da Rio, D Di Paola, A Dolci, M Dultzin, D Forne, E Gomez, JL Gurwell, MA Hagen-Thorn, VA Halkola, A Heidt, J Hiriart, D Hovatta, T Hsiao, HY Jorstad, SG Kimeridze, G Konstantinova, TS Kopatskaya, EN Koptelova, E Kurtanidze, O Lahteenmaki, A Larionov, VM Leto, P Ligustri, R Lindfors, E Lopez, JM Marscher, AP Mujica, R Nikolashvili, M Nilsson, K Mommert, M Palma, N Pasanen, M Roca-Sogorb, M Ros, JA Roustazadeh, P Sadun, AC Saino, J Sigua, L Sorcia, M Takalo, LO Tornikoski, M Trigilio, C Turchetti, R Umana, G AF Vercellone, S. D'Ammando, F. Vittorini, V. Donnarumma, I. Pucella, G. Tavani, M. Ferrari, A. Raiteri, C. M. Villata, M. Romano, P. Krimm, H. Tiengo, A. Chen, A. W. Giovannini, G. Venturi, T. Giroletti, M. Kovalev, Y. Y. Sokolovsky, K. Pushkarev, A. B. Lister, M. L. Argan, A. Barbiellini, G. Bulgarelli, A. Caraveo, P. Cattaneo, P. W. Cocco, V. Costa, E. Del Monte, E. De Paris, G. Di Cocco, G. Evangelista, Y. Feroci, M. Fiorini, M. Fornari, F. Froysland, T. Fuschino, F. Galli, M. Gianotti, F. Labanti, C. Lapshov, I. Lazzarotto, F. Lipari, P. Longo, F. Giuliani, A. Marisaldi, M. Mereghetti, S. Morselli, A. Pellizzoni, A. Pacciani, L. Perotti, F. Piano, G. Picozza, P. Pilia, M. Prest, M. Rapisarda, M. Rappoldi, A. Sabatini, S. Soffitta, P. Striani, E. Trifoglio, M. Trois, A. Vallazza, E. Zambra, A. Zanello, D. Pittori, C. Verrecchia, F. Santolamazza, P. Giommi, P. Colafrancesco, S. Salotti, L. Agudo, I. Aller, H. D. Aller, M. F. Arkharov, A. A. Bach, U. Bachev, R. Beltrame, P. Benitez, E. Boettcher, M. Buemi, C. S. Calcidese, P. Capezzali, D. Carosati, D. Chen, W. P. Da Rio, D. Di Paola, A. Dolci, M. Dultzin, D. Forne, E. Gomez, J. L. Gurwell, M. A. Hagen-Thorn, V. A. Halkola, A. Heidt, J. Hiriart, D. Hovatta, T. Hsiao, H-Y. Jorstad, S. G. Kimeridze, G. Konstantinova, T. S. Kopatskaya, E. N. Koptelova, E. Kurtanidze, O. Lahteenmaki, A. Larionov, V. M. Leto, P. Ligustri, R. Lindfors, E. Lopez, J. M. Marscher, A. P. Mujica, R. Nikolashvili, M. Nilsson, K. Mommert, M. Palma, N. Pasanen, M. Roca-Sogorb, M. Ros, J. A. Roustazadeh, P. Sadun, A. C. Saino, J. Sigua, L. Sorcia, M. Takalo, L. O. Tornikoski, M. Trigilio, C. Turchetti, R. Umana, G. TI MULTIWAVELENGTH OBSERVATIONS OF 3C 454.3. III. EIGHTEEN MONTHS OF AGILE MONITORING OF THE "CRAZY DIAMOND" SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: jets; quasars: general; quasars: individual (3C 454.3); radiation mechanisms: non-thermal ID ACTIVE GALACTIC NUCLEI; RAY TIMING EXPLORER; BL-LAC OBJECTS; GAMMA-RAY; X-RAY; BLAZAR 3C-454.3; XMM-NEWTON; VARIABILITY PROPERTIES; INFRARED OBSERVATIONS; SPACE MISSION AB We report on 18 months of multiwavelength observations of the blazar 3C 454.3 ( Crazy Diamond) carried out in the period 2007 July-2009 January. In particular, we show the results of the AGILE campaigns which took place on 2008 May-June, 2008 July-August, and 2008 October-2009 January. During the 2008 May-2009 January period, the source average flux was highly variable, with a clear fading trend toward the end of the period, from an average. gamma-ray flux F-E>100 (MeV) greater than or similar to 200 x 10(-8) photons cm(-2) s(-1) in 2008 May-June, to F-E>100 MeV similar to 80 x 10(-8) photons cm(-2) s(-1) in 2008 October-2009 January. The average gamma-ray spectrum between 100 MeV and 1 GeV can be fit by a simple power law, showing a moderate softening ( from Gamma(GRID) similar to 2.0 to Gamma(GRID) similar to 2.2) toward the end of the observing campaign. Only 3 sigma upper limits can be derived in the 20-60 keV energy band with Super-AGILE, because the source was considerably off-axis during the whole time period. In 2007 July-August and 2008 May-June, 3C 454.3 was monitored by Rossi X-ray Timing Explorer (RXTE). The RXTE/Proportional Counter Array (PCA) light curve in the 3-20 keV energy band shows variability correlated with the gamma-ray one. The RXTE/PCA average flux during the two time periods is F3-20 keV = 8.4 x 10(-11) erg cm(-2) s(-1), and F3-20 keV = 4.5 x 10(-11) erg cm(-2) s(-1), respectively, while the spectrum ( a power law with photon index Gamma(PCA) = 1.65 +/- 0.02) does not show any significant variability. Consistent results are obtained with the analysis of the RXTE/High-Energy X-Ray Timing Experiment quasi-simultaneous data. We also carried out simultaneous Swift observations during all AGILE campaigns. Swift/XRT detected 3C 454.3 with an observed flux in the 2-10 keV energy band in the range (0.9-7.5) x 10(-11) erg cm(-2) s(-1) and a photon index in the range Gamma(XRT) = 1.33-2.04. In the 15-150 keV energy band, when detected, the source has an average flux of about 5 mCrab. GASP-WEBT monitored 3C 454.3 during the whole 2007-2008 period in the radio, millimeter, near-IR, and optical bands. The observations show an extremely variable behavior at all frequencies, with flux peaks almost simultaneous with those at higher energies. A correlation analysis between the optical and the gamma-ray fluxes shows that the gamma-optical correlation occurs with a time lag of tau = - 0.4(-0.8)(+0.6) days, consistent with previous findings for this source. An analysis of 15 GHz and 43 GHz VLBI core radio flux observations in the period 2007 July-2009 February shows an increasing trend of the core radio flux, anti-correlated with the higher frequency data, allowing us to derive the value of the source magnetic field. Finally, the modeling of the broadband spectral energy distributions for the still unpublished data, and the behavior of the long-term light curves in different energy bands, allow us to compare the jet properties during different emission states, and to study the geometrical properties of the jet on a time-span longer than one year. C1 [Vercellone, S.; Romano, P.] INAF IASF Palermo, I-90146 Palermo, Italy. [D'Ammando, F.; Vittorini, V.; Donnarumma, I.; Tavani, M.; Argan, A.; Cocco, V.; Costa, E.; Del Monte, E.; De Paris, G.; Evangelista, Y.; Feroci, M.; Froysland, T.; Lapshov, I.; Lazzarotto, F.; Pacciani, L.; Piano, G.; Sabatini, S.; Soffitta, P.; Striani, E.; Trois, A.] INAF IASF Roma, I-00133 Rome, Italy. [D'Ammando, F.; Tavani, M.] Univ Roma Tor Vergata, Dip Fis, I-00133 Rome, Italy. [Vittorini, V.; Tavani, M.; Ferrari, A.; Chen, A. W.] CNR, I-10133 Turin, Italy. [Pucella, G.; Rapisarda, M.] ENEA Roma, I-00044 Frascati, Roma, Italy. [Ferrari, A.] Univ Turin, Dip Fis, I-10125 Turin, Italy. [Raiteri, C. M.; Villata, M.] Osserv Astron Torino, INAF, I-10025 Pino Torinese, Italy. [Krimm, H.] CRESST, Greenbelt, MD USA. [Krimm, H.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Krimm, H.] Univ Space Res Assoc, Columbia, MD USA. [Tiengo, A.; Chen, A. W.; Caraveo, P.; Fiorini, M.; Fornari, F.; Giuliani, A.; Mereghetti, S.; Perotti, F.; Pilia, M.; Zambra, A.] INAF IASF Milano, I-20133 Milan, Italy. [Giovannini, G.] Univ Bologna, Dip Astron, I-40127 Bologna, Italy. [Giovannini, G.; Venturi, T.; Giroletti, M.] INAF IRA, I-40129 Bologna, Italy. [Kovalev, Y. Y.; Sokolovsky, K.; Pushkarev, A. B.; Bach, U.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Kovalev, Y. Y.; Sokolovsky, K.; Vallazza, E.] PN Lebedev Phys Inst, Ctr Astro Space, Moscow 117997, Russia. [Pushkarev, A. B.; Arkharov, A. A.; Larionov, V. M.] Pulkovo Observ, St Petersburg, Russia. [Pushkarev, A. B.] Crimean Astrophys Observ, UA-98049 Nauchnyi, Crimea, Ukraine. [Lister, M. L.] Purdue Univ, W Lafayette, IN 47906 USA. [Barbiellini, G.; Longo, F.] Dip Fis, I-34127 Trieste, Italy. [Barbiellini, G.; Longo, F.] Ist Nazl Fis Nucl, I-34127 Trieste, Italy. [Bulgarelli, A.; Di Cocco, G.; Fuschino, F.; Gianotti, F.; Labanti, C.; Marisaldi, M.; Trifoglio, M.] INAF IASF Bologna, I-40129 Bologna, Italy. [Cattaneo, P. W.; Rappoldi, A.] Ist Nazl Fis Nucl, I-27100 Pavia, Italy. [Galli, M.] ENEA, I-40129 Bologna, Italy. [Lapshov, I.] Acad Sci, IKI, Moscow, Russia. [Lipari, P.; Zanello, D.] INFN Roma La Spaienza, I-00185 Rome, Italy. [Morselli, A.; Picozza, P.] INFN Roma Tor Vergata, I-00133 Rome, Italy. [Pellizzoni, A.; Pilia, M.] Osservatorio Astron Cagliari, INAF, I-09012 Capoterra, Italy. [Pilia, M.; Prest, M.] Univ Insubria, Dipartimento Fis, I-22100 Como, Italy. [Pittori, C.; Verrecchia, F.; Santolamazza, P.; Giommi, P.; Colafrancesco, S.] ASI ASDC, I-00044 Frascati, Roma, Italy. [Salotti, L.] ASI, I-00198 Rome, Italy. [Agudo, I.; Gomez, J. L.; Roca-Sogorb, M.] CSIC, Inst Astrofis Andalucia, Madrid, Spain. [Aller, H. D.; Aller, M. F.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Bachev, R.] Bulgarian Acad Sci, Inst Astron, BG-1040 Sofia, Bulgaria. [Benitez, E.; Dultzin, D.; Hiriart, D.; Lopez, J. M.; Sorcia, M.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. [Boettcher, M.; Palma, N.; Roustazadeh, P.] Ohio Univ, Dept Phys & Astron, Inst Astrophys, Athens, OH 45701 USA. [Buemi, C. S.; Leto, P.; Trigilio, C.; Umana, G.] Osserv Astrofis Catania, INAF, Catania, Italy. [Calcidese, P.] Osservatorio Astron Reg Autonoma Valle Aosta, Aosta, Italy. [Chen, W. P.; Hsiao, H-Y.; Koptelova, E.] Natl Cent Univ, Inst Astron, Taipei, Taiwan. [Di Paola, A.] Osserv Astron Roma, INAF, Rome, Italy. [Forne, E.; Ros, J. A.] Agrupacio Astron Sabadell, Sabadell, Spain. [Gurwell, M. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. [Hagen-Thorn, V. A.; Konstantinova, T. S.; Kopatskaya, E. N.; Larionov, V. M.] St Petersburg State Univ, Astron Inst, St Petersburg, Russia. [Hagen-Thorn, V. A.; Larionov, V. M.] Isaac Newton Inst Chile, St Petersburg Branch, St Petersburg, Russia. [Halkola, A.; Lindfors, E.; Nilsson, K.; Pasanen, M.; Saino, J.; Takalo, L. O.] Univ Turku, Tuorla Observ, Dept Phys & Astron, SF-20500 Turku, Finland. [Heidt, J.; Mommert, M.] Heidelberg Univ, Landessternwarte Heidelberg Konigstuhl, ZAH, Heidelberg, Germany. [Hovatta, T.; Lahteenmaki, A.; Tornikoski, M.] Aalto Univ, Metsahovi Radio Observ, Helsinki, Finland. [Jorstad, S. G.; Marscher, A. P.] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA. [Mujica, R.] INAOF, Mexico City, DF, Mexico. [Sadun, A. C.] Univ Colorado, Dept Phys, Denver, CO 80202 USA. RP Vercellone, S (reprint author), INAF IASF Palermo, Via Malfa 153, I-90146 Palermo, Italy. EM stefano@ifc.inaf.it RI Pushkarev, Alexander/M-9997-2015; Pittori, Carlotta/C-7710-2016; Morselli, Aldo/G-6769-2011; Lazzarotto, Francesco/J-4670-2012; Larionov, Valeri/H-1349-2013; Kopatskaya, Evgenia/H-4720-2013; Grishina, Tatiana/H-6873-2013; Hagen-Thorn, Vladimir/H-3983-2013; Kovalev, Yuri/J-5671-2013; Lahteenmaki, Anne/L-5987-2013; Kurtanidze, Omar/J-6237-2014; Sokolovsky, Kirill/D-2246-2015; Trifoglio, Massimo/F-5302-2015; Agudo, Ivan/G-1701-2015; Jorstad, Svetlana/H-6913-2013 OI Giovannini, Gabriele/0000-0003-4916-6362; Marisaldi, Martino/0000-0002-4000-3789; Vercellone, Stefano/0000-0003-1163-1396; Raiteri, Claudia Maria/0000-0003-1784-2784; MEREGHETTI, SANDRO/0000-0003-3259-7801; Giroletti, Marcello/0000-0002-8657-8852; Tavani, Marco/0000-0003-2893-1459; Lazzarotto, Francesco/0000-0003-4871-4072; Costa, Enrico/0000-0003-4925-8523; giommi, paolo/0000-0002-2265-5003; Donnarumma, Immacolata/0000-0002-4700-4549; Pellizzoni, Alberto Paolo/0000-0002-4590-0040; Tiengo, Andrea/0000-0002-6038-1090; Venturi, Tiziana/0000-0002-8476-6307; Sabatini, Sabina/0000-0003-2076-5767; Caraveo, Patrizia/0000-0003-2478-8018; PREST, MICHELA/0000-0003-3161-4454; Verrecchia, Francesco/0000-0003-3455-5082; Fiorini, Mauro/0000-0001-8297-1983; Di Paola, Andrea/0000-0002-2189-8644; trois, alessio/0000-0002-3180-6002; Labanti, Claudio/0000-0002-5086-3619; Feroci, Marco/0000-0002-7617-3421; Soffitta, Paolo/0000-0002-7781-4104; Picozza, Piergiorgio/0000-0002-7986-3321; Villata, Massimo/0000-0003-1743-6946; Fuschino, Fabio/0000-0003-2139-3299; Gianotti, Fulvio/0000-0003-4666-119X; Leto, Paolo/0000-0003-4864-2806; Pittori, Carlotta/0000-0001-6661-9779; Dolci, Mauro/0000-0001-8000-5642; Buemi, Carla Simona/0000-0002-7288-4613; Bulgarelli, Andrea/0000-0001-6347-0649; galli, marcello/0000-0002-9135-3228; Cattaneo, Paolo Walter/0000-0001-6877-6882; Pacciani, Luigi/0000-0001-6897-5996; Morselli, Aldo/0000-0002-7704-9553; Larionov, Valeri/0000-0002-4640-4356; Kopatskaya, Evgenia/0000-0001-9518-337X; Grishina, Tatiana/0000-0002-3953-6676; Hagen-Thorn, Vladimir/0000-0002-6431-8590; Kovalev, Yuri/0000-0001-9303-3263; Sokolovsky, Kirill/0000-0001-5991-6863; Trifoglio, Massimo/0000-0002-2505-3630; Agudo, Ivan/0000-0002-3777-6182; Jorstad, Svetlana/0000-0001-9522-5453 NR 66 TC 47 Z9 48 U1 1 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 2010 VL 712 IS 1 BP 405 EP 420 DI 10.1088/0004-637X/712/1/405 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 564NX UT WOS:000275222900035 ER PT J AU Reeves, KK Moats, SJ AF Reeves, Katharine K. Moats, Stephanie J. TI RELATING CORONAL MASS EJECTION KINEMATICS AND THERMAL ENERGY RELEASE TO FLARE EMISSIONS USING A MODEL OF SOLAR ERUPTIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: coronal mass ejections (CMEs); Sun: flares ID FLUX-ROPE ACCELERATION; MAGNETIC RECONNECTION; X-RAY; EVAPORATION MODEL; LINE EMISSION; LOOPS; CMES; PHASES AB We use a model of solar eruptions that combines a loss-of-equilibrium coronal mass ejection (CME) model with a multi-threaded flare loop model in order to understand the relationship between the CME kinematics, thermal energy release, and soft X-ray emissions in solar eruptions. We examine the correlation between CME acceleration and the peak soft X-ray flux in many modeled cases with different parameters, and find that the two quantities are well correlated. We also examine the timing of the peak acceleration and the light curve derivative, and find that these quantities tend to peak at similar times for cases where the magnetic field is high and the inflow Alfven Mach number is fast. Finally, we study the relationship between the total thermal energy released in the model and the calculated peak soft X-ray flux of the resulting flare. We find that there is a power-law relationship between these two quantities, with F-peak similar to E-alpha, where alpha is between 2.54 and 1.54, depending on the reconnection rate. This finding has repercussions for the assumptions underlying the Neupert effect, in which the peak soft X-ray flux is assumed to be proportional to the thermal energy release. C1 [Reeves, Katharine K.; Moats, Stephanie J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Moats, Stephanie J.] New Mexico Inst Min & Technol, Socorro, NM 87801 USA. RP Reeves, KK (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 58, Cambridge, MA 02138 USA. EM kreeves@cfa.harvard.edu RI Reeves, Katharine/P-9163-2014 FU NSF-SHINE [ATM-0752257]; NSF-REU [ATM-0851866] FX The authors thank the anonymous referee for helpful comments on the manuscript. K. K. R. is supported under the NSF-SHINE program, grant number ATM-0752257. S.J.M. is supported under the NSF-REU solar physics program at CfA, grant number ATM-0851866. NR 39 TC 14 Z9 14 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 2010 VL 712 IS 1 BP 429 EP 434 DI 10.1088/0004-637X/712/1/429 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 564NX UT WOS:000275222900037 ER PT J AU Oda, H Machida, M Nakamura, KE Matsumoto, R AF Oda, H. Machida, M. Nakamura, K. E. Matsumoto, R. TI THERMAL EQUILIBRIA OF OPTICALLY THIN, MAGNETICALLY SUPPORTED, TWO-TEMPERATURE, BLACK HOLE ACCRETION DISKS SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; magnetic fields; X-rays: binaries ID ADVECTION-DOMINATED ACCRETION; X-RAY BINARIES; CYGNUS X-1; MAGNETOHYDRODYNAMIC SIMULATIONS; SPECTRAL TRANSITIONS; GLOBAL STRUCTURES; SAGITTARIUS-A; GAS-PRESSURE; HARD STATE; FLOWS AB We obtained thermal equilibrium solutions for optically thin, two-temperature black hole accretion disks incorporating magnetic fields. The main objective of this study is to explain the bright/hard state observed during the bright/slow transition of galactic black hole candidates. We assume that the energy transfer from ions to electrons occurs via Coulomb collisions. Bremsstrahlung, synchrotron, and inverse Compton scattering are considered as the radiative cooling processes. In order to complete the set of basic equations, we specify the magnetic flux advection rate instead of beta = p(gas)/p(mag). We find magnetically supported (low-beta), thermally stable solutions. In these solutions, the total amount of the heating via the dissipation of turbulent magnetic fields goes into electrons and balances the radiative cooling. The low-beta solutions extend to high mass accretion rates (greater than or similar to alpha(2)(M)over dot(Edd)) and the electron temperature is moderately cool (T(e) similar to 10(8)-10(9.5) K). High luminosities (greater than or similar to 0.1L(Edd)) and moderately high energy cutoffs in the X-ray spectrum (similar to 50-200 keV) observed in the bright/hard state can be explained by the low-beta solutions. C1 [Oda, H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Oda, H.; Matsumoto, R.] Chiba Univ, Grad Sch Sci, Dept Phys, Inage Ku, Chiba 2638522, Japan. [Machida, M.] Nagoya Univ, Dept Phys & Astrophys, Chikusa Ku, Aichi 4648602, Japan. [Nakamura, K. E.] Matsue Natl Coll Technol, Dept Sci, Matsue, Shimane 6908515, Japan. RP Oda, H (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM hoda@cfa.harvard.edu FU Ministry of Education, Culture, Sports, Science and Technology [20340040]; JSPS [20.1842] FX We are grateful to R. Narayan for valuable discussion and closely examining our draft. This work is supported by the Grant-in-Aid for Science Research of the Ministry of Education, Culture, Sports, Science and Technology (R. M.: 20340040) and Grant- in-Aid for JSPS Fellows (20.1842). NR 48 TC 23 Z9 23 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 MAR 20 PY 2010 VL 712 IS 1 BP 639 EP 652 DI 10.1088/0004-637X/712/1/639 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 564NX UT WOS:000275222900056 ER PT J AU Zhu, L Wright, MCH Zhao, JH Wu, YF AF Zhu, Lei Wright, M. C. H. Zhao, Jun-Hui Wu, Yuefang TI DUST AND HCO+ GAS IN THE STAR-FORMING CORE W3-SE SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: clouds; ISM: jets and outflows; ISM: kinematics and dynamics; ISM: molecules; radio lines: ISM; stars: formation ID GIANT MOLECULAR CLOUD; INFALL MOTIONS; DENSE CORES; REGIONS; EMISSION; COLLAPSE; OBJECTS AB We report new results from recent Combined Array for Research in Millimeter-wave Astronomy (CARMA) observations of both continuum and HCO+(1-0) line emission at lambda 3.4 mm from W3-SE, a molecular core of intermediate mass, together with the observations of continuum emission at lambda 1.1 and lambda 0.85/lambda 0.45 mm with the Submillimeter Array (SMA) and the James Clerk Maxwell Telescope, respectively. A continuum emission core elongated from SE to NW, with a size of similar to 10 '', has been observed at the millimeter and submillimeter wavelengths. The dust core has been resolved into a double source with the SMA at lambda 1.1 mm. The angular separation between the two components is similar to 4 ''. Together with the measurements from the Spitzer Space Telescope and the Midcourse Space Experiment at mid-IR wavelengths, we determined the spectral energy distribution (SED) of the continuum emission from W3-SE and fit it with a thermal dust emission model. Our best fitting of the SED suggests the presence of two dust components with different temperatures. The emission at millimeter/submillimeter wavelengths is dominated by a major component that is characterized by a temperature of T-d = 41 +/- 6 K with a mass of 65 +/- 10 M-circle dot. In addition, there is a weaker hot component (similar to 400 K) which accounts for emission in the mid-IR, suggesting that a small fraction of dust has been heated by newly formed stars. We also imaged the molecular core in the HCO+(1-0) line using CARMA at an angular resolution similar to 6 ''. In the central region of similar to 50 '', the integrated HCO+(1-0) line emission shows a main component A that coincides with the dust core, as well as two substructures B and C which are located N and SE of the dust core, respectively. With the CARMA observations, we have verified the presence of a blue-dominated double peak profile toward this core. The line profile cannot be explained by infall alone. The broad velocity wings of the line profile suggest that other kinematics such as outflows within the central 6 '' of the core likely dominate the resulting spectrum. The kinematics of the substructures of B and C suggest that the molecular gas outside the main component A appears to be dominated by the bipolar outflow originated from the dust core with a dynamical age of > 3 x 10(4) yr. Our analysis, based on the observations at wavelengths from millimeter, submillimeter, to mid-IR, suggest that the molecular core W3-SE hosts a group of newly formed young stars and protostars. C1 [Zhu, Lei; Zhao, Jun-Hui] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Wright, M. C. H.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Wu, Yuefang] Peking Univ, Dept Astron, Beijing 100871, Peoples R China. RP Zhu, L (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM lzhu@cfa.harvard.edu FU SAO predoctoral program; NSF; NSFC [10873019, 10733030] FX We are grateful for the staff of the CARMA, SMA, and JCMT for their assistance in the observations. L. Z. thanks the organizers and tutors of the CARMA 2008 summer school, and J. Carpenter for his help in data reduction. We are grateful to G. Ruch for providing the IRAC mosaic images and the point-source table, and the useful discussions with us on the infrared part of this work. L. Z. is supported by the SAO predoctoral program. L. Z. thanks the NRAO for providing him NSF travel fund to attend the millimeter/submillimeter conference in Taipei. Y. W. and L. Z. are grateful for the support of the grants 10873019 and 10733030 of NSFC. NR 25 TC 5 Z9 5 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 2010 VL 712 IS 1 BP 674 EP 684 DI 10.1088/0004-637X/712/1/674 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 564NX UT WOS:000275222900060 ER PT J AU Di Stefano, R AF Di Stefano, R. TI THE PROGENITORS OF TYPE Ia SUPERNOVAE. I. ARE THEY SUPERSOFT SOURCES? SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; planetary nebulae: general; stars: evolution; X-rays: general; X-rays: stars ID X-RAY SOURCES; FINAL MASS RELATION; XMM-NEWTON OBSERVATIONS; ACCRETING WHITE-DWARFS; QUASI-SOFT; LUMINOSITY FUNCTION; EXTERNAL GALAXIES; BLACK-HOLE; CHANDRA; NOVAE AB In a canonical model, the progenitors of Type Ia supernovae (SNe Ia) are accreting, nuclear-burning white dwarfs (NBWDs), which explode when the white dwarf reaches the Chandrasekhar mass, M(C). Such massive NBWDs are hot (kT similar to 100 eV), luminous (L similar to 10(38) erg s(-1)), and are potentially observable as luminous supersoft X-ray sources (SSSs). During the past several years, surveys for soft X-ray sources in external galaxies have been conducted. This paper shows that the results falsify the hypothesis that a large fraction of progenitors are NBWDs which are presently observable as SSSs. The data also place limits on sub-M(C) models. While SN Ia progenitors may pass through one or more phases of SSS activity, these phases are far shorter than the time needed to accrete most of the matter that brings them close to M(C). 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 and comments from many of the 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 suggestions that have been incorporated into Section 4. This work was supported in part by an LTSA grant from NASA and by funding from the Smithsonian Institution. NR 51 TC 65 Z9 65 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 MAR 20 PY 2010 VL 712 IS 1 BP 728 EP 733 DI 10.1088/0004-637X/712/1/728 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 564NX UT WOS:000275222900063 ER PT J AU Green, PJ Myers, AD Barkhouse, WA Mulchaey, JS Bennert, VN Cox, TJ Aldcroft, TL Wrobel, JM AF Green, Paul J. Myers, Adam D. Barkhouse, Wayne A. Mulchaey, John S. Bennert, Vardha N. Cox, Thomas J. Aldcroft, Thomas L. Wrobel, Joan M. TI SDSS J1254+0846: A BINARY QUASAR CAUGHT IN THE ACT OF MERGING (vol 710, 1578, 2010) SO ASTROPHYSICAL JOURNAL LA English DT Correction C1 [Green, Paul J.; Cox, Thomas J.; Aldcroft, Thomas L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Myers, Adam D.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Barkhouse, Wayne A.] Univ N Dakota, Dept Phys & Astrophys, Grand Forks, ND 58202 USA. [Mulchaey, John S.; Cox, Thomas J.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA. [Bennert, Vardha N.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Wrobel, Joan M.] Natl Radio Astron Observ, Socorro, NM 87801 USA. RP Green, PJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM pgreen@cfa.harvard.edu NR 1 TC 3 Z9 3 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 MAR 20 PY 2010 VL 712 IS 1 BP 762 EP 762 DI 10.1088/0004-637X/712/1/762 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 564NX UT WOS:000275222900068 ER PT J AU Pineda, JE Goodman, AA Arce, HG Caselli, P Foster, JB Myers, PC Rosolowsky, EW AF Pineda, Jaime E. Goodman, Alyssa A. Arce, Hector G. Caselli, Paola Foster, Jonathan B. Myers, Philip C. Rosolowsky, Erik W. TI DIRECT OBSERVATION OF A SHARP TRANSITION TO COHERENCE IN DENSE CORES SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE ISM: clouds; ISM: individual objects (B5, Perseus Molecular Complex); ISM: molecules; stars: formation ID PERSEUS MOLECULAR CLOUD; STAR-FORMING REGIONS; MASS FUNCTION; DARK CLOUDS; DUST EXTINCTION; PIPE NEBULA; EMISSION; COLLAPSE; BARNARD-5; QUIESCENT AB We present NH(3) observations of the B5 region in Perseus obtained with the Green Bank Telescope. The map covers a region large enough (similar to 11' x 14') that it contains the entire dense core observed in previous dust continuum surveys. The dense gas traced by NH(3)(1,1) covers a much larger area than the dust continuum features found in bolometer observations. The velocity dispersion in the central region of the core is small, presenting subsonic non-thermal motions which are independent of scale. However, it is because of the coverage and high sensitivity of the observations that we present the detection, for the first time, of the transition between the coherent core and the dense but more turbulent gas surrounding it. This transition is sharp, increasing the velocity dispersion by a factor of 2 in less than 0.04 pc (the 31 '' beam size at the distance of Perseus, similar to 250 pc). The change in velocity dispersion at the transition is approximate to 3 km s(-1) pc(-1). The existence of the transition provides a natural definition of dense core: the region with nearly constant subsonic non-thermal velocity dispersion. From the analysis presented here, we can neither confirm nor rule out a corresponding sharp density transition. C1 [Pineda, Jaime E.; Goodman, Alyssa A.; Foster, Jonathan B.; Myers, Philip C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Arce, Hector G.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Caselli, Paola] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Rosolowsky, Erik W.] Univ British Columbia Okanagan, Kelowna, BC V1V 1V7, Canada. RP Pineda, JE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jpineda@cfa.harvard.edu RI Pineda, Jaime/J-7405-2013; Goodman, Alyssa/A-6007-2010 OI Pineda, Jaime/0000-0002-3972-1978; Goodman, Alyssa/0000-0003-1312-0477 FU Association of Universities for Research in Astronomy, Inc. [AF002]; NSF [AST-9613615]; Fundacion Andes [C-13442]; NRAO [GSSP06-0015, GSSP08-0031]; National Science Foundation [AST-0407172, AST-0908159, AST-0845619, AST-0502605]; NSERC of Canada FX The Green Bank Telescope is operated by the National Radio Astronomy Observatory. The National Radio Astronomy Observatory is a facility of the National Science Foundation, operated under cooperative agreement by Associated Universities, Inc. J.E.P. is supported by the NSF through grant #AF002 from the Association of Universities for Research in Astronomy, Inc., under NSF cooperative agreement AST-9613615 and by Fundacion Andes under project No. C-13442. Support for this work was provided by the NSF through awards GSSP06-0015 and GSSP08-0031 from the NRAO. This material is based upon work supported by the National Science Foundation under grant No. AST-0407172 and AST-0908159 to AAG and AST-0845619 to HGA. E.W.R.'s work is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship (AST-0502605) and a Discovery Grant from NSERC of Canada. NR 42 TC 64 Z9 64 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 MAR 20 PY 2010 VL 712 IS 1 BP L116 EP L121 DI 10.1088/2041-8205/712/1/L116 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 567BV UT WOS:000275418200025 ER PT J AU Webb, NA Barret, D Godet, O Servillat, M Farrell, SA Oates, SR AF Webb, N. A. Barret, D. Godet, O. Servillat, M. Farrell, S. A. Oates, S. R. TI CHANDRA AND SWIFT FOLLOW-UP OBSERVATIONS OF THE INTERMEDIATE-MASS BLACK HOLE IN ESO 243-49 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE accretion, accretion disks; X-rays: binaries; X-rays: individual (HLX-1) ID STAR-FORMATION; CALIBRATION AB The brightest ultra-luminous X-ray source HLX-1 in the galaxy ESO 243-49 provides strong evidence for the existence of intermediate-mass black holes (IMBHs). As the luminosity and thus the mass estimate depend on the association of HLX-1 with ESO 243-49, it is essential to confirm its affiliation. This requires follow-up investigations at wavelengths other than X-rays, which in turn needs an improved source position. To further reinforce the IMBH identification, it is necessary to determine HLX-1's environment to establish whether it could potentially form and nourish a black hole at the observed luminosities. Using the High Resolution Camera on board Chandra, we determine a source position of R.A. = 01(h)10(m)28.(s)3 and decl. = -46 degrees 04'22.'' 3. A conservative 95% error of 0.'' 3 was found following a boresight correction by cross-matching the positions of three X-ray sources in the field with the Two Micron All Sky Survey catalog. Combining all Swift UV/Optical Telescope uvw2 images, we failed to detect a UV source at the Chandra position down to a 3 sigma limiting magnitude of 20.25 mag. However, there is evidence that the UV emission is elongated in the direction of HLX-1. This is supported by archival data from GALEX and suggests that the far-UV emission is stronger than the near-UV. This could imply that HLX-1 may be situated near the edge of a star-forming region. Using the latest X-ray observations, we deduce the mass accretion rate of a 500 M(circle dot) black hole with the observed luminosity and show that this is compatible with such an environment. C1 [Webb, N. A.; Barret, D.; Godet, O.] Univ Toulouse, UPS, CESR, F-31028 Toulouse 9, France. [Servillat, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Farrell, S. A.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Oates, S. R.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. RP Webb, NA (reprint author), Univ Toulouse, UPS, CESR, 9 Ave Colonel Roche, F-31028 Toulouse 9, France. EM natalie.webb@cesr.fr FU STFC FX We thank Neil Gehrels and the Swift team for according us the Swift observations as well as Harvey Tananbaum and the Chandra team for approving the two Chandra DDT observations. S. A. F. and S. O. acknowledge STFC funding. This research has made use of data obtained from the Chandra Data Archive and software provided by the Chandra X-ray Center. We thank the GALEX collaboration and the Space Telescope Science Institute for providing access to the UV images used in this work. GALEX is a NASA Small Explorer Class mission. We thank Simon Rosen for valuable discussions and are grateful to the referee for comments which improved this Letter. NR 12 TC 27 Z9 27 U1 1 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 MAR 20 PY 2010 VL 712 IS 1 BP L107 EP L110 DI 10.1088/2041-8205/712/1/L107 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 567BV UT WOS:000275418200023 ER PT J AU Jiang, LH Fan, XH Brandt, WN Carilli, CL Egami, E Hines, DC Kurk, JD Richards, GT Shen, Y Strauss, MA Vestergaard, M Walter, F AF Jiang, Linhua Fan, Xiaohui Brandt, W. N. Carilli, Chris L. Egami, Eiichi Hines, Dean C. Kurk, Jaron D. Richards, Gordon T. Shen, Yue Strauss, Michael A. Vestergaard, Marianne Walter, Fabian TI Dust-free quasars in the early Universe SO NATURE LA English DT Article ID BLACK-HOLE MASSES; NEAR-INFRARED SPECTROSCOPY; ACTIVE GALACTIC NUCLEI; DIGITAL SKY SURVEY; SIMILAR-TO 6; Z-SIMILAR-TO-6 QUASARS; ENERGY-DISTRIBUTIONS; DISTANT QUASARS; GALAXIES; EVOLUTION AB The most distant quasars known, at redshifts z approximate to 6, generally have properties indistinguishable from those of lower-redshift quasars in the rest-frame ultraviolet/optical and X-ray bands(1-3). This puzzling result suggests that these distant quasars are evolved objects even though the Universe was only seven per cent of its current age at these redshifts. Recently one z approximate to 6 quasar was shown not to have any detectable emission from hot dust(4), but it was unclear whether that indicated different hot-dust properties at high redshift or if it is simply an outlier. Here we report the discovery of a second quasar without hot-dust emission in a sample of 21 z approximate to 6 quasars. Such apparently hot-dust-free quasars have no counterparts at low redshift. Moreover, we demonstrate that the hot-dust abundance in the 21 quasars builds up in tandem with the growth of the central black hole, whereas at low redshift it is almost independent of the black hole mass. Thus z approximate to 6 quasars are indeed at an early evolutionary stage, with rapid mass accretion and dust formation. The two hot-dust-free quasars are likely to be first-generation quasars born in dust-free environments and are too young to have formed a detectable amount of hot dust around them. C1 [Jiang, Linhua; Fan, Xiaohui; Egami, Eiichi; Vestergaard, Marianne] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Fan, Xiaohui; Kurk, Jaron D.; Walter, Fabian] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Brandt, W. N.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Carilli, Chris L.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Hines, Dean C.] Space Sci Inst, Boulder, CO 80301 USA. [Kurk, Jaron D.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Richards, Gordon T.] Drexel Univ, Dept Phys, Philadelphia, PA 19104 USA. [Shen, Yue] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Strauss, Michael A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Vestergaard, Marianne] Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen O, Denmark. RP Jiang, LH (reprint author), Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA. EM ljiang@email.arizona.edu RI Vestergaard, Marianne/M-5247-2014; Brandt, William/N-2844-2015; Jiang, Linhua/H-5485-2016 OI Vestergaard, Marianne/0000-0001-9191-9837; Brandt, William/0000-0002-0167-2453; Jiang, Linhua/0000-0003-4176-6486 FU NASA; JPL/Caltech; NSF AST; Packard Fellowship; John Simon Guggenheim Memorial Fellowship; NASA ADP; Max-Planck-Gesellschaft; Humboldt-Stiftung; DFG; Danish National Research Foundation. FX This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. X. F. acknowledges support by NSF AST, a Packard Fellowship for Science and Engineering, and a John Simon Guggenheim Memorial Fellowship. W.N.B. was supported by the NASA ADP program. C. L. C. thanks the Max-Planck-Gesellschaft and the Humboldt-Stiftung for support through the Max-Planck-Forschungspreis. J.D.K. thanks the DFG for support via German-Israeli Project Cooperation. The Dark Cosmology Centre is funded by the Danish National Research Foundation. NR 30 TC 58 Z9 60 U1 0 U2 4 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD MAR 18 PY 2010 VL 464 IS 7287 BP 380 EP 383 DI 10.1038/nature08877 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 570FG UT WOS:000275657100039 PM 20237563 ER PT J AU Gotelli, NJ Graves, GR Rahbek, C AF Gotelli, Nicholas J. Graves, Gary R. Rahbek, Carsten TI Macroecological signals of species interactions in the Danish avifauna SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE null models; assembly rules; interspecific territoriality; conspecific social attraction; allee affect ID INTERSPECIFIC COMPETITION; HABITAT SELECTION; CLIMATE-CHANGE; BIRDS; COMMUNITIES; CONSEQUENCES; WARBLERS; TERRITORIALISM; DISTRIBUTIONS; ORGANIZATION AB The role of intraspecific and interspecific interactions in structuring biotic communities at fine spatial scales is well documented, but the signature of species interactions at coarser spatial scales is unclear. We present evidence that species interactions may be a significant factor in mediating the regional assembly of the Danish avifauna. Because >95% of breeding species (n = 197) are migratory, we hypothesized that dispersal limitation would not be important and that breeding distributions would largely reflect resource availability and autecological habitat preferences. Instead, we detected a striking pattern of spatial segregation between ecologically similar species at two spatial scales with a suite of null models that factored in the spatial distribution of habitats in Denmark as well as population size and biomass of each species. Habitat utilization analyses indicated that community-wide patterns of spatial segregation could not be attributed to the patchy distribution of habitat or to gross differences in habitat utilization among ecologically similar species. We hypothesize that, when habitat patch size is limited, conspecific attraction in concert with interspecific territoriality may result in spatially segregated distributions of ecologically similar species at larger spatial scales. In the Danish avifauna, the effects of species interactions on community assembly appear pervasive and can be discerned at grain sizes up to four orders of magnitude larger than those of individual territories. These results suggest that species interactions should be incorporated into species distribution modeling algorithms designed to predict species occupancy patterns based on environmental variables. C1 [Gotelli, Nicholas J.] Univ Vermont, Dept Biol, Burlington, VT 05405 USA. [Graves, Gary R.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA. [Rahbek, Carsten] Univ Copenhagen, Dept Biol, Ctr Macroecol Evolut & Climate, DK-2100 Copenhagen O, Denmark. RP Gotelli, NJ (reprint author), Univ Vermont, Dept Biol, Burlington, VT 05405 USA. EM ngotelli@uvm.edu RI Rahbek, Carsten/D-9372-2013; Rahbek, Carsten/L-1129-2013; publist, CMEC/C-3010-2012; publicationpage, cmec/B-4405-2017 NR 63 TC 106 Z9 108 U1 4 U2 72 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD MAR 16 PY 2010 VL 107 IS 11 BP 5030 EP 5035 DI 10.1073/pnas.0914089107 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 570YI UT WOS:000275714300042 PM 20194760 ER PT J AU Craft, KJ Pauls, SU Darrow, K Miller, SE Hebert, PDN Helgen, LE Novotny, V Weiblen, GD AF Craft, Kathleen J. Pauls, Steffen U. Darrow, Karolyn Miller, Scott E. Hebert, Paul D. N. Helgen, Lauren E. Novotny, Vojtech Weiblen, George D. TI Population genetics of ecological communities with DNA barcodes: An example from New Guinea Lepidoptera SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE community ecology; DNA barcoding; phylogeography; plant-insect interactions; speciation ID TROPICAL RAIN-FORESTS; PAPUA-NEW-GUINEA; HERBIVOROUS INSECTS; HOST-SPECIFICITY; DIVERSITY; BUTTERFLIES; DIFFERENTIATION; PHYLOGEOGRAPHY; BIODIVERSITY; BIOGEOGRAPHY AB Comparative population genetics of ecological guilds can reveal generalities in patterns of differentiation bearing on hypotheses regarding the origin and maintenance of community diversity. Contradictory estimates of host specificity and beta diversity in tropical Lepidoptera ( moths and butterflies) from New Guinea and the Americas have sparked debate on the role of host-associated divergence and geographic isolation in explaining latitudinal diversity gradients. We sampled haplotypes of mitochondrial cytochrome c oxidase I from 28 Lepidoptera species and 1,359 individuals across four host plant genera and eight sites in New Guinea to estimate population divergence in relation to host specificity and geography. Analyses of molecular variance and haplotype networks indicate varying patterns of genetic structure among ecologically similar sympatric species. One-quarter lacked evidence of isolation by distance or host-associated differentiation, whereas 21% exhibited both. Fourteen percent of the species exhibited host-associated differentiation without geographic isolation, 18% showed the opposite, and 21% were equivocal, insofar as analyses of molecular variance and haplotype networks yielded incongruent patterns. Variation in dietary breadth among community members suggests that speciation by specialization is an important, but not universal, mechanism for diversification of tropical Lepidoptera. Geographically widespread haplotypes challenge predictions of vicariance biogeography. Dispersal is important, and Lepidoptera communities appear to be highly dynamic according to the various phylogeographic histories of component species. Population genetic comparisons among herbivores of major tropical and temperate regions are needed to test predictions of ecological theory and evaluate global patterns of biodiversity. C1 [Craft, Kathleen J.; Weiblen, George D.] Univ Minnesota, Dept Plant Biol, St Paul, MN 55108 USA. [Pauls, Steffen U.] Univ Minnesota, Dept Entomol, St Paul, MN 55108 USA. [Darrow, Karolyn; Miller, Scott E.; Helgen, Lauren E.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. [Hebert, Paul D. N.] Univ Guelph, Biodivers Inst Ontario, Guelph, ON N1G 2W1, Canada. [Novotny, Vojtech] Univ S Bohemia, Czech Acad Sci, Inst Entomol, Ceske Budejovice 37005, Czech Republic. [Novotny, Vojtech] Univ S Bohemia, Dept Zool, Ceske Budejovice 37005, Czech Republic. RP Weiblen, GD (reprint author), Univ Minnesota, Dept Plant Biol, St Paul, MN 55108 USA. EM gweiblen@umn.edu RI Pauls, Steffen/C-2192-2011; Hebert, Paul/C-4161-2013; Novotny, Vojtech/G-9434-2014; OI Hebert, Paul/0000-0002-3081-6700; Novotny, Vojtech/0000-0001-7918-8023; Miller, Scott/0000-0002-4138-1378 FU National Science Foundation [DEB 9628840, 9707928, 0211591, 0515678]; Agencies of the Czech Republic [206/09/0115, 206/08/H044]; Czech Academy of Sciences [AA600960712, AV0Z50070508]; Czech Ministry of Education [LC06073, ME916, ME9082, MSM6007665801]; Darwin Initiative for the Survival of Species; David and Lucile Packard Fellowship in Science and Engineering; Gordon and Betty Moore Foundation; German Academy of Sciences Leopoldina [BMBF-LPD 9901/8-169] FX We thank the New Guinea Binatang Research Center staff, the more than 150 insect collectors from communities named in Fig. 1, J. D. Holloway, M. Horak, J. Miller, J. Brown, E. G. Munroe, M. Shaffer, and K. Tuck for technical and taxonomic assistance. We also thank three anonymous reviewers, V. Hypsa, and P. Tiffin for their comments on the manuscript. This paper is based on work supported by the National Science Foundation under Grants DEB 9628840, 9707928, 0211591, and 0515678. The work was also supported by grants from the Grant Agencies of the Czech Republic (206/09/0115 and 206/08/H044), Czech Academy of Sciences (AA600960712 and AV0Z50070508), Czech Ministry of Education (LC06073, ME916, ME9082, and MSM6007665801), Darwin Initiative for the Survival of Species, the David and Lucile Packard Fellowship in Science and Engineering ( to G. D. W.), the Gordon and Betty Moore Foundation ( to P.D.N.H.), and the German Academy of Sciences Leopoldina (BMBF-LPD 9901/8-169, to S. U. P.). Finally, we acknowledge the cooperation of the Papua New Guinea Department of Environment and Conservation, National Research Institute, Forest Research Institute, and National Agricultural Research Institute. NR 42 TC 56 Z9 62 U1 5 U2 48 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD MAR 16 PY 2010 VL 107 IS 11 BP 5041 EP 5046 DI 10.1073/pnas.0913084107 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 570YI UT WOS:000275714300044 PM 20202924 ER PT J AU Merrill, WL Hard, RJ Mabry, JB Fritz, GJ Adams, KR Roney, JR MacWilliams, AC AF Merrill, William L. Hard, Robert J. Mabry, Jonathan B. Fritz, Gayle J. Adams, Karen R. Roney, John R. MacWilliams, A. C. TI Reply to Hill and Brown: Maize and Uto-Aztecan cultural history SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Letter C1 [Merrill, William L.] Natl Museum Nat Hist, Smithsonian Inst, Dept Anthropol, Washington, DC 20013 USA. [Hard, Robert J.] Univ Texas, Dept Anthropol, San Antonio, TX 78249 USA. [Mabry, Jonathan B.] City Tucson, Hist Preservat Off, Tucson, AZ 85726 USA. [Fritz, Gayle J.] Washington Univ, Dept Anthropol, St Louis, MO 63130 USA. [Adams, Karen R.] Crow Canyon Archaeol Ctr, Cortez, CO 81321 USA. [Roney, John R.] Colinas Cultural Resource Consulting, Albuquerque, NM 87107 USA. [MacWilliams, A. C.] Univ Calgary, Dept Archaeol, Calgary, AB T2N 1N4, Canada. RP Hard, RJ (reprint author), Univ Texas, Dept Anthropol, San Antonio, TX 78249 USA. EM robert.hard@utsa.edu NR 11 TC 2 Z9 2 U1 0 U2 1 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD MAR 16 PY 2010 VL 107 IS 11 BP E35 EP E36 DI 10.1073/pnas.1000923107 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 570YI UT WOS:000275714300087 ER PT J AU Runyon, JB Robinson, H AF Runyon, Justin B. Robinson, Harold TI Hurleyella, a new genus of Nearctic Dolichopodidae (Diptera) SO ZOOTAXA LA English DT Article DE long-legged flies; Medeterinae; micro-dolichopodid; Enlinia; Harmstonia; Microcyrtura; Microchrysotus; Micromedetera ID REVISION AB The new micro-dolichopodid genus Hurleyella and two new species, H. cumberlandensis and H. brooksi are described from the Nearctic. Hurleyella resembles the subfamily Medeterinae in having the legs bare of major setae, a depressed posterior mesonotum, and concave dorsal postcranium, but the complex male genitalia is unlike the relatively simple structure of traditional Medeterinae (e. g., Medetera, Thrypyicus, Corindia, etc.). Until the relationship of Hurleyella to other genera can be determined, and the limits of dolichopodid subfamilies refined, it should be considered as incertae sedis. C1 [Runyon, Justin B.] US Forest Serv, Rocky Mt Res Stn, USDA, Bozeman, MT 59717 USA. [Runyon, Justin B.] Montana State Univ, Bozeman, MT 59717 USA. [Robinson, Harold] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. RP Runyon, JB (reprint author), US Forest Serv, Rocky Mt Res Stn, USDA, 1648 S 7th Ave, Bozeman, MT 59717 USA. EM jrunyon@montana.edu OI Runyon, Justin B./0000-0002-0271-0511 NR 20 TC 2 Z9 2 U1 0 U2 0 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD MAR 16 PY 2010 IS 2400 BP 57 EP 65 PG 9 WC Zoology SC Zoology GA 569MC UT WOS:000275600200006 ER PT J AU Penniston-Dorland, SC Sorensen, SS Ash, RD Khadke, SV AF Penniston-Dorland, Sarah C. Sorensen, Sorena S. Ash, Richard D. Khadke, Supriya V. TI Lithium isotopes as a tracer of fluids in a subduction zone melange: Franciscan Complex, CA SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE lithium isotopes; subduction zone; fluid; infiltration; diffusion; Franciscan ID MC-ICP-MS; OCEANIC-CRUST; OROGENIC ECLOGITES; CONTINENTAL-CRUST; METAMORPHIC ROCKS; AQUEOUS FLUIDS; FRACTIONATION; CALIFORNIA; LI; DIFFUSION AB High-grade blocks of eclogite, blueschist, and garnet amphibolite found in melange terrains in the Franciscan Complex, CA display petrologic and geochemical evidence for a complicated history of interactions with aqueous fluids. These blocks have features (actinolitic rinds, a blueschist layer) that have petrologic and geochemical indicators of interaction with retrograde aqueous fluids. Lithium concentrations and isotopic compositions of different portions of three high-grade blocks are different from those of MORB (their presumed protolith) and show systematic variations associated with fluid-related features. Block cores and an eclogite layer have high whole-rock Li concentrations relative to MORB (17 to 39 ppm) and low to moderate delta(7)Li (0.4 to 2.1 parts per thousand). This range of values is inconsistent with dehydration of MORB and is interpreted as the product of infiltration of aqueous fluids with an elevated Li concentration and low delta(7)Li. Rinds and a blueschist layer exhibit lower Li concentrations (7 to 24 ppm) and higher delta(7)Li (2.7 to 4.4 parts per thousand). The differences between cores and rinds, and the eclogite and blueschist layers are interpreted as the product of retrograde infiltration of an aqueous fluid with low Li concentrations and high delta(7)Li. Results of a small-scale traverse across the boundary between the blueschist and eclogite layers show that the boundary is gradational over similar to 0.5 cm, suggesting small-scale cross-layer diffusion/dispersion associated with the fluid infiltration. The high Li concentrations and low delta(7)Li of block cores suggests that the source of early fluids was likely subducted sedimentary rocks. The lower Li concentrations and higher delta(7)Li values of the rinds and blueschist layers do not fully constrain the source of retrograde fluids, but indicate that the fluid source likely had a lower Li concentration and higher delta(7)Li. (c) 2010 Elsevier By. All rights reserved. C1 [Penniston-Dorland, Sarah C.; Ash, Richard D.; Khadke, Supriya V.] Univ Maryland, Dept Geol, College Pk, MD 20742 USA. [Sorensen, Sorena S.] Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. RP Penniston-Dorland, SC (reprint author), Univ Maryland, Dept Geol, College Pk, MD 20742 USA. EM sarahpd@geol.umd.edu FU NSF [EAR-0609689, EAR-0911100]; Maryland NanoCenter FX We thank Roberta Rudnick and William McDonough for assistance with Li isotope analysis supported by NSF grant EAR-0609689. We thank the NSF for support to SP-D, grant EAR-0911100. We thank Philip Piccoli for assistance with the electron probe microanalyzer. We acknowledge the support of the Maryland NanoCenter and its Nisplab which is supported in part by NSF. We thank Mark Cloos and Roberta Rudnick for helpful comments on an early draft. Jay Ague and Fang-Zhen Teng are thanked for their constructive reviews. We thank Diane Moore for providing field notes from the Mt. Hamilton locality. NR 75 TC 38 Z9 39 U1 1 U2 29 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0012-821X J9 EARTH PLANET SC LETT JI Earth Planet. Sci. Lett. PD MAR 15 PY 2010 VL 292 IS 1-2 BP 181 EP 190 DI 10.1016/j.epsl.2010.01.034 PG 10 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 576IX UT WOS:000276138900018 ER PT J AU Yunes, N Psaltis, D Ozel, F Loeb, A AF Yunes, Nicolas Psaltis, Dimitrios Ozel, Feryal Loeb, Abraham TI Constraining parity violation in gravity with measurements of neutron-star moments of inertia SO PHYSICAL REVIEW D LA English DT Article ID PREFERRED-FRAME THEORIES; RAY MILLISECOND PULSARS; RELATIVISTIC GRAVITY; BLACK-HOLES; CONSERVATION LAWS; SCALAR THEORIES; STRING THEORY; FIELD; NONLOCALITY; LAGRANGIANS AB Neutron stars are sensitive laboratories for testing general relativity, especially when considering deviations where velocities are relativistic and gravitational fields are strong. One such deviation is described by dynamical, Chern-Simons modified gravity, where the Einstein-Hilbert action is modified through the addition of the gravitational parity-violating Pontryagin density coupled to a field. This four-dimensional effective theory arises naturally both in perturbative and nonperturbative string theory, loop quantum gravity, and generic effective field theory expansions. We calculate here Chern-Simons modifications to the properties and gravitational fields of slowly spinning neutron stars. We find that the Chern-Simons correction affects only the gravitomagnetic sector of the metric to leading order, thus introducing modifications to the moment-of-inertia but not to the mass-radius relation. We show that an observational determination of the moment-of-inertia to an accuracy of 10%, as is expected from near-future observations of the double pulsar, will place a constraint on the Chern-Simons coupling constant of xi(1/4) less than or similar to 5 km, which is at least three-orders of magnitude stronger than the previous strongest bound. C1 [Yunes, Nicolas] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA. [Psaltis, Dimitrios; Ozel, Feryal] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. [Psaltis, Dimitrios; Ozel, Feryal; Loeb, Abraham] Harvard Smithsonian Ctr Astrophys, ITC, Cambridge, MA 02138 USA. RP Yunes, N (reprint author), Princeton Univ, Dept Phys, Princeton, NJ 08544 USA. FU NSF [PHY-0745779, PHY-0746549, AST-0708640, AST-0907890] FX We are grateful to Ramesh Narayan for his insights and assistance with the numerical solutions, as well as to David Spergel, Frans Pretorius and Branson Stephens for useful suggestions and comments. Some calculations used the computer algebra systems MAPLE, in combination with the GRTensorII package [ 95]. N. Y. acknowledges the support of the NSF grant PHY-0745779. D. P. acknowledges the support of the NSF CAREER Grant No. PHY-0746549. This work was supported in part by NSF grant AST-0708640 for F.O .and NSF grant AST-0907890 for A. L.. NR 93 TC 20 Z9 20 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 MAR 15 PY 2010 VL 81 IS 6 AR 064020 DI 10.1103/PhysRevD.81.064020 PG 15 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 577BL UT WOS:000276195700070 ER PT J AU Xiao, JF Zhuang, QL Law, BE Chen, JQ Baldocchi, DD Cook, DR Oren, R Richardson, AD Wharton, S Ma, SY Martin, TA Verma, SB Suyker, AE Scott, RL Monson, RK Litvak, M Hollinger, DY Sun, G Davis, KJ Bolstad, PV Burns, SP Curtis, PS Drake, BG Falk, M Fischer, ML Foster, DR Gu, LH Hadley, JL Katul, GG Roser, Y McNulty, S Meyers, TP Munger, JW Noormets, A Oechel, WC Paw, KT Schmid, HP Starr, G Torn, MS Wofsy, SC AF Xiao, Jingfeng Zhuang, Qianlai Law, Beverly E. Chen, Jiquan Baldocchi, Dennis D. Cook, David R. Oren, Ram Richardson, Andrew D. Wharton, Sonia Ma, Siyan Martin, Timothy A. Verma, Shashi B. Suyker, Andrew E. Scott, Russell L. Monson, Russell K. Litvak, Marcy Hollinger, David Y. Sun, Ge Davis, Kenneth J. Bolstad, Paul V. Burns, Sean P. Curtis, Peter S. Drake, Bert G. Falk, Matthias Fischer, Marc L. Foster, David R. Gu, Lianhong Hadley, Julian L. Katul, Gabriel G. Matamala, Roser McNulty, Steve Meyers, Tilden P. Munger, J. William Noormets, Asko Oechel, Walter C. Paw U, Kyaw Tha Schmid, Hans Peter Starr, Gregory Torn, Margaret S. Wofsy, Steven C. TI A continuous measure of gross primary production for the conterminous United States derived from MODIS and AmeriFlux data SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Gross primary productivity; MODIS; AmeriFlux; Eddy covariance; Regression tree; US; Carbon fluxes; Interannual variability; Satellite data; Biomes ID CARBON-DIOXIDE EXCHANGE; NET ECOSYSTEM EXCHANGE; EDDY-COVARIANCE MEASUREMENTS; ELEVATED ATMOSPHERIC CO2; DIFFERENCE WATER INDEX; NORTHERN GREAT-PLAINS; LIGHT-USE EFFICIENCY; FOREST ECOSYSTEMS; PONDEROSA PINE; DECIDUOUS FOREST AB The quantification of carbon fluxes between the terrestrial biosphere and the atmosphere is of scientific importance and also relevant to climate-policy making. Eddy covariance flux towers provide continuous measurements of ecosystem-level exchange of carbon dioxide spanning diurnal, synoptic, seasonal, and interannual time scales. However, these measurements only represent the fluxes at the scale of the tower footprint. Here we used remotely sensed data from the Moderate Resolution Imaging Spectroradiometer (MODIS) to upscale gross primary productivity (GPP) data from eddy covariance flux towers to the continental scale. We first combined GPP and MODIS data for 42 AmeriFlux towers encompassing a wide range of ecosystem and climate types to develop a predictive GPP model using a regression tree approach. The predictive model was trained using observed GPP over the period 2000-2004, and was validated using observed GPP over the period 2005-2006 and leave-one-out cross-validation. Our model predicted GPP fairly well at the site level. We then used the model to estimate GPP for each I km x I km cell across the U.S. for each 8-day interval over the period from February 2000 to December 2006 using MODIS data. Our GPP estimates provide a spatially and temporally continuous measure of gross primary production for the U.S. that is a highly constrained by eddy covariance flux data. Our study demonstrated that our empirical approach is effective for upscaling eddy flux GPP data to the continental scale and producing continuous GPP estimates across multiple biomes. With these estimates, we then examined the patterns, magnitude, and interannual variability of GPP. We estimated a gross carbon uptake between 6.91 and 7.33 Pg C yr(-1) for the conterminous U.S. Drought, fires, and hurricanes reduced annual GPP at regional scales and could have a significant impact on the U.S. net ecosystem carbon exchange. The sources of the interannual variability of U.S. GPP were dominated by these extreme climate events and disturbances. (C) 2009 Elsevier Inc. All rights reserved. C1 [Xiao, Jingfeng] Purdue Univ, Purdue Climate Change Res Ctr, Dept Earth & Atmospher Sci, W Lafayette, IN 47907 USA. [Zhuang, Qianlai] Purdue Univ, Purdue Climate Change Res Ctr, Dept Earth & Atmospher Sci, Dept Agron, W Lafayette, IN 47907 USA. [Law, Beverly E.] Oregon State Univ, Coll Forestry, Corvallis, OR 97331 USA. [Chen, Jiquan] Univ Toledo, Dept Environm Sci, Toledo, OH 43606 USA. [Baldocchi, Dennis D.; Ma, Siyan] Univ Calif Berkeley, Dept Environm Sci Policy & Management, Ecosyst Sci Div, Berkeley, CA 94720 USA. [Cook, David R.] Argonne Natl Lab, Div Environm Sci, Argonne, IL 60439 USA. [Oren, Ram; Katul, Gabriel G.] Duke Univ, Nicholas Sch Environm, Durham, NC 27708 USA. [Richardson, Andrew D.] Harvard Univ, Dept Organism & Evolutionary Biol, Cambridge, MA 02138 USA. [Wharton, Sonia; Falk, Matthias; Paw U, Kyaw Tha] Univ Calif Davis, Dept Land Air & Water Resources, Davis, CA 95616 USA. [Martin, Timothy A.] Univ Florida, Sch Forest Resources & Conservat, Gainesville, FL 32611 USA. [Verma, Shashi B.; Suyker, Andrew E.] Univ Nebraska, Sch Nat Resources, Lincoln, NE 68583 USA. [Scott, Russell L.] USDA ARS, SW Watershed Res Ctr, Tucson, AZ 85719 USA. [Monson, Russell K.; Burns, Sean P.] Univ Colorado, Dept Ecol & Evolutionary Biol, Boulder, CO 80309 USA. [Litvak, Marcy] Univ New Mexico, Dept Biol, Albuquerque, NM 87131 USA. [Hollinger, David Y.] US Forest Serv, USDA, NE Res Stn, Durham, NH 03824 USA. [Sun, Ge; McNulty, Steve] US Forest Serv, USDA, So Res Stn, Raleigh, NC 27606 USA. [Davis, Kenneth J.] Univ New Hampshire, Complex Syst Res Ctr, Durham, NH 03824 USA. [Bolstad, Paul V.] Univ Minnesota, Dept Forest Resources, St Paul, MN 55108 USA. [Curtis, Peter S.] Ohio State Univ, Dept Evolut Ecol & Organismal Biol, Columbus, OH 43210 USA. [Drake, Bert G.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Fischer, Marc L.] Univ Calif Berkeley, Lawrence Berkeley Lab, Environm Energy Technol Div, Dept Atmospher Sci, Berkeley, CA 94720 USA. [Foster, David R.] Harvard Univ, Dept Organism & Evolutionary Biol, Petersham, MA 01366 USA. [Gu, Lianhong] Oak Ridge Natl Lab, Div Environm Sci, Oak Ridge, TN 37831 USA. [Matamala, Roser] Argonne Natl Lab, Biosci Div, Argonne, IL 60439 USA. [Meyers, Tilden P.] NOAA, ARL, Atmospher Turbulence & Diffus Div, Oak Ridge, TN 37831 USA. [Wofsy, Steven C.] Harvard Univ, Dept Earth & Planetary Sci, Div Engn & Appl Sci, Cambridge, MA 02138 USA. [Noormets, Asko] N Carolina State Univ, Dept Forestry & Environm Resources, Raleigh, NC 27695 USA. [Noormets, Asko] N Carolina State Univ, So Global Change Program, Raleigh, NC 27695 USA. [Oechel, Walter C.] San Diego State Univ, Dept Biol, San Diego, CA 92182 USA. [Schmid, Hans Peter] Indiana Univ, Dept Geog, Bloomington, IN 47405 USA. [Schmid, Hans Peter] FZK IMK IFU, Res Ctr Karlsruhe, Inst Meteorol & Climate Res, D-82467 Garmisch Partenkirchen, Germany. [Starr, Gregory] Univ Alabama, Dept Biol Sci, Tuscaloosa, AL 35487 USA. [Torn, Margaret S.] Univ Calif Berkeley, Lawrence Berkeley Lab, Div Earth Sci, Berkeley, CA 94720 USA. RP Xiao, JF (reprint author), Penn State Univ, Dept Meteorol, 503 Walker Bldg, University Pk, PA 16802 USA. EM j.xiao@unh.edu RI Munger, J/H-4502-2013; Oechel, Walter/F-9361-2010; Gu, Lianhong/H-8241-2014; Chen, Jiquan/D-1955-2009; Noormets, Asko/A-7257-2009; Katul, Gabriel/A-7210-2008; Richardson, Andrew/F-5691-2011; Hollinger, David/G-7185-2012; Schmid, Hans Peter/I-1224-2012; Garmisch-Pa, Ifu/H-9902-2014; Baldocchi, Dennis/A-1625-2009; Torn, Margaret/D-2305-2015; Meyers, Tilden/C-6633-2016 OI Munger, J/0000-0002-1042-8452; Oechel, Walter/0000-0002-3504-026X; Gu, Lianhong/0000-0001-5756-8738; Law, Beverly/0000-0002-1605-1203; Martin, Timothy/0000-0002-7872-4194; Noormets, Asko/0000-0003-2221-2111; Katul, Gabriel/0000-0001-9768-3693; Richardson, Andrew/0000-0002-0148-6714; Schmid, Hans Peter/0000-0001-9076-4466; Baldocchi, Dennis/0000-0003-3496-4919; FU National Science Foundation (NSF) [EAR-0630319] FX This research was partly supported by the National Science Foundation (NSF) Carbon and Water Program (EAR-0630319). We thank the principal investigators of the MODIS data products including Drs. A.R. Huete, R.B. Myneni, S.W. Running, E.F. Vermote, and Z. Wan. We also thank D.A. Sims, T.A. Boden, S.K.S. Vannan, M. Zhao, Z. Wan, and L Delp for helpful discussion. The MODIS data products were obtained from the Oak Ridge National Laboratory (ORNL) Distributed Active Archive Center (DAAC) and the Earth Observing System (EOS) Data Gateway for making these products available. The PRISM climate database was provided by the PRISM Group, Oregon State University (http://www.prismclimate.org). NR 102 TC 112 Z9 119 U1 8 U2 65 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 EI 1879-0704 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD MAR 15 PY 2010 VL 114 IS 3 BP 576 EP 591 DI 10.1016/j.rse.2009.10.013 PG 16 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA 559JP UT WOS:000274820700012 ER PT J AU Pennisi, E West-Eberhard, MJ AF Pennisi, E. West-Eberhard, Mary Jane TI Sex and social structure (October, pg 518, 2009) SO SCIENCE LA English DT Correction C1 [West-Eberhard, Mary Jane] Smithsonian Trop Res Inst, Balboa, Panama. NR 1 TC 0 Z9 0 U1 1 U2 8 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 MAR 12 PY 2010 VL 327 IS 5971 BP 1327 EP 1327 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 567CA UT WOS:000275418700021 ER PT J AU Norrbom, AL Sutton, BD Steck, GJ Monzon, J AF Norrbom, Allen L. Sutton, Bruce D. Steck, Gary J. Monzon, Jose TI New genera, species and host plant records of Nearctic and Neotropical Tephritidae (Diptera) SO ZOOTAXA LA English DT Article DE Diptera; Tephritidae; Tephritinae; taxonomy; host plant; Asteraceae ID IMMATURE STAGES; SOUTHERN-CALIFORNIA; LIFE-HISTORY; ASTERACEAE; BIOLOGY AB Three new genera and five new species of Tephritidae (Diptera) are described from the Nearctic and Neotropical Regions. The new genera are: Agallamyia Norrbom (type species: A. pendula Norrbom, n. sp.), Neosphaeniscus Norrbom (type species: Euribia m-nigrum Hendel), and Phacelochaeta Norrbom (type species: Procecidochares quinquefasciata Hendel). The new species include: Acidogona stecki Norrbom (Guatemala, Mexico: Chiapas), Agallamyia pendula Norrbom (Guatemala), Phacelochaeta obliqua Norrbom (Ecuador), Procecidochares suttoni Norrbom (Guatemala), Stenopa mexicana Norrbom (Mexico). Five new generic synonyms are proposed: Cecidocharella Hendel, 1936 = Dracontomyia Becker, 1919; Gerrhoceras Hering, 1942 = Pyrgotoides Curran, 1934; Stoneola Hering, 1941 = Rhagoletis Loew, 1862; Strobelia Rondani, 1868 = Rachiptera Bigot, 1859; and Xenochaeta Snow, 1894 = Acidogona Loew, 1873. The following 41 new combinations are proposed: Acidogona dichromata (Snow), Dictyotrypeta crenulata (Wulp), D. incisa (Wulp), Dioxyna crockeri (Curran), Dracontomyia tucumana (Aczel), D. borrichia (Bush & Huettel), and D. elegans (Hendel), Homoeothrix aberrans (Schiner), Neosphaeniscus m-nigrum (Hendel) and N. flexuosus (Bigot), Paracantha trinotata (Foote), Phacelochaeta quinquefasciata (Hendel) and P. quinquevittata (Norrbom), Plaumannimyia ameghinoi (Brethes), P. coelestina (Hering), P. delicatella (Blanchard), P. difficilis (Malloch), P. dolores (Hering), P. eugenia (Wulp), P. flava (Adams), P. hestiae (Hendel), P. imitatrix (Hering), P. miseta (Hering), P. plagiata (Blanchard), P. scutellata (Seguy), P. setulosa (Malloch), P. subaster (Malloch), P. suspecta (Malloch), P. thomsoni (Hendel), P. titschacki (Hering), and P. valdesiana (Gandolfo & Norrbom), Pyrgotoides paradoxus (Hering) and P. peruvianus (Korytkowski), Rachiptera alboguttata (Hendel), R. baccharidis (Rondani), R. bimaculata (Hendel), R. ferruginea (Hendel), R. lutulenta (Hendel), R. parallela (Hendel), and R. rubiginosa (Rondani), and Rhagoletis fuscobasalis (Hering). A lectotype is designated for R. fuscobasalis. New distribution and host plant records also are reported. C1 [Norrbom, Allen L.] ARS, Systemat Entomol Lab, USDA, Smithsonian Inst, Washington, DC 20013 USA. [Sutton, Bruce D.; Steck, Gary J.] Florida Dept Agr & Consumer Serv, Gainesville, FL 32614 USA. [Monzon, Jose] Univ Valle Guatemala, Lab Entomol Sistemat, Guatemala City 01901, Guatemala. RP Norrbom, AL (reprint author), ARS, Systemat Entomol Lab, USDA, Smithsonian Inst, POB 37012,MRC 168, Washington, DC 20013 USA. EM allen.norrbom@ars.usda.gov; tonb@doacs.state.fl.us; steckg@doacs.state.fl.us; dynastes@intelnett.com NR 43 TC 1 Z9 1 U1 1 U2 1 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD MAR 12 PY 2010 IS 2398 BP 1 EP 65 PG 65 WC Zoology SC Zoology GA 567NR UT WOS:000275454400001 ER PT J AU Woodley, NE AF Woodley, Norman E. TI Parameristomerinx copelandi-a new genus and species of Afrotropical Pachygastrinae and a new generic synonym of Dolichodema Kertesz (Diptera: Stratiomyidae) SO ZOOTAXA LA English DT Article DE Diptera; Stratiomyidae; Pachygastrinae; Parameristomerinx; Dolichodema; Afrotropical AB A new genus and species, Parameristomerinx copelandi gen. et sp. n. (Diptera: Stratiomyidae: Pachygastrinae) is described from material from Kenya. This genus is similar to the Afrotropical genera Meristomerinx Enderlein, 1914 and Meristomeringina James, 1952. A new generic synonym is also proposed, Nemodema Lindner, 1958 = Dolichodema Kertesz, 1916, syn. n. A key is included for the six genera related to Meristomerinx. C1 ARS, Systemat Entomol Lab, PSI, USDA,Smithsonian Inst NHB 168, Washington, DC 20013 USA. RP Woodley, NE (reprint author), ARS, Systemat Entomol Lab, PSI, USDA,Smithsonian Inst NHB 168, POB 37012, Washington, DC 20013 USA. EM norman.woodley@ars.usda.gov RI Woodley, Norman/M-6160-2014 NR 10 TC 1 Z9 1 U1 0 U2 0 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD MAR 12 PY 2010 IS 2397 BP 41 EP 47 PG 7 WC Zoology SC Zoology GA 567NQ UT WOS:000275454300004 ER PT J AU Mendelson, JR Mulcahy, DG AF Mendelson, Joseph R., III Mulcahy, Daniel G. TI A new species of toad (Bufonidae: Incilius) from central Panama SO ZOOTAXA LA English DT Article DE Anura; Bufonidae; Panama; Cocle Province; new species; Incilius karenlipsae; Incilius coniferus ID BUFO VALLICEPS; ANURA; PERU AB We describe Incilius karenlipsae sp. nov., a new species of toad known from a single locality in the Cordillera de Talamanca of central Panama. We describe this species based on a single individual of perhaps what is now an extinct species. We present mitochondrial sequence data from cyt b (675 base-pairs, bp) and 16S (566 bp) to infer its phylogenetic placement among other bufonids. The new species is closely related to the more widespread species I. coniferus, but is clearly distinguishable from it by its larger size, vestigial parotoid glands and extensively developed fleshy pads on the hands and feet. C1 [Mendelson, Joseph R., III] Zoo Atlanta, Dept Herpetol, Atlanta, GA 30315 USA. [Mulcahy, Daniel G.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Mendelson, JR (reprint author), Zoo Atlanta, Dept Herpetol, 800 Cherokee Ave SE, Atlanta, GA 30315 USA. EM jmendelson@zooatlanta.org FU JWS; Department of Biology; BYU FX For considerable logistical assistance during field efforts in 2005, we thank M. Ryan, S. Connelly, H. Ross, E. Griffith, M. Urriola, R. Gagliardo, R. Ibanez, K. Zippel, K. Lips, O. Arosemana, and especially George B. and Mary S. Rabb. All research was conducted under permit SEX/A-81-05 granted by the Autoridad Nacional del Ambiente of the Republic of Panama. Access to comparative materials was granted by D. Frost and D. Kizirian (AMNH), and R. McDiarmid and S. Gotte (USNM). The living collections at Zoo Atlanta are maintained thanks to the diligence of B. Lock, D. Brothers, L. Wyrwich, E. Kabay, and J. Brock; R. Hill and R. Gagliardo also provided considerable assistance. Helpful advice and assistance with the photographic illustrations were provided by M. Bustamante and J. Brock; photographs were made by E. Kabay. Helpful comments on the manuscript were provided by R. McDiarmid, J. Pramuk, and J. Townsend. Molecular work was done in the lab of J. W. Sites, Jr., at Brigham Young University and was funded by JWS, the Department of Biology, and the Mentoring for Undergraduate Research Program at BYU. NR 25 TC 5 Z9 7 U1 0 U2 0 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD MAR 11 PY 2010 IS 2396 BP 61 EP 68 PG 8 WC Zoology SC Zoology GA 566KY UT WOS:000275370300005 ER PT J AU Cenko, SB Frail, DA Harrison, FA Kulkarni, SR Nakar, E Chandra, PC Butler, NR Fox, DB Gal-Yam, A Kasliwal, MM Kelemen, J Moon, DS Ofek, EO Price, PA Rau, A Soderberg, AM Teplitz, HI Werner, MW Bock, DCJ Bloom, JS Starr, DA Filippenko, AV Chevalier, RA Gehrels, N Nousek, JN Piran, T AF Cenko, S. B. Frail, D. A. Harrison, F. A. Kulkarni, S. R. Nakar, E. Chandra, P. C. Butler, N. R. Fox, D. B. Gal-Yam, A. Kasliwal, M. M. Kelemen, J. Moon, D. -S Ofek, E. O. Price, P. A. Rau, A. Soderberg, A. M. Teplitz, H. I. Werner, M. W. Bock, D. C. -J. Bloom, J. S. Starr, D. A. Filippenko, A. V. Chevalier, R. A. Gehrels, N. Nousek, J. N. Piran, T. TI THE COLLIMATION AND ENERGETICS OF THE BRIGHTEST SWIFT GAMMA-RAY BURSTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma-ray burst: general; X-rays: individual (GRB 050820A,GRB 050904, GRB 060418, GRB 070125, GRB 080319B) ID AFTERGLOW LIGHT CURVES; X-RAY; GRB 080319B; INTERNAL SHOCKS; BLAST WAVE; JET BREAKS; MULTIWAVELENGTH OBSERVATIONS; RELATIVISTIC TURBULENCE; CIRCUMSTELLAR MEDIUM; MILLISECOND PULSARS AB Long-duration gamma-ray bursts (GRBs) are widely believed to be highly collimated explosions ( bipolar conical outflows with half-opening angle theta approximate to 1 degrees -10 degrees). As a result of this beaming factor, the true energy release from a GRB is usually several orders of magnitude smaller than the observed isotropic value. Measuring this opening angle, typically inferred from an achromatic steepening in the afterglow light curve (a "jet" break), has proven exceedingly difficult in the Swift era. Here, we undertake a study of five of the brightest ( in terms of the isotropic prompt. gamma-ray energy release, E(gamma,iso)) GRBs in the Swift era to search for jet breaks and hence constrain the collimation-corrected energy release. We present multi-wavelength ( radio through X-ray) observations of GRBs 050820A, 060418, and 080319B, and construct afterglow models to extract the opening angle and beaming-corrected energy release for all three events. Together with results from previous analyses of GRBs 050904 and 070125, we find evidence for an achromatic jet break in all five events, strongly supporting the canonical picture of GRBs as collimated explosions. The most natural explanation for the lack of observed jet breaks from most Swift GRBs is therefore selection effects. However, the opening angles for the events in our sample are larger than would be expected if all GRBs had a canonical energy release of similar to 10(51) erg. The total energy release we measure for the "hyper-energetic" (E(tot) greater than or similar to 10(52) erg) events in our sample is large enough to start challenging models with a magnetar as the compact central remnant. C1 [Cenko, S. B.; Butler, N. R.; Bloom, J. S.; Starr, D. A.; Filippenko, A. V.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Frail, D. A.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Harrison, F. A.] CALTECH, Space Radiat Lab, Pasadena, CA 91125 USA. [Kulkarni, S. R.; Kasliwal, M. M.; Ofek, E. O.; Rau, A.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Nakar, E.] Tel Aviv Univ, Raymond & Beverly Sackler Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Chandra, P. C.] Royal Mil Coll Canada, Dept Phys, Kingston, ON, Canada. [Fox, D. B.; Nousek, J. N.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Gal-Yam, A.] Weizmann Inst Sci, Benoziyo Ctr Astrophys, IL-76100 Rehovot, Israel. [Kelemen, J.] Konkoly Observ Budapest, H-1525 Budapest, Hungary. [Moon, D. -S] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Price, P. A.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Rau, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Soderberg, A. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Teplitz, H. I.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Werner, M. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bock, D. C. -J.] Combined Array Res Millimeter Wave Astron, Big Pine, CA 93513 USA. [Starr, D. A.] Las Cumbres Observ Global Telescope Network Inc, Santa Barbara, CA 93117 USA. [Chevalier, R. A.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Gehrels, N.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20770 USA. [Piran, T.] Hebrew Univ Jerusalem, Racah Inst Phys, IL-91904 Jerusalem, Israel. RP Cenko, SB (reprint author), Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RI Gehrels, Neil/D-2971-2012 FU Gary and Cynthia Bengier; Richard and Rhoda Goldman Fund; NASA/Swift [NNG06GI86G, NNX09AL08G, NAS5-00136, NNG06GH61G, NAS 5-26555, NNG06GH50G, NNX08AN84G]; NSF [AST-0607485, AST-0908886]; Israeli Science Foundation; EU; Benoziyo Center for Astrophysics; Peter and Patricia Gruber Awards; William Z. and Eda Bess Novick New Scientists Fund at the Weizmann Institute; ERC [P60]; Gordon and Betty Moore Foundation; Kenneth T. and Eileen L. Norris Foundation; Associates of the California Institute of Technology; states of California, Illinois, and Maryland; Harvard University Milton Fund; SAO; UC Berkeley; W. M. Keck Foundation; [GO-10551] FX S. B. C. and A. V. F. acknowledge generous support from Gary and Cynthia Bengier, the Richard and Rhoda Goldman Fund, NASA/Swift grants NNG06GI86G and NNX09AL08G, and NSF grants AST-0607485 and AST-0908886. A. G. acknowledges support 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. J.N.N. is supported by NASA contract NAS5-00136. T. P. acknowledges support from an ERC advanced research grant. P60 operations are funded in part by NASA through the Swift Guest Investigator Program ( grant number NNG06GH61G). Based on observations made with the NASA/ESA Hubble Space Telescope, obtained from the Data Archive at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These data are associated with program GO-10551. 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. We thank the SSC Director for an award of discretionary time and the Spitzer Operations team for their quick response to our request. This publication has made use of data obtained from the Swift interface of the High-Energy Astrophysics Archive (HEASARC), provided by NASA's Goddard Space Flight Center. Support for CARMA construction was derived from the Gordon and Betty Moore Foundation, the Kenneth T. and Eileen L. Norris Foundation, the Associates of the California Institute of Technology, the states of California, Illinois, and Maryland, and the NSF. Ongoing CARMA development and operations are supported by the NSF under a cooperative agreement, and by the CARMA partner universities. PAIRITEL is operated by the Smithsonian Astrophysical Observatory (SAO) and was made possible by a grant from the Harvard University Milton Fund, a camera loan from the University of Virginia, and continued support of the SAO and UC Berkeley. The PAIRITEL project is further supported by NASA/Swift Guest Investigator grants NNG06GH50G and NNX08AN84G. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the NASA; the observatory 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. NR 134 TC 64 Z9 65 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 MAR 10 PY 2010 VL 711 IS 2 BP 641 EP 654 DI 10.1088/0004-637X/711/2/641 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 559SN UT WOS:000274848100039 ER PT J AU Lee, JJ Park, S Hughes, JP Slane, PO Gaensler, BM Ghavamian, P Burrows, DN AF Lee, Jae-Joon Park, Sangwook Hughes, John P. Slane, Patrick O. Gaensler, B. M. Ghavamian, Parviz Burrows, David N. TI THE OUTER SHOCK OF THE OXYGEN-RICH SUPERNOVA REMNANT G292.0+1.8: EVIDENCE FOR THE INTERACTION WITH THE STELLAR WINDS FROM ITS MASSIVE PROGENITOR SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual objects (G292.0+1.8); ISM: supernova remnants; shock waves; stars: mass-loss; X-rays: ISM ID X-RAY-EMISSION; CORE-COLLAPSE; CASSIOPEIA-A; ELEMENTAL ABUNDANCES; PSR J1124-5916; RADIO-EMISSION; EVOLUTION; PULSAR; EJECTA; BUBBLES AB We study the outer-shock structure of the oxygen-rich supernova remnant G292.0+1.8 using a deep observation with the Chandra X-ray Observatory. We measure radial variations of the electron temperature and emission measure that we identify as the outer shock propagating into a medium with a radially decreasing density profile. The inferred ambient density structure is consistent with models for the circumstellar wind of a massive progenitor star rather than for a uniform interstellar medium. The estimated wind density (n(H) = 0.1-0.3 cm(-3)) at the current outer radius (similar to 7.7 pc) of the remnant is consistent with a slow wind from a red supergiant (RSG) star. The total mass of the wind is estimated to be similar to 15-40 M(circle dot) (depending on the estimated density range), assuming that the wind extended down to near the surface of the progenitor. The overall kinematics of G292.0+1.8 are consistent with the remnant expanding through the RSG wind. C1 [Lee, Jae-Joon; Park, Sangwook; Burrows, David N.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Hughes, John P.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Slane, Patrick O.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gaensler, B. M.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Ghavamian, Parviz] Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Lee, JJ (reprint author), Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. EM lee@astro.psu.edu RI Gaensler, Bryan/F-8655-2010; OI Gaensler, Bryan/0000-0002-3382-9558 FU SAO [G06-7049A, G06-7049B, G06-7049C]; Australian Research Council [FF0561298] FX This work was supported in parts by the SAO under Chandra grants G06-7049A (Penn State), G06-7049B (Johns Hopkins), and G06-7049C (Rutgers). B. M. G. acknowledges the support of a Federation Fellowship from the Australian Research Council through grant FF0561298. J. P. H. acknowledges fruitful discussions with Vikram Dwarkadas. NR 38 TC 12 Z9 12 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 MAR 10 PY 2010 VL 711 IS 2 BP 861 EP 869 DI 10.1088/0004-637X/711/2/861 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 559SN UT WOS:000274848100053 ER PT J AU Andrade-Velazquez, M Krongold, Y Elvis, M Nicastro, F Brickhouse, N Binette, L Mathur, S Jimenez-Bailon, E AF Andrade-Velazquez, Mercedes Krongold, Yair Elvis, Martin Nicastro, Fabrizio Brickhouse, Nancy Binette, Luc Mathur, Smita Jimenez-Bailon, Elena TI THE TWO-PHASE, TWO-VELOCITY IONIZED ABSORBER IN THE SEYFERT 1 GALAXY NGC 5548 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: Seyfert; quasars: absorption lines; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; TRANSMISSION GRATING SPECTROMETER; SUPERSOLAR METAL ABUNDANCES; X-RAY SPECTROSCOPY; XMM-NEWTON VIEW; WARM ABSORBER; ULTRAVIOLET ABSORBER; SPECTRAL VARIABILITY; PHYSICAL CONDITIONS; FAR-ULTRAVIOLET AB We present an analysis of X-ray high-quality grating spectra of the Seyfert 1 galaxy NGC 5548 using archival Chandra-High Energy Transmission Grating Spectrometer and Low Energy Transmission Grating Spectrometer observations for a total exposure time of 800 ks. The continuum emission (between 0.2 keV and 8 keV) is well represented by a power law (Gamma = 1.6) plus a blackbody component (kT = 0.1 keV). We find that the well-known X-ray warm absorber (WA) in this source consists of two different outflow velocity systems. One absorbing system has a velocity of -1110 +/- 150 km s(-1) and the other of -490 +/- 150 km s(-1). Recognizing the presence of these kinematically distinct components allows each system to be fitted independently, each with two absorption components with different ionization levels. The high-velocity system consists of two components, one with a temperature of 2.7 +/- 0.6 x 10(6) K, log U = 1.23, and another with a temperature of 5.8 +/- 1.0 x 10(5) K, log U = 0.67. The high-velocity, high-ionization component produces absorption by charge states Fe XXI-XXIV, while the high-velocity, low-ionization component produces absorption by Ne IX-X, Fe XVII-XX, and O VII-VIII. The low-velocity system also required two absorbing components, one with a temperature of 5.8 +/- 0.8 x 10(5) K, log U = 0.67, producing absorption by Ne IX-X, Fe XVII-XX, and O VII-VIII, and the other with a lower temperature of 3.5 +/- 0.35 x 10(4) K and a lower ionization of log U = -0.49, producing absorption by O VI-VII and the Fe VII-XII M-shell Unresolved Transitions Array. Once these components are considered, the data do not require any further absorbers. In particular, a model consisting of a continuous radial range of ionization structures (as suggested by a previous analysis) is not required. The two absorbing components in each velocity system are in pressure equilibrium with each other. This suggests that each velocity system consists of a multi-phase medium. This is the first time that different outflow velocity systems have been modeled independently in the X-ray band for this source. The kinematic components and column densities found from the X-rays are in agreement with the main kinematic components found in the UV absorber. This supports the idea that the UV and X-ray absorbing gas is part of the same phenomenon. NGC 5548 can now be seen to fit in a pattern established for other WAs: two or three discrete phases in pressure equilibrium. There are no remaining cases of a well-studied WA in which a model consisting of a multi-phase medium is not viable. C1 [Andrade-Velazquez, Mercedes; Krongold, Yair; Binette, Luc; Jimenez-Bailon, Elena] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. [Elvis, Martin; Nicastro, Fabrizio; Brickhouse, Nancy] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Nicastro, Fabrizio] OAR INAF, I-00040 Monte Porzio Catone, RM, Italy. [Nicastro, Fabrizio] Fdn Res & Technol, IESL, Iraklion 71110, Crete, Greece. [Mathur, Smita] Ohio State Univ, Columbus, OH 43210 USA. RP Andrade-Velazquez, M (reprint author), Univ Nacl Autonoma Mexico, Inst Astron, Apartado Postal 70-264, Mexico City 04510, DF, Mexico. OI Brickhouse, Nancy/0000-0002-8704-4473; Nicastro, Fabrizio/0000-0002-6896-1364 FU UNAM PAPIIT [IN118905]; CONACyT [J-49594]; NASA [NAS8-03060, NNX08AB81G] FX This work was supported by the UNAM PAPIIT grant IN118905 and the CONACyT grant J-49594. A.-V. M. acknowledges support from a CONACyT scholarship. N.S.B. acknowledges support from NASA to the Chandra X-ray Center through NAS8-03060. This work was supported by the NASA grant NNX08AB81G. NR 78 TC 17 Z9 17 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 MAR 10 PY 2010 VL 711 IS 2 BP 888 EP 906 DI 10.1088/0004-637X/711/2/888 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 559SN UT WOS:000274848100056 ER PT J AU Hatsukade, B Iono, D Akiyama, T Yoshikawa, M Dunlop, JS Ivison, RJ Peck, AB Ikarashi, S Biggs, A Ezawa, H Hanami, H Ho, P Hughes, DH Kawabe, R Kohno, K Matsushita, S Nakanishi, K Padilla, N Petitpas, G Tamura, Y Wagg, J Wilner, DJ Wilson, GW Yamada, T Yun, MS AF Hatsukade, B. Iono, D. Akiyama, T. Yoshikawa, M. Dunlop, J. S. Ivison, R. J. Peck, A. B. Ikarashi, S. Biggs, A. Ezawa, H. Hanami, H. Ho, P. Hughes, D. H. Kawabe, R. Kohno, K. Matsushita, S. Nakanishi, K. Padilla, N. Petitpas, G. Tamura, Y. Wagg, J. Wilner, D. J. Wilson, G. W. Yamada, T. Yun, M. S. TI UNVEILING THE NATURE OF SUBMILLIMETER GALAXY SXDF 850.6 SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; galaxies: evolution; galaxies: formation; galaxies: high-redshift; galaxies: starburst; submillimeter: galaxies ID DEGREE EXTRAGALACTIC SURVEY; STAR-FORMING GALAXIES; AZTEC MILLIMETER SURVEY; HIGH-REDSHIFT GALAXIES; NUMBER COUNTS; PHOTOMETRIC REDSHIFTS; SPACE-TELESCOPE; RADIO GALAXIES; SCUBA GALAXIES; STELLAR MASSES AB We present an 880 mu m Submillimeter Array (SMA) detection of the submillimeter galaxy SXDF 850.6. SXDF 850.6 is a bright source (S(850 mu m) = 8 mJy) detected in the SCUBA Half Degree Extragalactic Survey and has multiple possible radio counterparts in its deep radio image obtained at the VLA. Our new SMA detection finds that the submillimeter emission coincides with the brightest radio emission that is found similar to 8 '' north of the coordinates determined from SCUBA. Despite the lack of detectable counterparts in deep UV/optical images, we find a source at the SMA position in near-infrared and longer wavelength images. We perform spectral energy distribution (SED) model fits to UV-optical-IR photometry (u, B, V, R, i', z', J, H, K, 3.6 mu m, 4.5 mu m, 5.8 mu m, and 8.0 mu m) and to submillimeter-radio photometry (850 mu m, 880 mu m, 1100 mu m, and 21 cm) independently, and we find both are well described by starburst templates at a redshift of z similar or equal to 2.2 +/- 0.3. The best-fit parameters from the UV-optical-IR SED fit are a redshift of z = 1.87(-0.07)(+0.15), a stellar mass of M(star) = 2.5(-0.3)(+2.2) x 10(11)M(circle dot), an extinction of Lambda(V) = 3.0(-1.0)(+0.3) mag, and an age of 720(-210)(+1880) Myr. The submillimeter-radio SED fit provides a consistent redshift of z similar to 1.8-2.5, an IR luminosity of L(IR) = (7-26) x 10(12) L(circle dot), and a star formation rate of 1300-4500 M(circle dot) yr(-1). These results suggest that SXDF 850.6 is a mature system already having a massive amount of old stellar population constructed before its submillimeter bright phase and is experiencing a dusty starburst, possibly induced by major mergers. C1 [Hatsukade, B.; Ikarashi, S.; Kohno, K.] Univ Tokyo, Inst Astron, Tokyo 1810015, Japan. [Iono, D.; Kawabe, R.; Nakanishi, K.; Tamura, Y.] Nobeyama Radio Observ, Minamisa Ku, Nagano 3841805, Japan. [Akiyama, T.; Yoshikawa, M.; Yamada, T.] Tohoku Univ, Astron Inst, Aoba Ku, Sendai, Miyagi 9808578, Japan. [Dunlop, J. S.; Ivison, R. J.] Univ Edinburgh, Royal Observ, Sch Phys & Astron, Scottish Univ Phys Alliance,Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Ivison, R. J.] Royal Observ, Sci & Technol Res Council, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Peck, A. B.] Joint ALMA Observ, Santiago 7550108, Chile. [Biggs, A.] European So Observ, D-85748 Garching, Germany. [Ezawa, H.] Natl Inst Nat Sci, Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Hanami, H.] Iwate Univ, Fac Humanities & Social Sci, Phys Sect, Morioka, Iwate 0208550, Japan. [Ho, P.; Matsushita, S.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Hughes, D. H.; Wagg, J.] INAOE, Puebla 72000, Pue, Mexico. [Kohno, K.] Univ Tokyo, Res Ctr Early Universe, Bunkyo Ku, Tokyo 1130033, Japan. [Padilla, N.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 4860, Chile. [Petitpas, G.] Harvard Smithsonian Ctr Astrophys, Hilo, HI 96720 USA. [Wagg, J.] European So Observ, Santiago 19, Chile. [Wagg, J.; Wilner, D. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Wilson, G. W.; Yun, M. S.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. RP Hatsukade, B (reprint author), Univ Tokyo, Inst Astron, 2-21-1 Osawa, Tokyo 1810015, Japan. EM hatsukade@ioa.s.u-tokyo.ac.jp RI Ivison, R./G-4450-2011 OI Ivison, R./0000-0001-5118-1313 NR 79 TC 21 Z9 21 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 MAR 10 PY 2010 VL 711 IS 2 BP 974 EP 979 DI 10.1088/0004-637X/711/2/974 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 559SN UT WOS:000274848100060 ER PT J AU Peters, T Banerjee, R Klessen, RS Mac Low, MM Galvan-Madrid, R Keto, ER AF Peters, Thomas Banerjee, Robi Klessen, Ralf S. Mac Low, Mordecai-Mark Galvan-Madrid, Roberto Keto, Eric R. TI H II REGIONS: WITNESSES TO MASSIVE STAR FORMATION SO ASTROPHYSICAL JOURNAL LA English DT Article DE hydrodynamics; H II regions; radiative transfer; stars: massive ID ULTRACOMPACT HII-REGIONS; MOLECULAR CLOUD CORES; COLLAPSING DENSE CORE; RADIATIVE-TRANSFER; COMPETITIVE ACCRETION; PROTOSTELLAR DISCS; MAGNETIC PROCESSES; STELLAR CLUSTERS; RADIO-CONTINUUM; TIME-VARIATION AB We describe the first three-dimensional simulation of the gravitational collapse of a massive, rotating molecular cloud that includes heating by both non-ionizing and ionizing radiation. These models were performed with the FLASH code, incorporating a hybrid, long characteristic, ray-tracing technique. We find that as the first protostars gain sufficient mass to ionize the accretion flow, their H II regions are initially gravitationally trapped, but soon begin to rapidly fluctuate between trapped and extended states, in agreement with observations. Over time, the same ultracompact H II region can expand anisotropically, contract again, and take on any of the observed morphological classes. In their extended phases, expanding H II regions drive bipolar neutral outflows characteristic of high-mass star formation. The total lifetime of H II regions is given by the global accretion timescale, rather than their short internal sound-crossing time. This explains the observed number statistics. The pressure of the hot, ionized gas does not terminate accretion. Instead, the final stellar mass is set by fragmentation-induced starvation. Local gravitational instabilities in the accretion flow lead to the build-up of a small cluster of stars, all with relatively high masses due to heating from accretion radiation. These companions subsequently compete with the initial high-mass star for the same common gas reservoir and limit its mass growth. This is in contrast to the classical competitive accretion model, where the massive stars are never hindered in growth by the low-mass stars in the cluster. Our findings show that the most significant differences between the formation of low-mass and high-mass stars are all explained as the result of rapid accretion within a dense, gravitationally unstable, ionized flow. C1 [Peters, Thomas; Banerjee, Robi; Klessen, Ralf S.] Univ Heidelberg, Inst Theoret Astrophys, Zentrum Astron, D-69120 Heidelberg, Germany. [Mac Low, Mordecai-Mark] Amer Museum Nat Hist, Dept Astrophys, New York, NY 10024 USA. [Galvan-Madrid, Roberto; Keto, Eric R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Galvan-Madrid, Roberto] UNAM, Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico. [Galvan-Madrid, Roberto] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. RP Peters, T (reprint author), Univ Heidelberg, Inst Theoret Astrophys, Zentrum Astron, Albert Ueberle Str 2, D-69120 Heidelberg, Germany. EM thomas.peters@ita.uni-heidelberg.de OI Mac Low, Mordecai-Mark/0000-0003-0064-4060 FU Deutsche Forschungsgemeinschaft (DFG) [BA 3607/1, KL1358/1, KL1358/4, KL1358/5]; German Bundesministerium fur Bildung und Forschung [05A09VHA]; Landesstiftung Baden-Wurttemberg; U.S. National Science Foundation [AST08-35734] FX T.P. is a fellow of the International Max Planck Research School for Astronomy and Cosmic Physics at the University of Heidelberg and the Heidelberg Graduate School of Fundamental Physics. He also acknowledges support from an Annette Kade Fellowship for his visit to the American Museum of Natural History. We also thank the Deutsche Forschungsgemeinschaft (DFG) for support via the Emmy Noether Grant BA 3607/1, via the priority program SFB 439 "Galaxies in the Early Universe" as well as via grants KL1358/1, KL1358/4, and KL1358/5. In addition, we also acknowledge partial support from a Frontier grant of Heidelberg University funded by the German Excellence Initiative, from the German Bundesministerium fur Bildung und Forschung via the ASTRONET project STAR FORMAT (grant 05A09VHA) and from the Landesstiftung Baden-Wurttemberg via their program International Collaboration II. M.-M. M. L. thanks the Max-Planck-Institut fur Astronomie and the Institut fur Theoretische Astrophysik der Universitat Heidelberg for hospitality, and the U.S. National Science Foundation for funding under grant AST08-35734. We acknowledge computing time at the Leibniz-Rechenzentrum in Garching (Germany), the NSF-supported Texas Advanced Computing Center (USA), and Julich Supercomputing Centre (Germany). The FLASH code was in part developed by the DOE-supported Alliances Center for Astrophysical Thermonuclear Flashes (ASCI) at the University of Chicago. We thank C. Federrath for important improvements to the sink particle module. We also thank the anonymous referee for the useful comments, which helped to improve the paper. NR 76 TC 121 Z9 122 U1 0 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 MAR 10 PY 2010 VL 711 IS 2 BP 1017 EP 1028 DI 10.1088/0004-637X/711/2/1017 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 559SN UT WOS:000274848100002 ER PT J AU Zhang, YY Okabe, N Finoguenov, A Smith, GP Piffaretti, R Valdarnini, R Babul, A Evrard, AE Mazzotta, P Sanderson, AJR Marrone, DP AF Zhang, Yu-Ying Okabe, Nobuhiro Finoguenov, Alexis Smith, Graham P. Piffaretti, Rocco Valdarnini, Riccardo Babul, Arif Evrard, August E. Mazzotta, Pasquale Sanderson, Alastair J. R. Marrone, Daniel P. TI LoCuSS: A COMPARISON OF CLUSTER MASS MEASUREMENTS FROM XMM-NEWTON AND SUBARU-TESTING DEVIATION FROM HYDROSTATIC EQUILIBRIUM AND NON-THERMAL PRESSURE SUPPORT SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; galaxies: clusters: general; galaxies: clusters: individual (Abell 1914); gravitational lensing: weak; surveys; X-rays: galaxies: clusters ID RELAXED GALAXY CLUSTERS; X-RAY OBSERVATIONS; SCALING RELATIONS; INTRACLUSTER MEDIUM; DARK-MATTER; HYDRODYNAMICAL SIMULATIONS; COSMOLOGICAL SIMULATIONS; STAR-FORMATION; GAS FRACTION; CHANDRA AB We compare X-ray hydrostatic and weak-lensing mass estimates for a sample of 12 clusters that have been observed with both XMM-Newton and Subaru. At an over-density of Delta = 500, we obtain 1 - M(X)/M(WL) = 0.01 +/- 0.07 for the whole sample. We also divided the sample into undisturbed and disturbed sub-samples based on quantitative X-ray morphologies using asymmetry and fluctuation parameters, obtaining 1 - M(X)/M(WL) = 0.09 +/- 0.06 and -0.06 +/- 0.12 for the undisturbed and disturbed clusters, respectively. In addition to non-thermal pressure support, there may be a competing effect associated with adiabatic compression and/or shock heating which leads to overestimate of X-ray hydrostatic masses for disturbed clusters, for example, in the famous merging cluster A1914. Despite the modest statistical significance of the mass discrepancy, on average, in the undisturbed clusters, we detect a clear trend of improving agreement between M(X) and M(WL) as a function of increasing overdensity, M(X)/M(WL) = (0.908 +/- 0.004) + (0.187 +/- 0.010) . log(10)(Delta/500). We also examine the gas mass fractions, f(gas) = M(gas)/M(WL), finding that they are an increasing function of cluster radius, with no dependence on dynamical state, in agreement with predictions from numerical simulations. Overall, our results demonstrate that XMM-Newton and Subaru are a powerful combination for calibrating systematic uncertainties in cluster mass measurements. C1 [Zhang, Yu-Ying] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany. [Okabe, Nobuhiro] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Okabe, Nobuhiro] Tohoku Univ, Astron Inst, Aoba Ku, Sendai, Miyagi 9808578, Japan. [Finoguenov, Alexis] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Finoguenov, Alexis] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA. [Smith, Graham P.; Sanderson, Alastair J. R.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Piffaretti, Rocco] CEA Saclay, CEA, F-91191 Gif Sur Yvette, France. [Valdarnini, Riccardo] SISSA ISAS, I-34014 Trieste, Italy. [Babul, Arif] Univ Victoria, Dept Phys & Astron, Victoria, BC, Canada. [Evrard, August E.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Evrard, August E.] Univ Michigan, Michigan Ctr Theoret Phys, Ann Arbor, MI 48109 USA. [Evrard, August E.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Evrard, August E.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Mazzotta, Pasquale] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. [Mazzotta, Pasquale] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Marrone, Daniel P.] Univ Chicago, Dept Astron & Astrophys, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. RP Zhang, YY (reprint author), Univ Bonn, Argelander Inst Astron, Hugel 71, D-53121 Bonn, Germany. EM yyzhang@astro.uni-bonn.de RI Mazzotta, Pasquale/B-1225-2016; OI Mazzotta, Pasquale/0000-0002-5411-1748; Evrard, August/0000-0002-4876-956X; Babul, Arif/0000-0003-1746-9529 FU DFG [RE 1462/2]; German BMBF through the Verbundforschung [50 OR 0601]; Ministry of Education, Science, Sports and Culture of Japan; Ministry of Education, Culture, Sports, Science, and Technology of Japan [18072001, 20740099]; BMBF/DLR [50 OR 0207]; MPG; NASA [NNX08AX46G, HF-51259.01, NAS5-26555]; Royal Society; STFC FX We acknowledge support from KICP in Chicago for hospitality, and thank our LoCuSS collaborators, especially Masahiro Takada and Keiichi Umetsu, for helpful comments on the manuscript. Y.Y.Z. thanks Massimo Meneghetti and Gabriel Pratt for useful discussion. Y.Y.Z. acknowledges support by the DFG through Emmy Noether Research Grant RE 1462/2, through Schwerpunkt Program 1177, and through project B6 "Gravitational Lensing and X-ray Emission by Non-Linear Structures" of Transregional Collaborative Research Centre TRR 33 The Dark Universe, and support by the German BMBF through the Verbundforschung under grant 50 OR 0601. This work is supported by a Grant-in-Aid for the COE Program "Exploring New Science by Bridging Particle-Matter Hierarchy" and G-COE Program "Weaving Science Web beyond Particle-Matter Hierarchy" in Tohoku University, funded by the Ministry of Education, Science, Sports and Culture of Japan. This work is, in part, supported by a Grant-in-Aid for Science Research in a Priority Area "Probing the Dark Energy through an Extremely Wide and Deep Survey with Subaru Telescope" (18072001) from the Ministry of Education, Culture, Sports, Science, and Technology of Japan. N.O. is, in part, supported by a Grant-in-Aid from the Ministry of Education, Culture, Sports, Science, and Technology of Japan (20740099). A. F. acknowledges support from BMBF/DLR under grant 50 OR 0207 and MPG, and was partially supported by a NASA grant NNX08AX46G to UMBC. G.P.S. acknowledges support from the Royal Society and STFC. D.P.M. acknowledges support provided by NASA through Hubble Fellowship grant HF-51259.01 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. NR 68 TC 99 Z9 99 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 MAR 10 PY 2010 VL 711 IS 2 BP 1033 EP 1043 DI 10.1088/0004-637X/711/2/1033 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 559SN UT WOS:000274848100004 ER PT J AU Machacek, ME O'Sullivan, E Randall, SW Jones, C Forman, WR AF Machacek, M. E. O'Sullivan, E. Randall, S. W. Jones, C. Forman, W. R. TI THE MYSTERIOUS MERGER OF NGC 6868 AND NGC 6861 IN THE TELESCOPIUM GROUP SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: general; galaxies: individual (NGC 6868, NGC 6861); intergalactic medium; X-rays: galaxies ID EARLY-TYPE GALAXIES; BLACK-HOLE MASS; X-RAY LUMINOSITIES; COLD-GAS ACCRETION; ELLIPTIC GALAXY; XMM-NEWTON; VIRGO CLUSTER; VORONOI TESSELLATIONS; INTERGALACTIC MEDIUM; VELOCITY DISPERSION AB We use Chandra X-ray observations of the hot gas in and around NGC 6868 and NGC 6861 in the Telescopium galaxy group (Lambda S0851) to probe the interaction history between these galaxies. Mean surface brightness profiles for NGC 6868 and NGC 6861 are each well described by double beta-models, suggesting that they are each the dominant galaxy in a galaxy subgroup about to merge. Surface brightness and temperature maps of the brightest group galaxy NGC 6868 show a cold front edge similar to 23 kpc to the north, and a cool 0.62 keV spiral-shaped tail to the south. Analysis of the temperature and density across the cold front constrains the relative motion between NGC 6868 and the ambient group gas to be at most transonic; while the spiral morphology of the tail strongly suggests that the cold front edge and tail are the result of gas sloshing due to the subgroup merger. The cooler central region of NGC 6861 is surrounded by a sheath of hot gas to the east and hot, bifurcated tails of X-ray emission to the west and northwest. We discuss supersonic infall of the NGC 6861 subgroup, sloshing from the NGC 6868 and NGC 6861 subgroup merger, and AGN heating as possible explanations for these features, and discuss possible scenarios that may contribute to the order of magnitude discrepancy between the Margorrian and black hole mass-sigma predictions for its central black hole. C1 [Machacek, M. E.; O'Sullivan, E.; Randall, S. W.; Jones, C.; Forman, W. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Machacek, ME (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mmachacek@cfa.harvard.edu OI Randall, Scott/0000-0002-3984-4337; O'Sullivan, Ewan/0000-0002-5671-6900 FU NASA [NNX07AH65G]; Smithsonian Institution FX This work is supported in part by NASA grant NNX07AH65G and the Smithsonian Institution. 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 thank John Huchra for help using the Harvard-Smithsonian CfA Redshift Survey (ZCAT) database for galaxy redshift data, Ryan Johnson and Paul Nulsen for helpful discussions, and an anonymous referee for helpful comments. NR 88 TC 9 Z9 9 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 MAR 10 PY 2010 VL 711 IS 2 BP 1316 EP 1332 DI 10.1088/0004-637X/711/2/1316 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 559SN UT WOS:000274848100028 ER PT J AU Luna, GJM Raymond, JC Brickhouse, NS Mauche, CW Proga, D Steeghs, D Hoogerwerf, R AF Luna, G. J. M. Raymond, J. C. Brickhouse, N. S. Mauche, C. W. Proga, D. Steeghs, D. Hoogerwerf, R. TI PHOTOIONIZED FEATURES IN THE X-RAY SPECTRUM OF EX HYDRAE SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; novae, cataclysmic variables; stars: individual (EX Hydrae); X-rays: binaries ID WHITE-DWARF; CATACLYSMIC VARIABLES; INTERMEDIATE POLARS; SPECTROSCOPY; ACCRETION; EMISSION; HYA; DENSITY; SYSTEM; MODEL AB We present the first results from a long ( 496 ks) Chandra High Energy Transmission Grating observation of the intermediate polar EX Hydrae ( EX Hya). In addition to the narrow emission lines from the cooling post-shock gas, for the first time we have detected a broad component in some of the X-ray emission lines, namely, O VIII lambda 18.97, Mg XII lambda 8.42, Si XIV lambda 6.18, and Fe XVII lambda 16.78. The broad and narrow components have widths of similar to 1600 km s(-1) and similar to 150 km s(-1), respectively. We propose a scenario where the broad component is formed in the pre-shock accretion flow, photoionized by radiation from the post-shock flow. Because the photoionized region has to be close to the radiation source in order to produce strong photoionized emission lines from ions such as O VIII, Fe XVII, Mg XII, and Si XIV, our photoionization model constrains the height of the standing shock above the white dwarf surface. Thus, the X-ray spectrum from EX Hya manifests features of both magnetic and non-magnetic cataclysmic variables. C1 [Luna, G. J. M.; Raymond, J. C.; Brickhouse, N. S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Mauche, C. W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Proga, D.] Univ Nevada, Dept Phys & Astron, Las Vegas, NV 89154 USA. [Steeghs, D.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Hoogerwerf, R.] Interact Supercomp Inc, Waltham, MA 02452 USA. RP Luna, GJM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM gluna@cfa.harvard.edu; jraymond@cfa.harvard.edu; nbrickhouse@cfa.harvard.edu; mauche@cygnus.llnl.gov; dproga@physics.unlv.edu; dsteeghs@cfa.harvard.edu; hoogerw@pobox.com RI Steeghs, Danny/C-5468-2009; OI Steeghs, Danny/0000-0003-0771-4746; Brickhouse, Nancy/0000-0002-8704-4473 FU NASA [GO7- 8026X, NAS8-03060]; U.S. Department of Energy by Lawrence Livermore National Laboratory [DE-AC52-07NA27344] FX We thank the anonymous referee for useful comments which help to improve the final manuscript. We acknowledge support from NASA to the Smithsonian Astrophysical Observatory (SAO) under Chandra GO7- 8026X for G.J.M.L. C.W.M.'s contribution to this work was performed under the auspices of the U.S. Department of Energy by Lawrence Livermore National Laboratory under Contract DE-AC52-07NA27344. N.S.B. is supported by NASA Contract NAS8-03060 to SAO for the Chandra X-ray Center. NR 28 TC 5 Z9 5 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 MAR 10 PY 2010 VL 711 IS 2 BP 1333 EP 1337 DI 10.1088/0004-637X/711/2/1333 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 559SN UT WOS:000274848100029 ER PT J AU Elias-Rosa, N Van Dyk, SD Li, WD Morrell, N Gonzalez, S Hamuy, M Filippenko, AV Cuillandre, JC Foley, RJ Smith, N AF Elias-Rosa, Nancy Van Dyk, Schuyler D. Li, Weidong Morrell, Nidia Gonzalez, Sergio Hamuy, Mario Filippenko, Alexei V. Cuillandre, Jean-Charles Foley, Ryan J. Smith, Nathan TI ON THE PROGENITOR OF THE TYPE II-PLATEAU SN 2008cn IN NGC 4603 (vol 706, pg 1174, 2009) SO ASTROPHYSICAL JOURNAL LA English DT Correction C1 [Elias-Rosa, Nancy; Van Dyk, Schuyler D.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Li, Weidong; Filippenko, Alexei V.; Foley, Ryan J.; Smith, Nathan] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Morrell, Nidia; Gonzalez, Sergio] Carnegie Observ, Las Campanas Observ, La Serena, Chile. [Hamuy, Mario] Univ Chile, Dept Astron, Santiago, Chile. [Cuillandre, Jean-Charles] Canada France Hawaii Telescope Corp, Kamuela, HI 96743 USA. [Foley, Ryan J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Elias-Rosa, N (reprint author), CALTECH, Spitzer Sci Ctr, 1200 E Calif Blvd, Pasadena, CA 91125 USA. EM nelias@ipac.caltech.edu; vandyk@ipac.caltech.edu RI Elias-Rosa, Nancy/D-3759-2014; Hamuy, Mario/G-7541-2016 OI Elias-Rosa, Nancy/0000-0002-1381-9125; NR 1 TC 2 Z9 2 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 MAR 10 PY 2010 VL 711 IS 2 BP 1343 EP 1343 DI 10.1088/0004-637X/711/2/1343 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 559SN UT WOS:000274848100031 ER PT J AU Boyer, ML van Loon, JT McDonald, I Gordon, KD Babler, B Block, M Bracker, S Engelbracht, C Hora, J Indebetouw, R Meade, M Meixner, M Misselt, K Sewilo, M Shiao, B Whitney, B AF Boyer, Martha L. van Loon, Jacco Th. McDonald, Iain Gordon, Karl D. Babler, Brian Block, Miwa Bracker, Steve Engelbracht, Charles Hora, Joe Indebetouw, Remy Meade, Marilyn Meixner, Margaret Misselt, Karl Sewilo, Marta Shiao, Bernie Whitney, Barbara TI IS DUST FORMING ON THE RED GIANT BRANCH IN 47 Tuc? SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE circumstellar matter; globular clusters: individual (47 Tuc); infrared: stars; stars: AGB and post-AGB; stars: mass-loss; stars: winds, outflows ID SPITZER-SPACE-TELESCOPE; GALACTIC GLOBULAR-CLUSTERS; POPULATION-II GIANTS; MASS-LOSS RATES; AGB-STARS; INTRACLUSTER MEDIUM; MAGELLANIC-CLOUD; OMEGA-CENTAURI; WHITE-DWARFS; EVOLUTION AB Using Spitzer Infrared Array Camera (IRAC) observations from the SAGE-SMC Legacy program and archived Spitzer IRAC data, we investigate dust production in 47 Tuc, a nearby massive Galactic globular cluster. A previous study detected infrared excess, indicative of circumstellar dust, in a large population of stars in 47 Tuc, spanning the entire red giant branch (RGB). We show that those results suffered from effects caused by stellar blending and imaging artifacts and that it is likely that no stars below approximate to 1 mag from the tip of the RGB are producing dust. The only stars that appear to harbor dust are variable stars, which are also the coolest and most luminous stars in the cluster. C1 [Boyer, Martha L.; Gordon, Karl D.; Meixner, Margaret; Sewilo, Marta; Shiao, Bernie] STScI, Baltimore, MD 21218 USA. [van Loon, Jacco Th.] Keele Univ, Astrophys Grp, Lennard Jones Labs, Keele ST5 5BG, Staffs, England. [McDonald, Iain] Univ Manchester, Jodrell Bank, Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Babler, Brian; Bracker, Steve; Meade, Marilyn] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Block, Miwa; Engelbracht, Charles; Misselt, Karl] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Hora, Joe] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Indebetouw, Remy] Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. [Whitney, Barbara] Space Sci Inst, Boulder, CO 80301 USA. RP Boyer, ML (reprint author), STScI, 3700 San Martin Dr, Baltimore, MD 21218 USA. EM mboyer@stsci.edu OI Babler, Brian/0000-0002-6984-5752; Hora, Joseph/0000-0002-5599-4650 FU Spitzer [1309827, 1340964]; NASA; NSF FX We thank the anonymous referee for his/her thorough review. This work was supported by Spitzer via JPL contracts 1309827 and 1340964 and makes use of data products from 2MASS, a joint project of the University of Massachusetts and IPAC/Caltech, funded by NASA and the NSF. NR 49 TC 28 Z9 28 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD MAR 10 PY 2010 VL 711 IS 2 BP L99 EP L103 DI 10.1088/2041-8205/711/2/L99 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 567BT UT WOS:000275418000011 ER PT J AU MacPherson, GJ Bullock, ES Janney, PE Kita, NT Ushikubo, T Davis, AM Wadhwa, M Krot, AN AF MacPherson, G. J. Bullock, E. S. Janney, P. E. Kita, N. T. Ushikubo, T. Davis, A. M. Wadhwa, M. Krot, A. N. TI EARLY SOLAR NEBULA CONDENSATES WITH CANONICAL, NOT SUPRACANONICAL, INITIAL Al-26/Al-27 RATIOS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE astrochemistry; nuclear reactions, nucleosynthesis, abundances; protoplanetary disks ID REFRACTORY INCLUSIONS; RICH INCLUSIONS; ISOTOPE FRACTIONATION; AL-26; CHONDRULES; ALLENDE; SYSTEM; AL-26-MG-26; EVAPORATION; CHONDRITES AB The short-lived radionuclide Al-26 existed throughout the solar nebula 4.57 Ga ago, and the initial abundance ratio (Al-26/Al-27)(0), as inferred from magnesium isotopic compositions of calcium-aluminum-rich inclusions (CAIs) in chondritic meteorites, has become a benchmark for understanding early solar system chronology. Internal mineral isochrons in most CAIs measured by secondary ion mass spectrometry (SIMS) give (Al-26/Al-27)(0) similar to (4-5) x 10(-5), called "canonical." Some recent high-precision analyses of (1) bulk CAIs measured by multicollector inductively coupled plasma mass spectrometry (MC-ICPMS), (2) individual CAI minerals and their mixtures measured by laser ablation MC-ICPMS, and (3) internal isochrons measured by multicollector (MC)-SIMS indicated a somewhat higher "supracanonical" (Al-26/Al-27)(0) ranging from (5.85 +/- 0.05) x 10(-5) to > 7 x 10(-5). These measurements were done on coarse-grained Type B and Type A CAIs that probably formed by recrystallization and/or melting of fine-grained condensate precursors. Thus the supracanonical ratios might record an earlier event, the actual nebular condensation of the CAI precursors. We tested this idea by performing in situ high-precision magnesium isotope measurements of individual minerals in a fine-grained CAI whose structures and volatility-fractionated trace element abundances mark it as a primary solar nebula condensate. Such CAIs are ideal candidates for the fine-grained precursors to the coarse-grained CAIs, and thus should best preserve a supracanonical ratio. Yet, our measured internal isochron yields (Al-26/Al-27)(0) = (5.27 +/- 0.17) x 10(-5). Thus our data do not support the existence of supracanonical (Al-26/Al-27)(0) = (5.85-7) x 10 (5). There may not have been a significant time interval between condensation of the CAI precursors and their subsequent melting into coarse-grained CAIs. C1 [MacPherson, G. J.; Bullock, E. S.] Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. [Janney, P. E.; Wadhwa, M.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Janney, P. E.; Wadhwa, M.] Arizona State Univ, Ctr Meteorite Studies, Tempe, AZ 85287 USA. [Kita, N. T.; Ushikubo, T.] Univ Wisconsin, Dept Geosci, WiscSIMS, Madison, WI 53706 USA. [Davis, A. M.] Univ Chicago, Dept Geophys Sci, Chicago, IL 60637 USA. [Davis, A. M.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Krot, A. N.] Univ Hawaii Manoa, Hawaii Inst Geophys Planetol, Honolulu, HI 96822 USA. RP MacPherson, GJ (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. EM macphers@si.edu RI Janney, Philip/K-2733-2013; Kita, Noriko/H-8035-2016; OI Janney, Philip/0000-0001-5740-4266; Kita, Noriko/0000-0002-0204-0765; Davis, Andrew/0000-0001-7955-6236 NR 31 TC 32 Z9 32 U1 1 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD MAR 10 PY 2010 VL 711 IS 2 BP L117 EP L121 DI 10.1088/2041-8205/711/2/L117 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 567BT UT WOS:000275418000015 ER PT J AU Roelofs, GHA Rau, A Marsh, TR Steeghs, D Groot, PJ Nelemans, G AF Roelofs, Gijs H. A. Rau, Arne Marsh, Tom R. Steeghs, Danny Groot, Paul J. Nelemans, Gijs TI SPECTROSCOPIC EVIDENCE FOR A 5.4 MINUTE ORBITAL PERIOD IN HM CANCRI SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE binaries: close; gravitational waves; stars: individual (HM Cancri, V407 Vulpeculae); X-rays: binaries ID CANUM-VENATICORUM BINARIES; DOUBLE-DEGENERATE POLAR; RX J0806.3+1527; SPIN-UP; GRAVITATIONAL-RADIATION; ULTRACOMPACT BINARY; V407 VULPECULAE; GW EMISSION; CHANDRA; MODEL AB HM Cancri is a candidate ultracompact binary white dwarf with an apparent orbital period of only 5.4 minutes, as suggested by X-ray and optical light-curve modulations on that period, and by the absence of longer-period variability. In this Letter, we present Keck-I spectroscopy which shows clear modulation of the helium emission lines in both radial velocity and amplitude on the 5.4 minute period and no other. The data strongly suggest that the binary is emitting He I 4471 from the irradiated face of the cooler, less massive star, and He II 4686 from a ring around the more massive star. From their relative radial velocities, we measure a mass ratio q = 0.50 +/- 0.13. We conclude that the observed 5.4 minute period almost certainly represents the orbital period of an interacting binary white dwarf. We thus confirm that HM Cnc is the shortest period binary star known: a unique test for stellar evolution theory, and one of the strongest known sources of gravitational waves for LISA. C1 [Roelofs, Gijs H. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rau, Arne] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Rau, Arne] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Marsh, Tom R.; Steeghs, Danny] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Groot, Paul J.; Nelemans, Gijs] Radboud Univ Nijmegen, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands. RP Roelofs, GHA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM groelofs@cfa.harvard.edu; arau@mpe.mpg.de RI Nelemans, Gijs/D-3177-2012; Steeghs, Danny/C-5468-2009; Groot, Paul/K-4391-2016 OI Nelemans, Gijs/0000-0002-0752-2974; Steeghs, Danny/0000-0003-0771-4746; Groot, Paul/0000-0002-4488-726X NR 35 TC 35 Z9 35 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 MAR 10 PY 2010 VL 711 IS 2 BP L138 EP L142 DI 10.1088/2041-8205/711/2/L138 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 567BT UT WOS:000275418000019 ER PT J AU Sutton-Grier, AE Kenney, MA Richardson, CJ AF Sutton-Grier, Ariana E. Kenney, Melissa A. Richardson, Curtis J. TI Examining the relationship between ecosystem structure and function using structural equation modelling: A case study examining denitrification potential in restored wetland soils SO ECOLOGICAL MODELLING LA English DT Article DE Ecosystem structure; Ecosystem function; Wetland restoration; Denitrification potential (DNP); Structural equation modelling (SEM) ID RIPARIAN WETLAND; SELF-DESIGN; RESTORATION; PATTERNS AB An ongoing debate in ecology is the relationship between community or ecosystem structure and function. This relationship is particularly important in restored ecosystems because it is often assumed that restoring ecosystem structure will restore ecosystem functioning, but this assumption is frequently not tested. In this study, we used a novel application of structural equation modelling (SEM) to examine the relationship between ecosystem structure and function. To exemplify how to apply SEM to explore this relationship, we used a case study examining soil controls on denitrification potential (DNP) in two restored wetlands. Our objectives were to examine (1) whether both restored wetland soil ecosystems had similar relationships among soils variables (i.e. similar soil ecosystem structure) and (2) whether the soil variables driving denitrification potential (DNP) were similar at both sites (i.e. the soil ecosystems were functioning in a similar manner). Using the unique ability of SEM to test model structure, we proposed a SEM to represent the soil ecosystem and tested this structure with field data. We determined that the same model structure was supported by data from both systems suggesting that the two restored wetland systems had similar soil ecosystem structure. To test whether both ecosystems were functioning in a similar way, we examined the parameters of each model. We determined that the drivers of DNP function were not the same at both sites. Higher soil organic matter was the most important predictor of higher DNP at both sites. However, the other significant relationships among soils variables were different at each system indicating that the soils were not functioning in exactly the same way at each site. Overall, these results suggest that the restoration of ecosystem structure may not necessarily ensure the restoration of ecosystem functioning. In this study we capitalize on an inherent feature of SEM, the ability to test model structure, to test a fundamental ecological question. This novel approach is widely applicable to other systems and improves our understanding of the general relationship between ecosystem structure and function. (C) 2009 Elsevier B.V. All rights reserved. C1 [Sutton-Grier, Ariana E.] Duke Univ, Nicholas Sch Environm & Earth Sci, Durham, NC 27708 USA. [Kenney, Melissa A.] Johns Hopkins Univ, Natl Ctr Earth Surface Dynam, Dept Geog & Environm Engn, Baltimore, MD 21218 USA. [Richardson, Curtis J.] Duke Univ, Nicholas Sch Environm, Durham, NC 27708 USA. RP Sutton-Grier, AE (reprint author), Smithsonian Environm Res Ctr, Box 28,647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM ariana.suttongrier@gmail.com OI Sutton-Grier, Ariana/0000-0002-1242-7728 FU City of Charlotte and Mecklenburg County; Duke Wetland Case Studies Endowment; Society of Wetland Scientist Student Research Grant; NSF [DEB-05-08763]; Smithsonian Environmental Research Center; National Science Foundation via the National Center for Earth-surface Dynamics [EAR-0120914] FX We are grateful to Dr. Jim Grace for helpful suggestions about the SEM analysis and Jen Morse for suggestions about the construct model. We thank Nicolette Cagle and Dean Urban for useful comments on an earlier version of the manuscript as well as several anonymous reviewers. We are also grateful to the following for help in the field and lab: Joseph Lozier, Tracy Hamm, Amanda Ward, Sarah Eminhizer, Erin Brosnan, Josie Bamford, Serwaah Agyapong, Aileen Malloy, Tisha Johnson, Jim Pahl, Wes Willis, Mengchi Ho, Paul Heine, Julie DeMeester, Mike Osland, Amani McHugh, Wyatt Hartman, Brian Roberts, Sharon Madden, and Stephanie Chin. This project was funded by grants from the City of Charlotte and Mecklenburg County, the Duke Wetland Case Studies Endowment, a Society of Wetland Scientist Student Research Grant, a Doctoral Dissertation Improvement Grant from NSF DEB-05-08763, as well as an NSF Graduate Research Fellowship to A.E. Sutton-Grier. A.E. Sutton-Grier was also partially supported by a Smithsonian Fellowship at the Smithsonian Environmental Research Center. M.A. Kenney was partially supported by the STC program of the National Science Foundation via the National Center for Earth-surface Dynamics under the agreement Number EAR-0120914. NR 38 TC 16 Z9 17 U1 6 U2 42 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0304-3800 J9 ECOL MODEL JI Ecol. Model. PD MAR 10 PY 2010 VL 221 IS 5 BP 761 EP 768 DI 10.1016/j.ecolmodel.2009.11.015 PG 8 WC Ecology SC Environmental Sciences & Ecology GA 561UL UT WOS:000275004700003 ER PT J AU Leidner, AK Haddad, NM Lovejoy, TE AF Leidner, Allison K. Haddad, Nick M. Lovejoy, Thomas E. TI Does Tropical Forest Fragmentation Increase Long-Term Variability of Butterfly Communities? SO PLOS ONE LA English DT Article ID PLANT-SPECIES RICHNESS; HABITAT FRAGMENTATION; LANDSCAPE; BIRDS; DEFORESTATION; BIODIVERSITY; EXTINCTIONS; DIVERSITY; ABUNDANCE; RESPONSES AB Habitat fragmentation is a major driver of biodiversity loss. Yet, the overall effects of fragmentation on biodiversity may be obscured by differences in responses among species. These opposing responses to fragmentation may be manifest in higher variability in species richness and abundance (termed hyperdynamism), and in predictable changes in community composition. We tested whether forest fragmentation causes long-term hyperdynamism in butterfly communities, a taxon that naturally displays large variations in species richness and community composition. Using a dataset from an experimentally fragmented landscape in the central Amazon that spanned 11 years, we evaluated the effect of fragmentation on changes in species richness and community composition through time. Overall, adjusted species richness (adjusted for survey duration) did not differ between fragmented forest and intact forest. However, spatial and temporal variation of adjusted species richness was significantly higher in fragmented forests relative to intact forest. This variation was associated with changes in butterfly community composition, specifically lower proportions of understory shade species and higher proportions of edge species in fragmented forest. Analysis of rarefied species richness, estimated using indices of butterfly abundance, showed no differences between fragmented and intact forest plots in spatial or temporal variation. These results do not contradict the results from adjusted species richness, but rather suggest that higher variability in butterfly adjusted species richness may be explained by changes in butterfly abundance. Combined, these results indicate that butterfly communities in fragmented tropical forests are more variable than in intact forest, and that the natural variability of butterflies was not a buffer against the effects of fragmentation on community dynamics. C1 [Leidner, Allison K.; Haddad, Nick M.] N Carolina State Univ, Dept Biol, Raleigh, NC 27695 USA. [Lovejoy, Thomas E.] H John Heinz III Ctr Sci Econ & Environm, Washington, DC USA. [Lovejoy, Thomas E.] Inst Nacl de Pesquisas da Amazonia, Biol Dynam Forest Fragments Project, Manaus, Amazonas, Brazil. [Lovejoy, Thomas E.] Smithsonian Trop Res Inst, Manaus, Amazonas, Brazil. [Lovejoy, Thomas E.] George Mason Univ, Dept Environm Sci & Policy, Fairfax, VA 22030 USA. RP Leidner, AK (reprint author), Univ Maryland, Dept Plant Sci & Landscape Architecture, College Pk, MD 20742 USA. EM Leidner@umd.edu FU Andrew W. Mellon Foundation; CitiCorp; Smithsonian Institution; Man and the Biosphere Program (MAB); World Wildlife Fund FX The Andrew W. Mellon Foundation, CitiCorp, the Smithsonian Institution, the Man and the Biosphere Program (MAB), and World Wildlife Fund helped fund the Biological Dynamics of Forest Fragments Project. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 36 TC 17 Z9 18 U1 5 U2 25 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 MAR 10 PY 2010 VL 5 IS 3 AR e9534 DI 10.1371/journal.pone.0009534 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 565XE UT WOS:000275328800006 PM 20224772 ER PT J AU Lamsal, LN Martin, RV van Donkelaar, A Celarier, EA Bucsela, EJ Boersma, KF Dirksen, R Luo, C Wang, Y AF Lamsal, L. N. Martin, R. V. van Donkelaar, A. Celarier, E. A. Bucsela, E. J. Boersma, K. F. Dirksen, R. Luo, C. Wang, Y. TI Indirect validation of tropospheric nitrogen dioxide retrieved from the OMI satellite instrument: Insight into the seasonal variation of nitrogen oxides at northern midlatitudes SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID OZONE MONITORING INSTRUMENT; POWER-PLANT PLUMES; NOX EMISSIONS; GOME MEASUREMENTS; INTEX-B; SURFACE REFLECTIVITY; UNITED-STATES; LIGHTNING NOX; URBAN PLUME; MODEL AB We examine the seasonal variation in lower tropospheric nitrogen oxides (NOx = NO + NO2) at northern midlatitudes by evaluating tropospheric NO2 columns observed from the Ozone Monitoring Instrument (OMI) satellite instrument with surface NO2 measurements (SouthEastern Aerosol Research and Characterization and Air Quality System) and current bottom-up NOx emission inventories, using a global model of tropospheric chemistry (GEOS-Chem). The standard (SP) and DOMINO (DP) tropospheric NO2 column products from OMI exhibit broadly similar spatial and seasonal variation, but differ substantially over continental source regions. A comparison of the two OMI tropospheric NO2 products with in situ surface NO2 concentrations and bottom-up NOx emissions over the southeast United States indicates that annual mean NO2 columns from the DP are biased high by 21%-33% and those from the SP are biased high by 27%-43%. The bias in SP columns is highly seasonal, 67%-74% in summer compared with -6% to -1% in winter. Similar seasonal differences exist between top-down and bottom-up NOx emission inventories over North America, Europe, and East Asia. The air mass factor largely explains the observed seasonal difference between the DP and SP, and in turn the seasonal SP bias. We develop a third product (DP_GC) using averaging kernel information from the DP and NO2 vertical profiles from GEOS-Chem. This product reduces to 5%-21% the annual mean bias over the southeast United States. We use the seasonal variation in the DP_GC to estimate the seasonal variation in the lifetime of lower tropospheric NOx against oxidation to HNO3 over the eastern United States. The effective NOx lifetime at OMI overpass time (early afternoon) ranges from 7.6 h in summer to 17.8 h in winter, consistent within 3 h of the simulated lifetime. GEOS-Chem calculations reveal that the seasonal variation in OMI NO2 columns largely reflects gas-phase oxidation of NO2 in summer with an increasing role for heterogenous chemistry in winter. C1 [Lamsal, L. N.; 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. [Celarier, E. A.] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. [Bucsela, E. J.] SRI Int, Menlo Pk, CA 94025 USA. [Boersma, K. F.; Dirksen, R.] Royal Netherlands Meteorol Inst, Climate Observat Dept, NL-3732 GK De Bilt, Netherlands. [Luo, C.; Wang, Y.] Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA. RP Lamsal, LN (reprint author), Dalhousie Univ, Dept Phys & Atmospher Sci, James Dunn Bldg, Halifax, NS B3H 3J5, Canada. EM lok.lamsal@fizz.phys.dal.ca RI Lamsal, Lok/G-4781-2012; Boersma, Klaas/H-4559-2012; Pfister, Gabriele/A-9349-2008; Wang, Yuhang/B-5578-2014; Martin, Randall/C-1205-2014; Chem, GEOS/C-5595-2014 OI Boersma, Klaas/0000-0002-4591-7635; Martin, Randall/0000-0003-2632-8402; FU NASA's Atmospheric Composition; Canadian Foundation for Climate and Atmospheric Science FX We are grateful to Eric S. Edgerton, Ben Hartsell, and Callie Waid for providing the SEARCH data. We thank the OMI, AQS, and TEMIS teams for making the data available. This work was supported by NASA's Atmospheric Composition Program and Canadian Foundation for Climate and Atmospheric Science. NR 109 TC 92 Z9 92 U1 2 U2 51 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD MAR 6 PY 2010 VL 115 AR D05302 DI 10.1029/2009JD013351 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 565PA UT WOS:000275305100003 ER PT J AU Helgen, KM Leary, T Aplin, KP AF Helgen, Kristofer M. Leary, Tanya Aplin, Kenneth P. TI A Review of Microhydromys (Rodentia: Murinae), with Description of a New Species from Southern New Guinea SO AMERICAN MUSEUM NOVITATES LA English DT Article ID PAPUA-NEW-GUINEA; MORPHOMETRIC-ANALYSIS; MURIDAE; GENUS; BIOGEOGRAPHY; SYSTEMATICS; PHYLOGENY; DIVERSITY; EVOLUTION; ECOLOGY AB The murine rodent genus Microhydromys Tate and Archbold, 1941, includes the smallest of the native rodents of New Guinea and is the rarest Australo-Papuan rodent genus preserved in world museums. We discuss the morphological characteristics of Microhydromys and diagnose two species in the genus: M. richardsoni Tate and Archbold, 1941, distributed over northern New Guinea. and M. argenteus, n. sp., recorded from three localities in southern New Guinea. The only other species previously classified in the genus-Microhydromys musseri Flannery, 1989-is reallocated to the genus Pseudohydromys Rummler, 1934. The little available information relating to their biology indicates the species of Microhydromys to be terrestrial inhabitants of foothill and lower montane forest formations and probably naturally rare in those environments. C1 [Helgen, Kristofer M.; Aplin, Kenneth P.] Amer Museum Nat Hist, Div Vertebrate Zool Mammol, New York, NY 10024 USA. [Helgen, Kristofer M.] Smithsonian Inst, Natl Museum Nat Hist, Div Mammals, Washington, DC 20013 USA. [Leary, Tanya] Dept Environm Climate Change & Water, Pk & Wildlife Div, Parramatta, NSW 2124, Australia. [Leary, Tanya] Kikori Integrated Conservat & Dev Project, World Wide Fund Nat, Moro, So Highlands, Papua N Guinea. [Aplin, Kenneth P.] CSIRO, Div Sustainable Ecosyst, Australian Natl Wildlife Collect, Canberra, ACT 2601, Australia. RP Helgen, KM (reprint author), Amer Museum Nat Hist, Div Vertebrate Zool Mammol, New York, NY 10024 USA. EM helgenk@si.edu FU Smithsonian Institution; U.S. National Science Foundation; Australian American Fulbright Association; Bernice P. Bishop Museum; American Society of Mammalogists; Australian Research Council FX For their generosity in providing access to collections and loaning material, we thank Sandy Ingleby and Tish Ennis (AM), Darrin Lunde, Eileen Westwig, and Nancy Simmons (AMNH), Carla Kishinami and Kathleen Pumehana Imada (BBM), Robert Palmer (ANWC). and Rose Singadan (UPNG). Steve Hamilton assisted with specimen examinations at UPNG. Helgen's research was supported by grants and fellowships from the Smithsonian Institution, U.S. National Science Foundation, Australian American Fulbright Association. Bernice P. Bishop Museum, and American Society of Mammalogists. Helgen also gratefully acknowledges the hospitality of Conan and Elisheva Yuan during visits to New York and Allen Allison and Isabella Forster during visits to Honolulu.; Aplin's fieldwork in the Oenake Range was supported by an Australian Research Council Discovery Grant to Sue O'Connor of the Australian National University. The Darai Plateau specimen collected by Leary was collected during mammal surveys carried out on behalf of the WWF Kikorl Integrated Conservation and Development Project that is largely funded by Kutubu Joint Venture Petroleum Development Project, Gobe Main Joint Venture Partners. and SE Gobe Joint Venture Partners. Leary would like to thank the customary landowners of this part of the Darai Plateau for permission to work on their land and for sharing their stories with her. She would like to thank all those who assisted in the field, particularly Michael Pennay (who volunteered his time on the survey); Ted Mamu and Rex Namo (WWF); and Amos Binoi, Mou Tonny, and Binsy Muture (customary landowners). Logistic and other support for the Darai Plateau survey provided by WWF staff Max Kuduk, Amos Ona, Sam Moko, and Nellie Bou is sincerely appreciated. For sharing their botanical knowledge both during and after the survey Olo Gebia (WWF) and Lawong Balun (Unitech) are gratefully acknowledged. Lastly, Leary would like to thank Michael Pennay and Allen Allison for permission to use their photographs and who, in addition to Steve Richards, provided entertaining company on the Darai Plateau, and Rob Sheaffe for approving leave time for fieldwork. NR 86 TC 3 Z9 3 U1 1 U2 8 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 MAR 4 PY 2010 IS 3676 BP 1 EP 22 DI 10.1206/632.1 PG 22 WC Biodiversity Conservation; Zoology SC Biodiversity & Conservation; Zoology GA 565LD UT WOS:000275293100001 ER PT J AU Frebel, A Kirby, EN Simon, JD AF Frebel, Anna Kirby, Evan N. Simon, Joshua D. TI Linking dwarf galaxies to halo building blocks with the most metal-poor star in Sculptor SO NATURE LA English DT Article ID SPHEROIDAL GALAXY; MILKY-WAY; CHEMICAL-COMPOSITION; GALACTIC HALO; DARK-MATTER; ABUNDANCES; SPECTROSCOPY; SATELLITES; SIGNATURES; GIANT AB Current cosmological models(1,2) indicate that the Milky Way's stellar halo was assembled from many smaller systems. On the basis of the apparent absence of the most metal-poor stars in present-day dwarf galaxies, recent studies(3) claimed that the true Galactic building blocks must have been vastly different from the surviving dwarfs. The discovery of an extremely iron-poor star (S1020549) in the Sculptor dwarf galaxy based on a medium-resolution spectrum(4) cast some doubt on this conclusion. Verification of the iron-deficiency, however, and measurements of additional elements, such as the a-element Mg, are necessary to demonstrate that the same type of stars produced the metals found in dwarf galaxies and the Galactic halo. Only then can dwarf galaxy stars be conclusively linked to early stellar halo assembly. Here we report high-resolution spectroscopic abundances for 11 elements in S1020549, confirming its iron abundance of less than 1/4,000th that of the Sun, and showing that the overall abundance pattern follows that seen in low-metallicity halo stars, including the a-elements. Such chemical similarity indicates that the systems destroyed to form the halo billions of years ago were not fundamentally different from the progenitors of present-day dwarfs, and suggests that the early chemical enrichment of all galaxies may be nearly identical. C1 [Frebel, Anna] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kirby, Evan N.] CALTECH, Pasadena, CA 91125 USA. [Simon, Joshua D.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. RP Frebel, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM afrebel@cfa.harvard.edu OI Kirby, Evan/0000-0001-6196-5162 FU NASA; Space Telescope Science Institute; Carnegie Institution of Washington FX Our data was gathered using the 6.5-m Magellan telescopes located at Las Campanas Observatory, Chile. We thank L. Hernquist for discussions on galaxy formation. A. F. acknowledges support through a Clay Fellowship administered by the Smithsonian Astrophysical Observatory. Support for this work was provided by NASA through a 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 (to E.N.K., who is a Hubble Fellow). J.D.S. acknowledges the support of a Vera Rubin Fellowship provided by the Carnegie Institution of Washington. NR 30 TC 98 Z9 98 U1 0 U2 1 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD MAR 4 PY 2010 VL 464 IS 7285 BP 72 EP 75 DI 10.1038/nature08772 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 563GZ UT WOS:000275117500035 PM 20203604 ER PT J AU Muller-Landau, HC AF Muller-Landau, Helene C. TI The tolerance-fecundity trade-off and the maintenance of diversity in seed size SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE species coexistence; habitat partitioning; competition-colonization tradeoff; stress tolerance; seed mass ID RECRUITMENT LIMITATION; HABITAT DESTRUCTION; PERENNIAL PLANTS; SPECIES RICHNESS; COMPETITION; COEXISTENCE; COLONIZATION; DISPERSAL; COMMUNITIES; POPULATIONS AB Seed size commonly varies by five to six orders of magnitude among coexisting plant species, a pattern ecologists have long sought to explain. Because seed size trades off with seed number, small-seeded species clearly have the advantage in fecundity, but what is the countervailing advantage of large seeds? Higher competitive ability combined with strong competitive asymmetry can in theory allow coexistence through a competition-colonization trade-off, but empirical evidence is inconsistent with this mechanism. Instead, the key advantage of large seeds appears to be their tolerance of stresses such as shade or drought that are present in some but not all regeneration sites. Here I present a simple, analytically tractable model of species coexistence in heterogeneous habitats through a tolerance-fecundity trade-off. Under this mechanism, the more tolerant species win all of the more stressful regeneration sites and some of those that are less stressful, whereas the more fecund species win most but not all of the less stressful sites. The tolerance-fecundity trade-off enables stable coexistence of large numbers of species in models with and without seed limitation. The tolerance-fecundity mechanism provides an excellent explanation for the maintenance of diversity of seed size within plant communities and also suggests new hypotheses for coexistence in animal and microbial communities. C1 [Muller-Landau, Helene C.] Smithsonian Trop Res Inst, APO, AA 34002 USA. [Muller-Landau, Helene C.] Univ Minnesota, Dept Ecol Evolut & Behav, St Paul, MN 55108 USA. RP Muller-Landau, HC (reprint author), Smithsonian Trop Res Inst, APO, AA 34002 USA. EM mullerh@si.edu FU HSBC Climate Partnership; Packard Fellowship in Science and Engineering; University of Minnesota; National Science Foundation [DEB 614055, 0453445] FX I thank Egbert Leigh and three anonymous reviewers for valuable comments on this work and Claudia Neuhauser and David Tilman for stimulating discussions of these ideas. I very gratefully acknowledge the wonderful support of my husband Joe Wright, whose constant encouragement, constructive comments on drafts, and, not least, assumption of a large share of our joint parenting responsibilities were a tremendous aid in helping me to see this manuscript through to completion. The HSBC Climate Partnership, a Packard Fellowship in Science and Engineering, the University of Minnesota, and the National Science Foundation (DEB 614055 and 0453445) provided financial support. NR 49 TC 100 Z9 103 U1 7 U2 98 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD MAR 2 PY 2010 VL 107 IS 9 BP 4242 EP 4247 DI 10.1073/pnas.0911637107 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 563KP UT WOS:000275131100054 PM 20160078 ER PT J AU Kreamer, CM AF Kreamer, Christine Mullen TI Impermanent by Design The Ephemeral in Africa's Tradition-based Arts SO AFRICAN ARTS LA English DT Article C1 Smithsonian Inst, Natl Museum African Art, Washington, DC 20560 USA. RP Kreamer, CM (reprint author), Smithsonian Inst, Natl Museum African Art, Washington, DC 20560 USA. EM kreamerc@si.edu NR 33 TC 0 Z9 0 U1 0 U2 0 PU MIT PRESS PI CAMBRIDGE PA 55 HAYWARD STREET, CAMBRIDGE, MA 02142 USA SN 0001-9933 J9 AFR ARTS JI Afr. Arts PD SPR PY 2010 VL 43 IS 1 SI SI BP 14 EP 27 PG 14 WC Art SC Art GA 561KK UT WOS:000274975400004 ER PT J AU Binkley, DA AF Binkley, David A. TI Southern Kuba Initiation Rites The Ephemeral Face of Power and Secrecy SO AFRICAN ARTS LA English DT Article C1 [Binkley, David A.] Smithsonian Inst, Natl Museum African Art, Washington, DC 20560 USA. [Binkley, David A.] Univ Missouri, Columbia, MO 65211 USA. RP Binkley, DA (reprint author), Smithsonian Inst, Natl Museum African Art, Washington, DC 20560 USA. EM dabinkley@verizon.net NR 14 TC 0 Z9 0 U1 1 U2 1 PU M I T PRESS PI CAMBRIDGE PA 238 MAIN STREET, STE 500, CAMBRIDGE, MA 02142-1046 USA SN 0001-9933 J9 AFR ARTS JI Afr. Arts PD SPR PY 2010 VL 43 IS 1 SI SI BP 44 EP 59 DI 10.1162/afar.2010.43.1.44 PG 16 WC Art SC Art GA 561KK UT WOS:000274975400006 ER PT J AU Triplett, JK Oltrogge, KA Clark, LG AF Triplett, Jimmy K. Oltrogge, Kimberly A. Clark, Lynn G. TI PHYLOGENETIC RELATIONSHIPS AND NATURAL HYBRIDIZATION AMONG THE NORTH AMERICAN WOODY BAMBOOS (POACEAE: BAMBUSOIDEAE: ARUNDINARIA) SO AMERICAN JOURNAL OF BOTANY LA English DT Article DE AFLP; Arundinaria; bamboo phylogeny; Bambusoideae; natural hybridization; Poaceae; temperate bamboos ID FRAGMENT LENGTH POLYMORPHISM; SOUTHEASTERN UNITED-STATES; SPATIAL GENETIC-STRUCTURE; MULTILOCUS GENOTYPE DATA; POPULATION-STRUCTURE; HYBRID SPECIATION; CLONAL DIVERSITY; CHLOROPLAST DNA; SEQUENCE DATA; PHYLLOSTACHYS BAMBUSOIDEAE AB In spite of the ecological and economic importance of temperate bamboos, relatively little is known about their population biology or evolutionary history. Recently, hybridization has emerged as a potential source of diversity in this group, as well as an underlying cause of taxonomic problems. As part of a broader phylogenetic study of the temperate bamboos, we report the results of an analysis of the North American Arundinaria gigantea species complex, including estimates of genetic variation and molecular evidence of natural hybridization among A. gigantea, A. tecta, and A. appalachiana. The study involved a comparative analysis of amplified fragment length polymorphisms (AFLPs) and chloroplast DNA sequences representing diversity within and among all three species plus individuals with intermediate or unusual morphological characteristics (putative hybrids). Molecular results support the recognition of three species previously defined on the basis of morphology, anatomy, and ecology, with most of the molecular variance accounted for by among-species variation. Molecular evidence also demonstrates that A. tecta and A. appalachiana are sister species, forming a clade that is significantly divergent from A. gigantea. The role of hybridization in the phylogenetic history of Arundinaria is discussed along with implications for the evolution and taxonomy of the temperate woody bamboos. C1 [Triplett, Jimmy K.; Oltrogge, Kimberly A.; Clark, Lynn G.] Iowa State Univ, Dept Ecol Evolut & Organismal Biol, Ames, IA 50011 USA. RP Triplett, JK (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, MRC 166, Washington, DC 20013 USA. EM triplettj@si.edu FU American Society of Plant Taxonomists; American Bamboo Society; National Geographic Society [7336-02] FX The authors thank A. Gholson, M. Hotchkiss, A. Weakley, G. Kauffman, and J. Campbell for assistance locating natural populations; A. and S. Turtle (Earth Advocates Research Farm, Summertown, TN) and J. York (Bamboo Sourcery, Sebastopol, CA) for access to bamboos in cultivation; staff of the Great Dismal Swamp National Wildlife Refuge (VA) and Desoto State Park (AL) for access to protected populations; and M. Ozaki for help with fieldwork. The authors thank R. Percifield, C. Grover, and C. Tyrrell for technical assistance; J. Wendel and R. Wallace for access to laboratory facilities; and J. Nason for comments that substantially improved the manuscript. Fieldwork was supported by a Graduate Research Grant from the American Society of Plant Taxonomists and grants from the American Bamboo Society to J. T. and the National Geographic Society (#7336-02) to L. C. Support for J. T. for laboratory analyses and final preparation of this manuscript NR 190 TC 22 Z9 22 U1 4 U2 13 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 MAR PY 2010 VL 97 IS 3 BP 471 EP 492 DI 10.3732/ajb.0900244 PG 22 WC Plant Sciences SC Plant Sciences GA 563DF UT WOS:000275106800011 PM 21622410 ER PT J AU Saverschek, N Herz, H Wagner, M Roces, F AF Saverschek, N. Herz, H. Wagner, M. Roces, F. TI Avoiding plants unsuitable for the symbiotic fungus: learning and long-term memory in leaf-cutting ants SO ANIMAL BEHAVIOUR LA English DT Article DE Atta colombica; aversive learning; delayed rejection; experience; foraging; host plant selection; leaf-cutting ant; memory; Panama ID ACROMYRMEX-OCTOSPINOSUS REICH; ATTA-CEPHALOTES L; MUTUALISTIC FUNGUS; DECISION-MAKING; MANDUCA-SEXTA; HOST PLANTS; FORMICIDAE; SEXDENS; SELECTION; HYMENOPTERA AB Leaf-cutting ants are polyphagous herbivores that, despite their catholicity, show distinct preferences in the substrate choice for their symbiotic fungus. We investigated to what extent avoidance learning and long-term memory for plant unsuitability underlie foraging responses in the field. First, the acceptability of 10 rarely harvested plant species was tested on field colonies located in two different habitats, where the tested plant species were either present or not. Colonies in the habitat where the plant species occurred avoided all species on first encounter, suggesting previous experience with them. Colonies without the plant species in their habitat, however, first accepted, but then avoided four of them when tested after 24 and 48 h. Such an avoidance response towards previously acceptable leaves could be experimentally induced by infiltrating acceptable leaves with a fungicide (cycloheximide) not detectable to the ants, but harmful to the symbiotic fungus, indicating that workers learn to reject plants that have detrimental effects on the fungus, but not on themselves. To determine how robust memory for plant unsuitability was, workers from field colonies were offered the previously avoided, yet untreated plant every 2 weeks, and its acceptance monitored in the long term. It took up to 18 weeks until foragers harvested the plant again, indicating the involvement of robust long-term avoidance learning in foragers. We argue that the harvesting pattern observed in field colonies largely depends on the workers' foraging experience, essential in a highly diverse environment where both leaf availability and quality vary throughout the year. (C) 2009 The Association for the Study of Animal Behaviour. Published by Elsevier Ltd. All rights reserved. C1 [Saverschek, N.; Wagner, M.; Roces, F.] Univ Wurzburg, Bioctr, D-97074 Wurzburg, Germany. [Herz, H.] Smithsonian Trop Res Inst, Washington, DC USA. RP Roces, F (reprint author), Univ Wurzburg, Bioctr, D-97074 Wurzburg, Germany. EM roces@biozentrum.uni-wuerzburg.de FU German Academic Exchange Service; Smithsonian Tropical Research Institute; German Science Foundation (DFG) [567/TPC4] FX We thank the Editor and two anonymous referees for comments that helped improve the manuscript. This research was supported by the German Academic Exchange Service (DAAD scholarship granted to N.S.), the Smithsonian Tropical Research Institute, and the German Science Foundation (DFG), Sonderforschungsbereich 567/TPC4 'Mechanisms of Interspecific Interactions of Organisms'. NR 51 TC 27 Z9 27 U1 2 U2 50 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0003-3472 EI 1095-8282 J9 ANIM BEHAV JI Anim. Behav. PD MAR PY 2010 VL 79 IS 3 BP 689 EP 698 DI 10.1016/j.anbehav.2009.12.021 PG 10 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA 556JR UT WOS:000274587400023 ER PT J AU Sosa-Calvo, J Schultz, TR AF Sosa-Calvo, J. Schultz, T. R. TI Three Remarkable New Fungus-Growing Ant Species of the Genus Myrmicocrypta (Hymenoptera: Formicidae), With a Reassessment of the Characters That Define the Genus and Its Position Within the Attini SO ANNALS OF THE ENTOMOLOGICAL SOCIETY OF AMERICA LA English DT Article DE Brazil; Myrmicocrypta erectapilosa sp nov.; Myrmicocrypta camargoi sp nov.; Myrmicocrypta bucki sp nov.; Myrmicinae ID AGRICULTURE; PHYLOGENY; SEQUENCE; N. AB Three new species of the fungus-growing ant genus Myrmicocrypta Fr. Smith are described from Brazil and Peru, all unique within the genus due to their shared character state of erect pilosity. Myrmicocrypta erectapilosa sp. nov. and Myrmicocrypta bucki sp. nov. are otherwise typical for the genus in their small size and effaced, tuberculate sculpture, whereas Myrmicocrypta camargoi sp. nov. is also unique in its large size and pronounced sculpture. M. erectapilosa and M. bucki are closely related but can be distinguished by differences in the frontoclypeal and hypostomal teeth, frontal lobes, mesonotal sculpture, and propodeal spines. All castes (workers, gynes, and males) are described for M. camargoi, workers and gynes are described for M. erectapilosa, and only workers are described for M. bucki. Because the erect pilosity encountered in these species contradicts the state previously considered diagnostic for the genus, that of appressed, spatulate or squamiform pilosity found in all other Myrmicocrypta species, we necessarily discuss the characters that define the genus Myrmicocrypta and review its phylogenetic position within the tribe Attini. C1 [Sosa-Calvo, J.; Schultz, T. R.] Natl Museum Nat Hist, Dept Entomol, Smithsonian Inst, Washington, DC 20013 USA. [Sosa-Calvo, J.] Univ Maryland, Dept Entomol, Maryland Ctr Systemat Entomol, College Pk, MD 20742 USA. RP Schultz, TR (reprint author), Natl Museum Nat Hist, Dept Entomol, Smithsonian Inst, POB 37012,MRC 188 CE516, Washington, DC 20013 USA. EM schultzt@si.edu FU National Science Foundation [DEB 0110073, DEB 0431330]; Harvard University; University of Maryland; Amazon Conservation Association FX We are grateful to R. S. Camargo for collecting the type specimens of M. camargoi, to C. Rabeling and M. Verhaag for collecting additional specimens of M. bucki and to A. B. Casimiro, A. Y. Harada, and A. G. Bandeira for collecting the specimens of M. erectapilosa. We thank an anonymous reviewer for commenting on the manuscript. Carlos Roberto K Brandao (MZSP), Jacques Delabie (CPDC), Ana Harada (MPEG), Christian Rabeling (University of Texas at Austin), Roy Snelling, (LACM) and M. Verhaag (SMNK) loaned its specimens. Eugenia Okonski (USNM) photographed the worker of M. erectapilosa. Elaine Hodges and Vichai Malikul created the illustrations. Astrid Caldas provided information about Rio de Janeiro. This research was supported in part by National Science Foundation grants DEB 0110073 and DEB 0431330 (to T.R.S.). J.S.-C. was supported in part by an Ernst Mayr Travel Award in Animal Systematics (Harvard University), a Jacob K. Goldhaber Travel Award (University of Maryland), and an Amazon Conservation Association Graduate Research Grant. NR 65 TC 5 Z9 5 U1 1 U2 3 PU ENTOMOLOGICAL SOC AMER PI ANNAPOLIS PA 3 PARK PLACE, STE 307, ANNAPOLIS, MD 21401-3722 USA SN 0013-8746 EI 1938-2901 J9 ANN ENTOMOL SOC AM JI Ann. Entomol. Soc. Am. PD MAR PY 2010 VL 103 IS 2 BP 181 EP 195 DI 10.1603/AN09108 PG 15 WC Entomology SC Entomology GA 566QC UT WOS:000275386800007 ER PT J AU Pratt, LM Allen, C Allwood, A Anbar, A Atreya, S Carr, M Des Marais, D Grant, J Glavin, D Hamilton, V Herkenhoff, K Hipkin, V Lollar, BS McCollom, T McEwen, A McLennan, S Milliken, R Ming, D Ori, GG Parnell, J Poulet, F Westall, F AF Pratt, Lisa M. Allen, Carl Allwood, Abby Anbar, Ariel Atreya, Sushil Carr, Mike Des Marais, Dave Grant, John Glavin, Daniel Hamilton, Vicky Herkenhoff, Ken Hipkin, Vicky Lollar, Barbara Sherwood McCollom, Tom McEwen, Alfred McLennan, Scott Milliken, Ralph Ming, Doug Ori, Gian Gabrielle Parnell, John Poulet, Francois Westall, Frances CA Mars Mid-Range Rover Sci Anal Grp TI The Mars Astrobiology Explorer-Cacher (MAX-C): A Potential Rover Mission for 2018 SO ASTROBIOLOGY LA English DT Article ID BARBERTON MOUNTAIN LAND; RAMAN CROSS-SECTIONS; MARTIAN DUST STORMS; WESTERN-AUSTRALIA; MERIDIANI-PLANUM; OMEGA/MARS EXPRESS; MAGNETIC-FIELD; SOUTH-AFRICA; WARRAWOONA GROUP; ONVERWACHT GROUP C1 [Pratt, Lisa M.] Indiana Univ, Bloomington, IN 47405 USA. [Allen, Carl; Ming, Doug] NASA, Lyndon B Johnson Space Ctr, Washington, DC USA. [Allwood, Abby; Milliken, Ralph] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Anbar, Ariel] Arizona State Univ, Tempe, AZ 85287 USA. [Atreya, Sushil] Univ Michigan, Ann Arbor, MI 48109 USA. [Des Marais, Dave] NASA, Ames Res Ctr, Washington, DC USA. [Grant, John] Smithsonian Inst, Washington, DC 20560 USA. [Glavin, Daniel] NASA, Goddard Space Flight Ctr, Washington, DC USA. [Hamilton, Vicky] SW Res Inst, San Antonio, TX USA. [Lollar, Barbara Sherwood] Univ Toronto, Toronto, ON M5S 1A1, Canada. [McEwen, Alfred] Univ Arizona, Tucson, AZ 85721 USA. [McCollom, Tom] Univ Colorado, Boulder, CO 80309 USA. [McLennan, Scott] SUNY Stony Brook, Stony Brook, NY 11794 USA. [Parnell, John] Univ Aberdeen, Aberdeen AB9 1FX, Scotland. [Poulet, Francois] Univ Paris 11, Paris, France. [Westall, Frances] CNRS, F-75700 Paris, France. RP Pratt, LM (reprint author), Indiana Univ, Bloomington, IN 47405 USA. EM prattl@indiana.edu; Abigail.C.Allwood@jpl.nasa.gov RI Glavin, Daniel/D-6194-2012; OI Glavin, Daniel/0000-0001-7779-7765; Crisp, Joy/0000-0002-3202-4416 NR 167 TC 7 Z9 7 U1 0 U2 12 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 MAR PY 2010 VL 10 IS 2 BP 127 EP 163 DI 10.1089/ast.2010.0462 PG 37 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 585IN UT WOS:000276818700001 ER PT J AU Lal, DV Ho, LC AF Lal, Dharam Vir Ho, Luis C. TI THE RADIO PROPERTIES OF TYPE 2 QUASARS SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: jets; galaxies: nuclei; galaxies: Seyfert; galaxies: structure; radio continuum: galaxies ID DIGITAL-SKY-SURVEY; ACTIVE GALACTIC NUCLEI; HARD X-RAY; COMPACT STEEP-SPECTRUM; DUST-REDDENED QUASARS; O II EMISSION; QUIET QUASARS; STAR-FORMATION; LUMINOSITY FUNCTION; SEYFERT-GALAXIES AB This paper presents the first high-resolution and high-sensitivity study of the radio properties of optically selected type 2 quasars. We used the Very Large Array at 8.4 GHz to observe 59 sources drawn from the Sloan Digital Sky Survey sample of Zakamska et al.. The detection rate of our survey is 59% (35/59), comparable to the detection rate in FIRST at 1.4 GHz. Ongoing star formation, although present, contributes negligible radio emission at the current sensitivity limit. Comparing the radio powers with the [O III] lambda 5007 luminosities, we find that roughly 15% +/- 5% of the sample can be considered radio loud. Intriguingly, the vast majority of the detected sources in our sample fall in a region intermediate between those traditionally occupied by radio loud and radio quiet quasars. Moreover, most of these "radio intermediate" sources tend to have flat or inverted radio spectra, which we speculate may be caused by free-free absorption by ionized gas in the narrow-line region. The incidence of flat-spectrum sources in type 2 quasars appears to be much higher than in type 1 quasars, in apparent violation of the simple orientation-based unified model for active galaxies. C1 [Lal, Dharam Vir] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Lal, Dharam Vir] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ho, Luis C.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA. RP Lal, DV (reprint author), Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 10617, Taiwan. FU Carnegie Institution for Science FX We thank the anonymous referee for his/her comments that improved this paper. The VLA is operated by the U.S. National Radio Astronomy Observatory. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. We thank the staff of the VLA for carrying out these observations in their usual efficient manner. D. V. L. acknowledges the assistance from J. Lim and P. T. P. Ho on several occasions. L. C. H. thanks Jim Ulvestad for advice and Nadia Zakamska for clarification on the [O III] luminosity conversion of her sample. The work of L. C. H. is supported by the Carnegie Institution for Science. NR 83 TC 27 Z9 27 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD MAR PY 2010 VL 139 IS 3 BP 1089 EP 1105 DI 10.1088/0004-6256/139/3/1089 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 554IV UT WOS:000274429600023 ER PT J AU Nantais, JB Huchra, JP Barmby, P Olsen, KAG AF Nantais, Julie B. Huchra, John P. Barmby, Pauline Olsen, Knut A. G. TI NEARBY SPIRAL GALAXY GLOBULAR CLUSTER SYSTEMS. II. GLOBULAR CLUSTER METALLICITIES IN NGC 300 SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies: individual (NGC 300); galaxies: spiral; galaxies: star clusters: general ID OLD STELLAR POPULATIONS; EXTRAGALACTIC DISTANCE SCALE; FORNAX DWARF GALAXY; KECK SPECTROSCOPY; SCULPTOR GROUP; KEY PROJECT; DATA-BASE; M81; CALIBRATION; PARAMETERS AB We present new metallicity estimates for globular cluster (GC) candidates in the Sd spiral NGC 300, one of the nearest spiral galaxies outside the Local Group. We have obtained optical spectroscopy for 44 Sculptor Group GC candidates with the Boller and Chivens (B&C) spectrograph on the Baade Telescope at Las Campanas Observatory. There are two GCs in NGC 253 and 12 objects in NGC 300 with globular-cluster-like spectral features, nine of which have radial velocities above 0 km s(-1). The remaining three, due to their radial velocities being below the expected 95% confidence limit for velocities of NGC 300 halo objects, are flagged as possible foreground stars. The non-cluster-like candidates included 13 stars, 15 galaxies, and an H II region. One GC, four galaxies, two stars, and the H II region from our sample were identified in archival Hubble Space Telescope images. For the GCs, we measure spectral indices and estimate metallicities using an empirical calibration based on Milky Way GCs. The GCs of NGC 300 appear similar to those of the Milky Way. Excluding possible stars and including clusters from the literature, the GC system (GCS) has a velocity dispersion of 68 km s(-1) and has no clear evidence of rotation. The mean metallicity for our full cluster sample plus one literature object is [Fe/H] = -0.94, lying above the relationship between mean GC metallicity and overall galaxy luminosity. Excluding the three low-velocity candidates, we obtain a mean [Fe/H] = -0.98, still higher than expected, raising the possibility of significant foreground star contamination even in this sample. Visual confirmation of genuine GCs using high-resolution space-based imagery could greatly reduce the potential problem of interlopers in small samples of GCSs in low-radial-velocity galaxies. C1 [Nantais, Julie B.; Huchra, John P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Barmby, Pauline] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [Olsen, Knut A. G.] Cerro Tololo Interamer Observ, Natl Opt Astron Observ, La Serena, Chile. RP Nantais, JB (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Barmby, Pauline/I-7194-2016 OI Barmby, Pauline/0000-0003-2767-0090 FU Smithsonian Institution; Harvard College Observatory FX We thank the LCO staff for helping us use the Magellan Telescopes and instruments. This work has been supported by the Smithsonian Institution and Harvard College Observatory. We also thank Ricardo Schiavon and collaborators for making their Milky Way spectra available to the public at http://www.noao.edu/ggclib/. NR 57 TC 7 Z9 7 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD MAR PY 2010 VL 139 IS 3 BP 1178 EP 1189 DI 10.1088/0004-6256/139/3/1178 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 554IV UT WOS:000274429600030 ER PT J AU Stefanik, RP Torres, G Lovegrove, J Pera, VE Latham, DW Zajac, J Mazeh, T AF Stefanik, Robert P. Torres, Guillermo Lovegrove, Justin Pera, Vivian E. Latham, David W. Zajac, Joseph Mazeh, Tsevi TI EPSILON AURIGAE: AN IMPROVED SPECTROSCOPIC ORBITAL SOLUTION SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries: eclipsing; stars: individual (epsilon Aurigae); techniques: radial velocities ID RADIAL-VELOCITIES; BINARIES; SECONDARY; ECLIPSE AB A rare eclipse of the mysterious object epsilon Aurigae will occur in 2009-2011. We report an updated single-lined spectroscopic solution for the orbit of the primary star based on 20 years of monitoring at the CfA, combined with historical velocity observations dating back to 1897. There are 518 new CfA observations obtained between 1989 and 2009. Two solutions are presented. One uses the velocities outside the eclipse phases together with mid-times of previous eclipses, from photometry dating back to 1842, which provide the strongest constraint on the ephemeris. This yields a period of 9896.0 +/- 1.6 days (27.0938 +/- 0.0044 years) with a velocity semi-amplitude of 13.84 +/- 0.23 km s(-1) and an eccentricity of 0.227 +/- 0.011. The middle of the current ongoing eclipse predicted by this combined fit is JD 2,455,413.8 +/- 4.8, corresponding to 2010 August 5. If we use only the radial velocities, we find that the predicted middle of the current eclipse is nine months earlier. This would imply that the gravitating companion is not the same as the eclipsing object. Alternatively, the purely spectroscopic solution may be biased by perturbations in the velocities due to the short-period oscillations of the supergiant. C1 [Stefanik, Robert P.; Torres, Guillermo; Lovegrove, Justin; Latham, David W.; Zajac, Joseph] Harvard Smithsonian Ctr Astrophys CfA, Cambridge, MA 02138 USA. [Lovegrove, Justin] Univ Southampton, Appl Math Grp, Southampton SO17 1BJ, Hants, England. [Pera, Vivian E.] MIT Lincoln Lab, Lexington, MA 02420 USA. [Mazeh, Tsevi] Tel Aviv Univ, Wise Observ, IL-69978 Tel Aviv, Israel. [Mazeh, Tsevi] Harvard Univ, Radcliffe Inst Adv Studies, Cambridge, MA 02138 USA. RP Stefanik, RP (reprint author), Harvard Smithsonian Ctr Astrophys CfA, 60 Garden St, Cambridge, MA 02138 USA. EM rstefanik@cfa.harvard.edu NR 40 TC 19 Z9 19 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD MAR PY 2010 VL 139 IS 3 BP 1254 EP 1260 DI 10.1088/0004-6256/139/3/1254 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 554IV UT WOS:000274429600035 ER PT J AU Lombardi, M Lada, CJ Alves, J AF Lombardi, M. Lada, C. J. Alves, J. TI 2MASS wide field extinction maps III. The Taurus, Perseus, and California cloud complexes SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: clouds; dust, extinction; ISM: individual objects: Taurus molecular complex; ISM: structure; methods: statistical ID STAR-FORMING REGIONS; FULLY-DEVELOPED TURBULENCE; MOLECULAR CLOUDS; PROBABILITY-DISTRIBUTION; SUPERSONIC TURBULENCE; OB ASSOCIATIONS; COLUMN DENSITY; DARK CLOUDS; PIPE NEBULA; GAS AB We present a near-infrared extinction map of a large region in the sky (similar to 3500 deg(2)) in the general directions of Taurus, Perseus, and Aries. The map has been obtained using robust and optimal methods to map dust column density at near-infrared wavelengths (Nicer, described in Lombardi & Alves 2001, A&A, 377, 1023 and Nicest, described in Lombardi 2009, A&A, 493, 735) toward similar to 23 million stars from the Two Micron All Sky Survey (2MASS) point source catalog. We measure extinction as low as A(K) = 0.04 mag with a 1-sigma significance, and a resolution of 2.5 arcmin in our map. A 250 deg(2) section of our map encompasses the Taurus, Perseus, and California molecular cloud complexes. We determine the distances of the clouds by comparing the observed density of foreground stars with the prediction of galactic models, and we obtain results that are in excellent agreement with recent VLBI parallax measurements. We characterize the large-scale structure of the map and find a similar to 25 degrees x 15 degrees region close to the galactic plane (l similar to 135 degrees, b similar to -14 degrees) with small extinction (A(K) < 0.04 mag); we name this region the Perseus-Andromeda hole. We find that over the region that encompasses the Taurus, Perseus, and California clouds the column density measurements below A(K) < 0.2 mag are perfectly described by a log-normal distribution, and that a significant deviation is observed at larger extinction values. If turbulence models are invoked to justify the log-normal distribution, the observed departure could be interpreted as the result of the effect of gravity that acts on the cores of the clouds. Finally, we investigate the cloud structure function, and show that significant deviations from the results predicted by turbulent models are observed in at least one cloud. C1 [Lombardi, M.] European So Observ, D-85748 Garching, Germany. [Lada, C. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Alves, J.] Ctr Astron Hispano Aleman, Calar Alto Observ, Almeria 04004, Spain. RP Lombardi, M (reprint author), European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. EM mlombard@eso.org OI LOMBARDI, MARCO/0000-0002-3336-4965; Alves, Joao/0000-0002-4355-0921 FU National Aeronautics and Space Administration; NASA ORIGINS [NAG 5-13041] FX It is a pleasure to thank Tom Dame for many useful discussions. This research has made use of the 2MASS archive, provided by NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. C.J.L. acknowledges support from NASA ORIGINS Grant NAG 5-13041. NR 56 TC 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 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAR-APR PY 2010 VL 512 AR A67 DI 10.1051/0004-6361/200912670 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 577SY UT WOS:000276245500042 ER PT J AU Lusso, E Comastri, A Vignali, C Zamorani, G Brusa, M Gilli, R Iwasawa, K Salvato, M Civano, F Elvis, M Merloni, A Bongiorno, A Trump, JR Koekemoer, AM Schinnerer, E Le Floc'h, E Cappelluti, N Jahnke, K Sargent, M Silverman, J Mainieri, V Fiore, F Bolzonella, M Le Fevre, O Garilli, B Iovino, A Kneib, JP Lamareille, F Lilly, S Mignoli, M Scodeggio, M Vergani, D AF Lusso, E. Comastri, A. Vignali, C. Zamorani, G. Brusa, M. Gilli, R. Iwasawa, K. Salvato, M. Civano, F. Elvis, M. Merloni, A. Bongiorno, A. Trump, J. R. Koekemoer, A. M. Schinnerer, E. Le Floc'h, E. Cappelluti, N. Jahnke, K. Sargent, M. Silverman, J. Mainieri, V. Fiore, F. Bolzonella, M. Le Fevre, O. Garilli, B. Iovino, A. Kneib, J. P. Lamareille, F. Lilly, S. Mignoli, M. Scodeggio, M. Vergani, D. TI The X-ray to optical-UV luminosity ratio of X-ray selected type 1 AGN in XMM-COSMOS SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: active; Galaxy: evolution; quasars: general; methods: statistical ID ACTIVE GALACTIC NUCLEI; DIGITAL SKY SURVEY; QUASI-STELLAR OBJECTS; WIDE-FIELD SURVEY; CHANDRA MULTIWAVELENGTH PROJECT; SPECTRAL ENERGY-DISTRIBUTIONS; HIGH-REDSHIFT QUASARS; ASTRONOMICAL DATA; HOST GALAXIES; RADIO-QUIET AB We present a study of the X-ray to optical properties of a sample of 545 X-ray selected type 1 AGN, from the XMM-COSMOS survey, over a wide range of redshifts (0.04 < z < 4.25) and X-ray luminosities (40.6 <= Log L([2-10]) (keV) <= 45.3). About 60% of them are spectroscopically identified type 1 AGN, while the others have a reliable photometric redshift and are classified as type 1 AGN on the basis of their multi-band Spectral Energy Distributions. We discuss the relationship between UV and X-ray luminosity, as parameterized by the alpha(ox) spectral slope, and its dependence on redshift and luminosity. We compare our findings with previous investigations of optically selected broad-line AGN (mostly from SDSS). A highly significant correlation between alpha(ox) and L(2500) angstrom is found, in agreement with previous investigations of optically selected samples. We calculate bolometric corrections, k(bol), for the whole sample using hard X-ray luminosities (L([2-10] keV)), and the Eddington ratios for a subsample of 150 objects for which black hole mass estimates are available. We confirm the trend of increasing bolometric correction with increasing Eddington ratio as proposed in previous works. A tight correlation is found between alpha(ox) and k(bol), which can be used to estimate accurate bolometric corrections using only optical and X-ray data. We find a significant correlation between alpha(ox) and Eddington ratio, in which the ratio between X-ray and optical flux decreases with increasing Eddington ratio. C1 [Lusso, E.; Vignali, C.; Vergani, D.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. [Lusso, E.; Comastri, A.; Vignali, C.; Zamorani, G.; Gilli, R.; Iwasawa, K.; Mignoli, M.; Vergani, D.] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy. [Brusa, M.; Merloni, A.; Bongiorno, A.; Cappelluti, N.; Mainieri, V.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Salvato, M.] CALTECH, Pasadena, CA 91125 USA. [Civano, F.; Elvis, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Merloni, A.] Excellence Cluster Univ, D-85748 Garching, Germany. [Trump, J. R.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Koekemoer, A. M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Schinnerer, E.; Jahnke, K.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Le Floc'h, E.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Sargent, M.; Silverman, J.; Lilly, S.] ETH, Dept Phys, CH-8093 Zurich, Switzerland. [Mainieri, V.] ESO, D-85748 Garching, Germany. [Fiore, F.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Rm, Italy. [Le Fevre, O.; Kneib, J. P.] Univ Aix Marseille, CNRS, OAMP, Lab Astrophys Marseille, F-13388 Marseille 13, France. [Garilli, B.; Scodeggio, M.] INAF IASF, I-20133 Milan, Italy. [Iovino, A.] Osserv Astron Brera, INAF, I-20121 Milan, Italy. [Lamareille, F.] Univ Toulouse, CNRS, Lab Astrophys Toulouse Tarbes, F-31400 Toulouse, France. RP Lusso, E (reprint author), Univ Bologna, Dipartimento Astron, Via Ranzani 1, I-40127 Bologna, Italy. EM elisabeta.lusso2@unibo.it RI Le Fevre, Olivier/G-7389-2011; Vignali, Cristian/J-4974-2012; Kneib, Jean-Paul/A-7919-2015; Mignoli, Marco/O-9426-2015; Bolzonella, Micol/O-9495-2015; Comastri, Andrea/O-9543-2015; Gilli, Roberto/P-1110-2015; OI Jahnke, Knud/0000-0003-3804-2137; Scodeggio, Marco/0000-0002-2282-5850; Vergani, Daniela/0000-0003-0898-2216; Cappelluti, Nico/0000-0002-1697-186X; Garilli, Bianca/0000-0001-7455-8750; Zamorani, Giovanni/0000-0002-2318-301X; Koekemoer, Anton/0000-0002-6610-2048; Schinnerer, Eva/0000-0002-3933-7677; Brusa, Marcella/0000-0002-5059-6848; Fiore, Fabrizio/0000-0002-4031-4157; Vignali, Cristian/0000-0002-8853-9611; Kneib, Jean-Paul/0000-0002-4616-4989; Mignoli, Marco/0000-0002-9087-2835; Bolzonella, Micol/0000-0003-3278-4607; Comastri, Andrea/0000-0003-3451-9970; Gilli, Roberto/0000-0001-8121-6177; Bongiorno, Angela/0000-0002-0101-6624; Iovino, Angela/0000-0001-6958-0304 FU PRIN/MIUR [2006-02-5203]; ASI-INAF [I/023/05/00, I/088/06, ASI/COFIS/WP3110I/026/07/0]; Bundesministerium fur Wirtshaft und Techologie/Deutsches Zentrum fur Luft und Raumfahrt; Max-Planck society FX In Italy, the XMM-COSMOS project is supported by PRIN/MIUR under grant 2006-02-5203, ASI-INAF grants I/023/05/00, I/088/06 and ASI/COFIS/WP3110I/026/07/0. In Germany the XMM-Newton project is supported by the Bundesministerium fur Wirtshaft und Techologie/Deutsches Zentrum fur Luft und Raumfahrt and the Max-Planck society. The entire COSMOS collaboration is gratefully acknowledged. NR 79 TC 87 Z9 87 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 MAR-APR PY 2010 VL 512 AR A34 DI 10.1051/0004-6361/200913298 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 577SY UT WOS:000276245500024 ER PT J AU Vollmer, B Soida, M Chung, A Beck, R Urbanik, M Chyzy, KT Otmianowska-Mazur, K van Gorkom, JH AF Vollmer, B. Soida, M. Chung, A. Beck, R. Urbanik, M. Chyzy, K. T. Otmianowska-Mazur, K. van Gorkom, J. H. TI The influence of the cluster environment on the large-scale radio continuum emission of 8 Virgo cluster spirals SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: interactions; galaxies: ISM; galaxies: magnetic fields; radio continuum: galaxies ID RAM-PRESSURE; MAGNETIC-FIELDS; STAR-FORMATION; GALAXY NGC-6946; GASEOUS HALO; GAS; NGC-4438; DISK; MORPHOLOGIES; DIAGNOSTICS AB The influence of the environment on the polarized and total power radio continuum emission of cluster spiral galaxies is investigated. We present deep scaled array VLA 20 and 6 cm observations including polarization of 8 Virgo spiral galaxies. These data are combined with existing optical, HI, and H alpha data. Ram pressure compression leads to sharp edges of the total power distribution at one side of the galactic disk. These edges coincide with HI edges. In edge-on galaxies the extraplanar radio emission can extend further than the Hi emission. In the same galaxies asymmetric gradients in the degree of polarization give additional information on the ram pressure wind direction. The local total power emission is not sensitive to the effects of ram pressure. The radio continuum spectrum might flatten in the compressed region only for very strong ram pressure. This implies that neither the local star formation rate nor the turbulent small-scale magnetic field are significantly affected by ram pressure. Ram pressure compression occurs mainly on large scales (greater than or similar to 1 kpc) and is primarily detectable in polarized radio continuum emission. C1 [Vollmer, B.] Observ Astron, CDS, UMR 7550, F-67000 Strasbourg, France. [Soida, M.; Urbanik, M.; Chyzy, K. T.; Otmianowska-Mazur, K.] Jagiellonian Univ, Astron Observ, Krakow, Poland. [Chung, A.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Beck, R.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [van Gorkom, J. H.] Columbia Univ, Dept Astron, New York, NY 10027 USA. RP Vollmer, B (reprint author), Observ Astron, CDS, UMR 7550, 11 Rue Univ, F-67000 Strasbourg, France. EM bvollmer@astro.u-strasbg.fr FU Polish-French (ASTRO-LEA-PF) cooperation; Polish Ministry of Sciences and Higher Education [3033/B/H03/2008/35] FX This research has made use of the GOLD Mine Database. This work was supported by the Polish-French (ASTRO-LEA-PF) cooperation program and by the Polish Ministry of Sciences and Higher Education grant 3033/B/H03/2008/35. The authors would like to thank E. M. Berkhuijsen for careful reading of the manuscript. NR 53 TC 14 Z9 14 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 MAR-APR PY 2010 VL 512 AR A36 DI 10.1051/0004-6361/200913591 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 577SY UT WOS:000276245500025 ER PT J AU Zurita, C Kuulkers, E Bandyopadhyay, RM Cackett, EM Groot, PJ Orosz, JA Torres, MAP Wijnands, R AF Zurita, C. Kuulkers, E. Bandyopadhyay, R. M. Cackett, E. M. Groot, P. J. Orosz, J. A. Torres, M. A. P. Wijnands, R. TI Optical/infrared observations of the X-ray burster KS1731-260 in quiescence SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE astrometry; X-rays: binaries; stars: individual: KS 1731-260 ID BLACK-HOLE BINARIES; KS 1731-260; NEUTRON-STAR; INFRARED OBSERVATIONS; KS-1731-260; SYSTEMS; TRANSIENTS; PHOTOMETRY; A0620-00 AB Aims. We performed an optical/infrared study of the counterpart of the low-mass X-ray binary KS 1731-260 to test its identification and obtain information about the donor. Methods. Optical and infrared images of the counterpart of KS 1731-260 were taken in two different epochs (2001 and 2007) after the source returned to quiescence in X-rays. We compared these observations with those obtained when KS 1731-260 was still active. Results. We confirm the identification of KS 1731-260 with the previously proposed counterpart and improve its position to alpha = 17:34:13.46 and delta = -26:05:18.60. The H-band magnitude of this candidate showed a decline of similar to 1.7 mag from outburst to quiescence. In 2007 April we obtained R = 22.8 +/- 0.1 and I = 20.9 +/- 0.1 for KS 1731-260. Similar optical brightness was measured in June 2001 and July 2007. The intrinsic optical color R-I is consistent with spectral types from F to G for the secondary although there is a large excess over that from the secondary at the infrared wavelengths. This may be due to emission from the cooler outer regions of the accretion disk. We cannot rule out a brown dwarf as a donor star, although it would require that the distance to the source is significantly lower than the 7 kpc reported by Muno et al. (2000, ApJ, 542, 1016). C1 [Zurita, C.] Inst Astrofis Canarias, San Cristobal la Laguna 3800, Spain. [Zurita, C.] Univ La Laguna, Dept Astrofis, Tenerife 38205, Spain. [Kuulkers, E.] European Space Astron Ctr ESAC, ESA, ISOC, Madrid 28691, Spain. [Bandyopadhyay, R. M.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Cackett, E. M.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Groot, P. J.] Radboud Univ Nijmegen, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands. [Orosz, J. A.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. [Torres, M. A. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. [Wijnands, R.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. RP Zurita, C (reprint author), Inst Astrofis Canarias, C Via Lactea S-N, San Cristobal la Laguna 3800, Spain. EM czurita@iac.es OI Groot, Paul/0000-0002-4488-726X FU NASA [PF8-90052] FX We thank Christian Motch for providing the archival CFHT data. C.Z. is grateful to Celia Sanchez and for the hospitality of the ESA, European Space Astronomy Centre (ESAC). E. M. C. gratefully acknowledges support provided by NASA through the Chandra Fellowship Program, grant number PF8-90052. NR 33 TC 2 Z9 2 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAR-APR PY 2010 VL 512 AR A26 DI 10.1051/0004-6361/200913061 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 577SY UT WOS:000276245500048 ER PT J AU Tchekhovskoy, A Narayan, R McKinney, JC AF Tchekhovskoy, Alexander Narayan, Ramesh McKinney, Jonathan C. TI BLACK HOLE SPIN AND THE RADIO LOUD/QUIET DICHOTOMY OF ACTIVE GALACTIC NUCLEI SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion; accretion disks; black hole physics; galaxies: jets; galaxies: nuclei; magnetohydrodynamics (MHD); quasars: general; relativistic processes ID BLANDFORD-ZNAJEK MECHANISM; GENERAL-RELATIVISTIC MAGNETOHYDRODYNAMICS; ACCRETION FLOWS; ELECTROMAGNETIC EXTRACTION; MAGNETIC ACCELERATION; ELLIPTIC GALAXIES; NUMERICAL SCHEME; JET POWER; ENERGY; SIMULATIONS AB Radio loud active galactic nuclei (AGNs) are on average 1000 times brighter in the radio band compared to radio quiet AGNs. We investigate whether this radio loud/quiet dichotomy can be due to differences in the spin of the central black holes (BHs) that power the radio-emitting jets. Using general relativistic magnetohydrodynamic simulations, we construct steady state axisymmetric numerical models for a wide range of BH spins (dimensionless spin parameter 0.1 <= a <= 0.9999) and a variety of jet geometries. We assume that the total magnetic flux through the BH horizon at radius r(H)(a) is held constant. If the BH is surrounded by a thin accretion disk, we find that the total BH power output depends approximately quadratically on the angular frequency of the hole, P alpha Omega(2)(H) alpha(a/r(H))(2). We conclude that, in this scenario, differences in the BH spin can produce power variations of only a few tens at most. However, if the disk is thick such that the jet subtends a narrow solid angle around the polar axis, then the power dependence becomes much steeper, P alpha Omega(4)(H) or even alpha Omega(6)(H). Power variations of 1000 are then possible for realistic BH spin distributions. We derive an analytic solution that accurately reproduces the steeper scaling of jet power with Omega(H) and we provide a numerical fitting formula that reproduces all our simulation results. We discuss other physical effects that might contribute to the observed radio loud/quiet dichotomy of AGNs. C1 [Tchekhovskoy, Alexander; Narayan, Ramesh] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. [McKinney, Jonathan C.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94309 USA. RP Tchekhovskoy, A (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St, Cambridge, MA 02138 USA. EM atchekho@cfa.harvard.edu; rnarayan@cfa.harvard.edu; jmckinne@stanford.edu OI Narayan, Ramesh/0000-0002-1919-2730 FU NASA [NNX08AH32G]; NSF [AST-0805832]; NASA Chandra Fellowship [PF7-80048] FX We thank Vasily Beskin and Serguei Komissarov for useful comments on the manuscript. This work was supported in part by NASA grant NNX08AH32G (A.T. and R.N.), NSF grant AST-0805832 (A.T. and R.N.), NASA Chandra Fellowship PF7-80048 (J.C.M.), and by NSF through TeraGrid resources (Catlett et al. 2007) provided by the Louisiana Optical Network Initiative (http://www.loni.org). NR 70 TC 171 Z9 171 U1 1 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 MAR 1 PY 2010 VL 711 IS 1 BP 50 EP 63 DI 10.1088/0004-637X/711/1/50 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 554EE UT WOS:000274417500005 ER PT J AU Landi, E Raymond, JC Miralles, MP Hara, H AF Landi, E. Raymond, J. C. Miralles, M. P. Hara, H. TI PHYSICAL CONDITIONS IN A CORONAL MASS EJECTION FROM HINODE, STEREO, AND SOHO OBSERVATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: activity; Sun: corona; Sun: coronal mass ejections (CMEs); Sun: UV radiation; techniques: spectroscopic ID SOLAR CORONA; IMAGING SPECTROMETER; DENSITY DIAGNOSTICS; ATOMIC DATABASE; EMISSION-LINES; FE XIII; ULTRAVIOLET; WAVELENGTHS; CALIBRATION; UVCS/SOHO AB In the present work, we analyze multiwavelength observations from Hinode, Solar and Heliospheric Observatory (SOHO), and STEREO of the early phases of a coronal mass ejection (CME). We use Hinode/EIS and SOHO/UVCS high-resolution spectra to measure the physical properties of the CME ejecta as a function of time at 1.1 and 1.9 solar radii. Hinode/XRT images are used in combination with EIS spectra to constrain the high temperature plasma properties of the ejecta. SECCHI/EUVI, SECCHI/COR 1, SOHO/EIT, and SOHO/LASCO images are used to measure the CME trajectory, velocity, and acceleration. The combination of measurements of plane of the sky velocities from two different directions allows us to determine the total velocity of the CME plasma up to 5 solar radii. Plasma properties, dynamical status, thermal structure, and brightness distributions are used to constrain the energy content of the CME plasma and to determine the heating rate. We find that the heating is larger than the kinetic energy, and compare it to theoretical predictions from models of CME plasma heating and acceleration. C1 [Landi, E.] USN, Res Lab, Washington, DC 20375 USA. [Raymond, J. C.; Miralles, M. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hara, H.] Natl Inst Nat Sci, Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. RP Landi, E (reprint author), USN, Res Lab, Washington, DC 20375 USA. RI Landi, Enrico/H-4493-2011 FU NASA [NNX09AB17G-R, NNX06AG95G]; [NNH06CD24C]; [NNG04ED07P]; [NNH09AL49I] FX The work of E.L. is supported by the NNH06CD24C, NNG04ED07P, NNH09AL49I and other NASA grants. J.R.'s work was supported by NASA grant NNX09AB17G-R to the Smithsonian Astrophysical Observatory. The work of M.P.M. is supported by NASA grant NNX06AG95G to the Smithsonian Astrophysical Observatory. The authors acknowledge the help of Drs. R. Colaninno and G. Stenborg on the use of STEREO data, and Dr. A. van Ballegooijen for helpful discussions. STEREO is a project of NASA, SOHO is a joint ESA/NASA project. Hinode is a Japanese mission built and launched by JAXA/ISAS, collaborating with NAOJ as a domestic partner, NASA (USA), and PPARC (UK) as international partners. We warmly thank the anonymous referee for his/her valuable comments and suggestions that helped us greatly improve the paper. NR 35 TC 42 Z9 43 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 MAR 1 PY 2010 VL 711 IS 1 BP 75 EP 98 DI 10.1088/0004-637X/711/1/75 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 554EE UT WOS:000274417500007 ER PT J AU Machalek, P Greene, T McCullough, PR Burrows, A Burke, CJ Hora, JL Johns-Krull, CM Deming, DL AF Machalek, Pavel Greene, Tom McCullough, Peter R. Burrows, Adam Burke, Christopher J. Hora, Joseph L. Johns-Krull, Christopher M. Deming, Drake L. TI THERMAL EMISSION AND TIDAL HEATING OF THE HEAVY AND ECCENTRIC PLANET XO-3b SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: eclipsing; infrared: stars; planetary systems; stars: individual (XO-3) ID EXTRASOLAR GIANT PLANETS; EXOPLANET HD 189733B; HOT JUPITERS; TEMPERATURE INVERSION; LIGHT CURVES; DAYSIDE SPECTRUM; SPIN-ORBIT; ATMOSPHERE; EVOLUTION; 209458B AB We determined the flux ratios of the heavy and eccentric planet XO-3b to its parent star in the four Infrared Array Camera bands of the Spitzer Space Telescope: 0.101% +/- 0.004% at 3.6 mu m; 0.143% +/- 0.006% at 4.5 mu m; 0.134% +/- 0.049% at 5.8 mu m; and 0.150% +/- 0.036% at 8.0 mu m. The flux ratios are within [-2.2, 0.3, -0.8, and -1.7]sigma of the model of XO-3b with a thermally inverted stratosphere in the 3.6 mu m, 4.5 mu m, 5.8 mu m, and 8.0 mu m channels, respectively. XO-3b has a high illumination from its parent star (F(p) similar to (1.9-4.2) x 10(9) erg cm(-2) s(-1)) and is thus expected to have a thermal inversion, which we indeed observe. When combined with existing data for other planets, the correlation between the presence of an atmospheric temperature inversion and the substellar flux is insufficient to explain why some high insolation planets like TrES-3 do not have stratospheric inversions and some low insolation planets like XO-1b do have inversions. Secondary factors such as sulfur chemistry, atmospheric metallicity, amounts of macroscopic mixing in the stratosphere, or even dynamical weather effects likely play a role. Using the secondary eclipse timing centroids, we determined the orbital eccentricity of XO-3b as e = 0.277 +/- 0.009. The model radius-age trajectories for XO-3b imply that at least some amount of tidal heating is required to inflate the radius of XO-3b, and the tidal heating parameter of the planet is constrained to Q(p) less than or similar to 10(6). C1 [Machalek, Pavel; Greene, Tom] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Machalek, Pavel] Bay Area Environm Res Inst, Sonoma, CA 95476 USA. [McCullough, Peter R.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Burrows, Adam] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Burke, Christopher J.; Hora, Joseph L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Johns-Krull, Christopher M.] Rice Univ, Dept Phys & Astron, Houston, TX 77005 USA. [Deming, Drake L.] NASA, Goddard Space Flight Ctr, Planetary Syst Lab, Greenbelt, MD 20771 USA. RP Machalek, P (reprint author), NASA, Ames Res Ctr, MS 245-6, Moffett Field, CA 94035 USA. EM pavel.machalek@nasa.gov OI Hora, Joseph/0000-0002-5599-4650 FU Spitzer Science Center [C4030]; NASA [NNX07AG80G]; JPL/Spitzer [1328092, 1348668, 1312647]; National Aeronautics and Space Administration; National Science Foundation FX The authors thank the anonymous referee for a speedy and thorough review, which has substantially improved the manuscript. The authors also acknowledge the use of publicly available routines by Eric Agol and Levenberg-Marquardt least-squares minimization routine MPFITFUN by Craig Markwardt. P.M. and P.R.M. were supported by the Spitzer Science Center grant C4030 to the Space Telescope Science Institute, and the Bay Area Environmental Research Institute. A.B. was supported in part by NASA grant NNX07AG80G. We also acknowledge support through JPL/Spitzer Agreements 1328092, 1348668, and 1312647. T.G. acknowledges funding by NASA Ames Research Center to the Ames Center for Exoplanet Studies in support of this work. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. This publication also 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 57 TC 16 Z9 16 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 MAR 1 PY 2010 VL 711 IS 1 BP 111 EP 118 DI 10.1088/0004-637X/711/1/111 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 554EE UT WOS:000274417500009 ER PT J AU van Ballegooijen, AA Cranmer, SR AF van Ballegooijen, A. A. Cranmer, S. R. TI TANGLED MAGNETIC FIELDS IN SOLAR PROMINENCES SO ASTROPHYSICAL JOURNAL LA English DT Article DE magnetic fields; magnetohydrodynamics (MHD); Sun: corona; Sun: filaments; prominences ID TWISTED FLUX-TUBE; QUIESCENT PROMINENCES; FINE-STRUCTURE; FILAMENTS; THREADS; WAVES; CONDENSATION; EVOLUTION; TOPOLOGY; DYNAMICS AB Solar prominences are an important tool for studying the structure and evolution of the coronal magnetic field. Here we consider so-called hedgerow prominences, which consist of thin vertical threads. We explore the possibility that such prominences are supported by tangled magnetic fields. A variety of different approaches are used. First, the dynamics of plasma within a tangled field is considered. We find that the contorted shape of the flux tubes significantly reduces the flow velocity compared to the supersonic free fall that would occur in a straight vertical tube. Second, linear force-free models of tangled fields are developed, and the elastic response of such fields to gravitational forces is considered. We demonstrate that the prominence plasma can be supported by the magnetic pressure of a tangled field that pervades not only the observed dense threads but also their local surroundings. Tangled fields with field strengths of about 10 G are able to support prominence threads with observed hydrogen density of the order of 10(11) cm(-3). Finally, we suggest that the observed vertical threads are the result of Rayleigh-Taylor instability. Simulations of the density distribution within a prominence thread indicate that the peak density is much larger than the average density. We conclude that tangled fields provide a viable mechanism for magnetic support of hedgerow prominences. C1 [van Ballegooijen, A. A.; Cranmer, S. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP van Ballegooijen, AA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St MS-15, Cambridge, MA 02138 USA. OI van Ballegooijen, Adriaan/0000-0002-5622-3540 NR 75 TC 39 Z9 39 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 MAR 1 PY 2010 VL 711 IS 1 BP 164 EP 178 DI 10.1088/0004-637X/711/1/164 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 554EE UT WOS:000274417500015 ER PT J AU Just, DW Zaritsky, D Sand, DJ Desai, V Rudnick, G AF Just, Dennis W. Zaritsky, Dennis Sand, David J. Desai, Vandana Rudnick, Gregory TI THE ENVIRONMENTAL DEPENDENCE OF THE EVOLVING S0 FRACTION SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: general; galaxies: evolution; galaxies: groups: general ID MORPHOLOGY-DENSITY RELATION; DISTANT CLUSTER SURVEY; EARLY-TYPE GALAXIES; HUBBLE-SPACE-TELESCOPE; MU-M SOURCES; RICH CLUSTERS; VELOCITY DISPERSIONS; DISK GALAXIES; SURVEY EDISCS; EVOLUTION AB We re-investigate the dramatic rise in the S0 fraction, f(S0), within clusters since z similar to 0.5. In particular, we focus on the role of the global galaxy environment on fS0 by compiling, either from our own observations or the literature, robust line-of-sight velocity dispersions, sigma's, for a sample of galaxy groups and clusters at 0.1 < z < 0.8 that have uniformly determined, published morphological fractions. We find that the trend of f(S0) with redshift is twice as strong for sigma < 750 km s(-1) groups/poor clusters than for higher-sigma, rich clusters. From this result, we infer that over this redshift range galaxy-galaxy interactions, which are more effective in lower-sigma environments, are more responsible for transforming spiral galaxies into S0's than galaxy-environment processes, which are more effective in higher-sigma environments. The rapid, recent growth of the S0 population in groups and poor clusters implies that large numbers of progenitors exist in low-sigma systems at modest redshifts (similar to 0.5), where morphologies and internal kinematics are within the measurement range of current technology. C1 [Just, Dennis W.; Zaritsky, Dennis; Sand, David J.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Sand, David J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Desai, Vandana] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Desai, Vandana] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Rudnick, Gregory] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA. RP Just, DW (reprint author), Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA. OI Rudnick, Gregory/0000-0001-5851-1856 FU NASA LTSA [NNG05GE82G]; NASA XMM [NNX06AG39A, NNX06AE41G]; NASA Spitzer [1344985] FX We thank the anonymous referee for insightful comments that improved the content and presentation of this paper. D.J. thanks Michael Cooper for useful conversations and Daniel Christlein for helping with the Magellan observations. D.Z. acknowledges financial support for this work from NASA LTSA award NNG05GE82G, NASA XMM grants NNX06AG39A, NNX06AE41G, and NASA Spitzer grant 1344985. D.Z. also thanks the NYU Physics Department and CCPP for their hospitality during his visit. NR 53 TC 38 Z9 39 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 MAR 1 PY 2010 VL 711 IS 1 BP 192 EP 200 DI 10.1088/0004-637X/711/1/192 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 554EE UT WOS:000274417500018 ER PT J AU Fressin, F Knutson, HA Charbonneau, D O'Donovan, FT Burrows, A Deming, D Mandushev, G Spiegel, D AF Fressin, Francois Knutson, Heather A. Charbonneau, David O'Donovan, Francis T. Burrows, Adam Deming, Drake Mandushev, Georgi Spiegel, David TI THE BROADBAND INFRARED EMISSION SPECTRUM OF THE EXOPLANET TrES-3 SO ASTROPHYSICAL JOURNAL LA English DT Article DE eclipses; infrared: stars; planetary systems; stars: individual (TrES-3); techniques: photometric ID EXTRASOLAR GIANT PLANETS; SPITZER-SPACE-TELESCOPE; LIGHT-CURVE PROJECT; THERMAL EMISSION; HD 189733B; HOT JUPITERS; THEORETICAL SPECTRA; ARRAY CAMERA; ATMOSPHERES; TRANSIT AB We use the Spitzer Space Telescope to estimate the dayside thermal emission of the exoplanet TrES-3 integrated in the 3.6, 4.5, 5.8, and 8.0 mu m bandpasses of the Infrared Array Camera (IRAC) instrument. We observe two secondary eclipses and find relative eclipse depths of 0.00346 +/- 0.00035, 0.00372 +/- 0.00054, 0.00449 +/- 0.00097, and 0.00475 +/- 0.00046, respectively, in the four IRAC bandpasses. We combine our results with the earlier K-band measurement of De Mooij et al., and compare them with models of the planetary emission. We find that the planet does not require the presence of an inversion layer in the high atmosphere. This is the first very strongly irradiated planet that does not have a temperature inversion, which indicates that stellar or planetary characteristics other than temperature have an important impact on temperature inversion. De Mooij & Snellen also detected a possible slight offset in the timing of the secondary eclipse in the K band. However, based on our four Spitzer channels, we place a 3 sigma upper limit of vertical bar e cos(omega)vertical bar < 0.0056, where e is the planet's orbital eccentricity and omega is the longitude of the periastron. This result strongly indicates that the orbit is circular, as expected from tidal circularization theory. C1 [Fressin, Francois; Knutson, Heather A.; Charbonneau, David; O'Donovan, Francis T.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Burrows, Adam; Spiegel, David] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Deming, Drake] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Mandushev, Georgi] Lowell Observ, Flagstaff, AZ 86001 USA. RP Fressin, F (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM ffressin@cfa.harvard.edu OI Charbonneau, David/0000-0002-9003-484X FU NASA 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 to NASA. NR 49 TC 46 Z9 46 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 MAR 1 PY 2010 VL 711 IS 1 BP 374 EP 379 DI 10.1088/0004-637X/711/1/374 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 554EE UT WOS:000274417500032 ER PT J AU Cotton, WD Ragland, S Pluzhnik, EA Danchi, WC Traub, WA Willson, LA Lacasse, MG AF Cotton, W. D. Ragland, S. Pluzhnik, E. A. Danchi, W. C. Traub, W. A. Willson, L. A. Lacasse, M. G. TI SiO MASERS IN ASYMMETRIC MIRAS. III. IK TAURI SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE radio lines: stars; stars: AGB and post-AGB; stars: atmospheres ID PERIOD VARIABLE-STARS; GIANT BRANCH STARS; MASS-LOSS; DUST SHELLS; R-AQUARII; STELLAR POPULATIONS; RADIO PHOTOSPHERES; AGB STARS; TX CAM; EMISSION AB This is the third paper in a series of multi-epoch observations at 7 mm wavelength of the SiO masers in several asymptotic giant branch stars from a sample of Mira variable stars showing evidence of asymmetric structure in the infrared. These stars have been observed interferometrically in the infrared by Infrared Optical Telescope Array and with Very Long Baseline Array measurements of the SiO masers. In this paper, we present the observations of IK Tauri (IK Tau). There is a persistent elliptical distribution of the masers around the star similar to 40 x similar to 30 mas in size with a major axis at position angle similar to 30 degrees. The SiO masers in the circumstellar envelope exhibit large-scale systematic motions which reverse direction on timescales of a decade, roughly the interval between the ejections of dust shells. The orientations on the sky of the apparent rotation-like bulk motion and of the major axis of the maser ellipse differ by 37 degrees (2.5 sigma) making any relationship uncertain. The systemic velocity of IK Tau is estimated to be 33.3 +/- 1.0 km s(-1). A comparison is made with the model calculations of Gray et al. which predict some but not all observed features. C1 [Cotton, W. D.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Ragland, S.] WM Keck Observ, Kamuela, HI 96743 USA. [Pluzhnik, E. A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Danchi, W. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Traub, W. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Willson, L. A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50014 USA. [Lacasse, M. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Cotton, WD (reprint author), Natl Radio Astron Observ, 520 Edgemont Rd, Charlottesville, VA 22903 USA. EM bcotton@nrao.edu FU NSF [AST-0456047] FX We acknowledge support from NSF of the IOTA observations through grant AST-0456047. We thank the anonymous referee for suggestions leading to the improvement of this paper. NR 34 TC 5 Z9 5 U1 0 U2 1 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 MAR PY 2010 VL 187 IS 1 BP 107 EP 118 DI 10.1088/0067-0049/187/1/107 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 564CZ UT WOS:000275192200003 ER PT J AU Gallimore, JF Yzaguirre, A Jakoboski, J Stevenosky, MJ Axon, DJ Baum, SA Buchanan, CL Elitzur, M Elvis, M O'Dea, CP Robinson, A AF Gallimore, J. F. Yzaguirre, A. Jakoboski, J. Stevenosky, M. J. Axon, D. J. Baum, S. A. Buchanan, C. L. Elitzur, M. Elvis, M. O'Dea, C. P. Robinson, A. TI INFRARED SPECTRAL ENERGY DISTRIBUTIONS OF SEYFERT GALAXIES: SPITZER SPACE TELESCOPE OBSERVATIONS OF THE 12 mu m SAMPLE OF ACTIVE GALAXIES SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE galaxies: active; galaxies: Seyfert; galaxies: spiral; infrared: galaxies ID RESOLUTION RADIO OBSERVATIONS; MULTIBAND IMAGING PHOTOMETER; EXTENDED 12-MU-M SAMPLE; STAR-FORMING GALAXIES; AGN DUSTY TORI; GALACTIC NUCLEI; X-RAY; OPTICAL SPECTROSCOPY; STARBURST GALAXIES; ABSOLUTE CALIBRATION AB The mid-infrared spectral energy distributions (SEDs) of 83 active galaxies, mostly Seyfert galaxies, selected from the extended 12 mu m sample are presented. The data were collected using all three instruments, Infrared Array Camera (IRAC), Infrared Spectrograph (IRS), and Multiband Imaging Photometer for Spitzer (MIPS), aboard the Spitzer Space Telescope. The IRS data were obtained in spectral mapping mode, and the photometric data from IRAC and IRS were extracted from matched, 20 '' diameter circular apertures. The MIPS data were obtained in SED mode, providing very low-resolution spectroscopy (R similar to 20) between similar to 55 and 90 mu m in a larger, 20 '' x 30 '' synthetic aperture. We further present the data from a spectral decomposition of the SEDs, including equivalent widths and fluxes of key emission lines; silicate 10 mu m and 18 mu m emission and absorption strengths; IRAC magnitudes; and mid-far-infrared spectral indices. Finally, we examine the SEDs averaged within optical classifications of activity. We find that the infrared SEDs of Seyfert 1s and Seyfert 2s with hidden broad line regions (HBLRs, as revealed by spectropolarimetry or other technique) are qualitatively similar, except that Seyfert 1s show silicate emission and HBLR Seyfert 2s show silicate absorption. The infrared SEDs of other classes within the 12 mu m sample, including Seyfert 1.8-1.9, non-HBLR Seyfert 2 (not yet shown to hide a type 1 nucleus), LINER, and H Pi galaxies, appear to be dominated by star formation, as evidenced by blue IRAC colors, strong polycyclic aromatic hydrocarbon emission, and strong far-infrared continuum emission, measured relative to mid-infrared continuum emission. C1 [Gallimore, J. F.; Yzaguirre, A.; Jakoboski, J.; Stevenosky, M. J.] Bucknell Univ, Dept Phys & Astron, Lewisburg, PA 17837 USA. [Yzaguirre, A.] Calif State Univ Fullerton, Dept Phys, Fullerton, CA 92834 USA. [Jakoboski, J.] Jet Prop Lab, Pasadena, CA 91190 USA. [Stevenosky, M. J.] Franklin Pierce Law Ctr, Concord, NH 03301 USA. [Axon, D. J.; O'Dea, C. P.; Robinson, A.] Rochester Inst Technol, Dept Phys, Rochester, NY 14623 USA. [Axon, D. J.] Univ Sussex, Sch Math & Phys Sci, Brighton BN1 9QH, E Sussex, England. [Baum, S. A.] Rochester Inst Technol, Chester F Carlson Ctr Imaging Sci, Rochester, NY 14623 USA. [Buchanan, C. L.] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia. [Elitzur, M.] Univ Kentucky, Dept Phys & Astron, Lexington, KY 40506 USA. [Elvis, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gallimore, JF (reprint author), NRAO, 520 Edgemont Rd, Charlottesville, VA 22903 USA. FU National Science Foundation REU Program [0097424] FX The authors gratefully acknowledge the anonymous referee for a careful reading of the manuscript and very helpful comments. 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 at Bucknell University, the University of Rochester, and the Rochester Institute of Technology was provided by NASA through an award issued by JPL/ Caltech. A. Yzaguirre received support from the National Science Foundation REU Program, grant 0097424. J. Jakoboski received support as a Bucknell Presidential Fellow. NR 119 TC 35 Z9 35 U1 0 U2 1 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 MAR PY 2010 VL 187 IS 1 BP 172 EP 211 DI 10.1088/0067-0049/187/1/172 PG 40 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 564CZ UT WOS:000275192200007 ER PT J AU Ryder, TB Tori, WP Blake, JG Loiselle, BA Parker, PG AF Ryder, T. B. Tori, W. P. Blake, J. G. Loiselle, B. A. Parker, P. G. TI Mate choice for genetic quality: a test of the heterozygosity and compatibility hypotheses in a lek-breeding bird SO BEHAVIORAL ECOLOGY LA English DT Article DE compatibility; genetic quality; good-genes; heterozygosity; lekking; mate choice; Pipra filicauda; territory acquisition ID SPARROWS MELOSPIZA-MELODIA; MICROSATELLITE DNA MARKERS; WIRE-TAILED MANAKIN; INBREEDING DEPRESSION; SEXUAL SELECTION; MULTILOCUS HETEROZYGOSITY; PARENTAL RELATEDNESS; NATURAL-POPULATIONS; EASTERN ECUADOR; MATING SUCCESS AB Understanding female mate choice in nonresource-based mating systems, where females appear to express strong preferences despite receiving no direct benefits from mate choice, remain a challenge to behavioral ecology. Brown (Brown JL. 1997. A theory of mate choice based on heterozygosity. Behav Ecol. 8:60-65) proposed the "good-genes-as-heterozygosity" hypothesis, which sought to establish the genetic nature of male quality. Despite recent attention, few studies have examined how multiple components of genetic quality influence mate choice in a highly promiscuous mating system such as that of the lekking wire-tailed manakin (Pipra filicauda, Aves: Pipridae). Based on a 4-year study in the Amazon basin of Ecuador we ask whether female wire-tailed manakins use heterozygosity and/or dissimilarity (relatedness) as mate-choice criteria, and if heterozygosity influences the ontogeny of male social status. Our data show that females select more heterozygous males as their partners. Females do not, however, appear to select mates based on their genetic dissimilarity as mated pairs were more related than expected under random mating. Heterozygosity of territorial males was correlated with 2 male morphological traits (wing and tarsus length), which suggests that females may assess male genetic quality via phenotypic correlates. In addition, our data show that heterozygosity was related to male social rise (territory acquisition) and suggests that heterozygosity may act as a filter of male reproductive potential. Lastly, we find no support for indirect benefits (i.e., increased offspring genetic quality) obtained via female choice for heterozygous males. C1 Univ Missouri, Dept Biol, St Louis, MO 63121 USA. Univ Missouri, Whitney R Harris World Ecol Ctr, St Louis, MO 63121 USA. RP Ryder, TB (reprint author), Natl Zool Pk, Smithsonian Migratory Bird Ctr, POB 37012 MRC 5503, Washington, DC 20013 USA. EM pipridae@gmail.com RI Loiselle, Bette/O-7106-2016 OI Loiselle, Bette/0000-0003-1434-4173 FU International Center for Tropical Ecology; Association of Field Ornithologists'; National Geographic Society [7113-01]; National Science Foundation [IBN 0235141, IOB 0508189, OISE 0513341] FX International Center for Tropical Ecology, the Association of Field Ornithologists' Alexander Bergstrom Award; National Geographic Society (7113-01); National Science Foundation (IBN 0235141, IOB 0508189, OISE 0513341).; We thank the numerous people who assisted in collecting field data for this project: F. Narvaez, S. Frey, J. Klavins, M. Euaparadorn, J. D. Wolfe, and M. Stake. Thanks to R. Duraes and J. Hidalgo for their field and emotional support. Previous versions of the manuscript were greatly improved by B. Kempenaers and several anonymous reviewers. Special thanks to the Feder's for financial support. We are indebted K. Halbert and C. Rettke for their knowledge and help in the laboratory. Special thanks to D., and C. Romo, K. Swing, J. Guerra and all the Tiputini Biodiversity Station staff for logistical and field support. IACUC protocol number 5-12-20. This research was conducted in accordance with permit number 13-IC-FAU-DFN, Ministerio de Ambiente, Distrito Forestal Napo, Tena, Ecuador. We thank them for allowing us to conduct our research at the Tiputini Biodiversity Station. NR 75 TC 17 Z9 17 U1 2 U2 42 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1045-2249 J9 BEHAV ECOL JI Behav. Ecol. PD MAR-APR PY 2010 VL 21 IS 2 BP 203 EP 210 DI 10.1093/beheco/arp176 PG 8 WC Behavioral Sciences; Biology; Ecology; Zoology SC Behavioral Sciences; Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Zoology GA 555BZ UT WOS:000274483400001 ER PT J AU Hultgren, KM Stachowicz, JJ AF Hultgren, Kristin M. Stachowicz, John J. TI Size-related habitat shifts facilitated by positive preference induction in a marine kelp crab SO BEHAVIORAL ECOLOGY LA English DT Article DE habitat selection; kelp forest; ontogenetic habitat shift; positive preference induction; Pugettia producta; size ID CARIBBEAN SPINY LOBSTERS; PREDATION RISK; PHYTOPHAGOUS INSECTS; HOST SPECIFICITY; SEA-URCHIN; SELECTION; HERBIVORES; EXPERIENCE; CAMOUFLAGE; BEHAVIOR AB Individual variation in habitat use has important ecological and evolutionary consequences. Here, we combine developmental and functional approaches to study habitat use in Pugettia producta, a marine crab that sequesters pigments from the algae it inhabits and consumes to camouflage with different colored algal habitats. Pugettia from different habitats differ in size and color; individuals living in red intertidal algae are small and red, whereas crabs in amber-colored kelp forests are larger and more amber. We examine the developmental causes (effects of size and experience) and the functional consequences (growth and mortality rates) of size-specific habitat use in Pugettia. We demonstrate that positive preference induction may be a mechanism facilitating size-specific habitat use: prior feeding experience with kelp (in the field or laboratory) increases habitat preferences for kelp but only for larger crabs. Habitat use also has important fitness consequences; small red crabs grow equally fast on both kelp and red algae but suffer much higher mortality in kelp; large red crabs grow faster on kelp diets relative to red algae but experience only marginally higher mortality in kelp. Thus, habitat-specific mortality rates may explain the use of intertidal red algal habitats by small crabs, whereas reduced growth of large crabs on red algae may help trigger shifts to subtidal kelp habitats. Size-specific functional consequences of habitat use may select for developmental processes-such as positive preference induction-that facilitate shifts in habitat use in Pugettia and other phenotypically plastic organisms that shift habitats through ontogeny. C1 [Hultgren, Kristin M.; Stachowicz, John J.] Univ Calif Davis, Dept Ecol & Evolut, Davis, CA 95616 USA. RP Hultgren, KM (reprint author), Smithsonian Inst, Natl Museum Nat Hist, MRC 163,POB 37012, Washington, DC 20013 USA. EM hultgrenk@si.edu RI Hultgren, Kristin/F-6862-2011 FU Center for Population Biology (UC Davis); National Science Foundation; National Science Foundation [OCE 03-51778] FX Center for Population Biology (UC Davis); and National Science Foundation Predoctoral fellowship (to K.M.H.); and National Science Foundation (OCE 03-51778 to J.J.S.). NR 54 TC 13 Z9 14 U1 4 U2 29 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1045-2249 J9 BEHAV ECOL JI Behav. Ecol. PD MAR-APR PY 2010 VL 21 IS 2 BP 329 EP 336 DI 10.1093/beheco/arp192 PG 8 WC Behavioral Sciences; Biology; Ecology; Zoology SC Behavioral Sciences; Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Zoology GA 555BZ UT WOS:000274483400017 ER PT J AU Spiering, PA Somers, MJ Maldonado, JE Wildt, DE Gunther, MS AF Spiering, Penny A. Somers, Michael J. Maldonado, Jesus E. Wildt, David E. Gunther, Micaela Szykman TI Reproductive sharing and proximate factors mediating cooperative breeding in the African wild dog (Lycaon pictus) SO BEHAVIORAL ECOLOGY AND SOCIOBIOLOGY LA English DT Article DE Dominance; Lycaon pictus; Multiple parentage; Proximate mechanisms; Reproductive sharing; Subordinate breeding ID HETEROCEPHALUS-GLABER; NATURAL-POPULATIONS; GENETIC-ANALYSIS; SOCIAL-CONTROL; MOLE-RATS; SUPPRESSION; COMPETITION; MECHANISMS; LIKELIHOOD; TOLERANCE AB Although dominant African wild dogs (Lycaon pictus) are generally believed to be the sole breeders within a pack, earlier behavioral and endocrine data suggest that reproduction could be shared with subordinates. We performed an extensive behavioral, demographic, and genetic evaluation of a wild dog population in South Africa to examine the level of such sharing and the proximate mechanisms influencing reproductive contributions of each sex. While a majority of pups were born to dominants because of a lack of subordinate potential breeders, we discovered a substantial portion of reproductive sharing between dominants and subordinates. Compared with alpha females that mated annually, subordinate beta females bred in 54.5% of years whereas thetas never bred. The three top-ranking males all sired pups (56.0%, 32.0%, and 12.0%, respectively) when three or more adult males were present. With only two pack males, alpha and beta individuals shared reproduction nearly equally (55.2% and 44.8%, respectively), and litters of mixed paternity were discovered on eight of 15 (53.3%) occasions. A skewed adult sex-ratio and frequent alpha mortalities for females and behavioral aggression in males allowed most individuals to attain dominant status in their lifetime, creating a constantly shifting social hierarchy. Genetic parentage results corresponded to reported hormone profiles, suggesting physiological suppression in some lower-ranked individuals of both sexes. Thus, a combination of demographic, behavioral, and hormonal proximate factors mediates reproductive partitioning in wild dogs. We conclude that reproductive sharing can be significant in this species, especially for males that have less robust suppressive mechanisms than females. C1 [Spiering, Penny A.; Wildt, David E.; Gunther, Micaela Szykman] Smithsonian Inst, Conservat & Res Ctr, Ctr Species Survival, Front Royal, VA 22630 USA. [Spiering, Penny A.; Maldonado, Jesus E.] Smithsonian Inst, Ctr Conservat & Evolutionary Genet, Washington, DC 20008 USA. [Spiering, Penny A.; Somers, Michael J.] Univ Pretoria, Ctr Wildlife Management, ZA-0002 Pretoria, South Africa. [Somers, Michael J.] Univ Pretoria, Ctr Invas Biol, ZA-0002 Pretoria, South Africa. [Gunther, Micaela Szykman] Humboldt State Univ, Dept Wildlife, Arcata, CA 95521 USA. RP Spiering, PA (reprint author), Smithsonian Inst, Conservat & Res Ctr, Ctr Species Survival, Natl Zool Pk, Front Royal, VA 22630 USA. EM SpieringP@si.edu RI Somers, Michael/A-1523-2008; OI Szykman Gunther, Micaela/0000-0002-7822-8094; /0000-0002-5836-8823 FU Smithsonian Institution Undersecretary for Science Endowment, University of Pretoria; Rotterdam Zoo Thandiza Fund, Humboldt State University; Conservation Endowment Fund of the Association of Zoos and Aquariums; Disney Wildlife Conservation Fund; Knowsley Safari Park; DST-NRF Centre of Excellence for Invasion Biology; Khaki Fever Work Wear; Pittsburgh Zoo Conservation Fund; Morris Animal Foundation FX We thank Ezemvelo KwaZulu-Natal Wildlife, especially the management teams at Hluhluwe-Imfolozi Park and the uMkhuze section of iSimangaliso Wetland Park. We also appreciate the assistance of Thanda Private Game Reserve and their wildlife management team. We are grateful to Rob Fleischer, Emily Latch, Sarah Haas, Kalon Armstrong, and Nancy Rotzel of the Smithsonian's Center for Conservation and Evolutionary Genetics for laboratory support and assistance with protocols and procedures. Sarah Arnoff, Jan Graf, Gabriella Flacke, Mariana Venter, Carla Naude-Graaff, Sboniso (Zama) Zwane, and Chris Kelly provided invaluable assistance in monitoring and sample collection in the field. This research was supported by funding from the Smithsonian Institution Undersecretary for Science Endowment, University of Pretoria, Rotterdam Zoo Thandiza Fund, Humboldt State University, Conservation Endowment Fund of the Association of Zoos and Aquariums, Disney Wildlife Conservation Fund, Knowsley Safari Park, DST-NRF Centre of Excellence for Invasion Biology, Khaki Fever Work Wear, Pittsburgh Zoo Conservation Fund, and the Morris Animal Foundation. International travel was generously provided by British Airways. NR 44 TC 15 Z9 15 U1 7 U2 55 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0340-5443 J9 BEHAV ECOL SOCIOBIOL JI Behav. Ecol. Sociobiol. PD MAR PY 2010 VL 64 IS 4 BP 583 EP 592 DI 10.1007/s00265-009-0875-6 PG 10 WC Behavioral Sciences; Ecology; Zoology SC Behavioral Sciences; Environmental Sciences & Ecology; Zoology GA 554KJ UT WOS:000274433600009 ER PT J AU Estrada-Villegas, S Meyer, CFJ Kalko, EKV AF Estrada-Villegas, Sergio Meyer, Christoph F. J. Kalko, Elisabeth K. V. TI Effects of tropical forest fragmentation on aerial insectivorous bats in a land-bridge island system SO BIOLOGICAL CONSERVATION LA English DT Article DE Isolation; Chiroptera; Acoustic monitoring; Bat detector; Echolocation; Neotropics ID NEOTROPICAL BATS; ECHOLOCATION CALLS; PHYLLOSTOMID BATS; SPECIES RICHNESS; HABITAT FRAGMENTATION; ATLANTIC FOREST; TREE DIVERSITY; BULLDOG BAT; LANDSCAPE; INVENTORY AB Habitat fragmentation causes drastic changes in the biota and it is crucial to understand these modifications to mitigate its consequences. While studies on Neotropical bats have mainly targeted phyllostomid bats, impacts of fragmentation on the equally important aerial insectivores remain largely unexplored. We studied species richness, composition, count abundance and feeding activity of aerial insectivorous bats in a system of land-bridge islands in Panama with acoustic sampling. We predicted negative effects of fragmentation on forest species while bats foraging in open space should remain essentially unaffected. Rarefaction analyses indicated higher species richness for islands than mainland sites. For forest species, multivariate analyses suggested compositional differences between sites due to effects of isolation, area and vegetation structure. Contrary to our expectations, count abundance of forest species was similar across site categories. Feeding activity, however, was curtailed on far islands compared to near islands. As expected, bats hunting in open space did not reveal negative responses to fragmentation. Interestingly, they even displayed higher abundance counts on far and small islands. On the species level, two forest bats responded negatively to size reduction or site isolation, respectively, while a forest bat and a bat hunting in open space were more abundant on islands, irrespectively of island isolation or size. Our findings suggest that small forest remnants are of considerable conservation value as many aerial insectivores intensively use them. Hence high conservation priority should be given to retain or re-establish a high degree of forest integrity and low levels of isolation. (C) 2009 Elsevier Ltd. All rights reserved. C1 [Estrada-Villegas, Sergio] Univ Andes, Lab Ecol Vertebrados, Dept Ciencias Biol, Bogota, DC, Colombia. [Meyer, Christoph F. J.; Kalko, Elisabeth K. V.] Univ Ulm, Inst Expt Ecol, D-89069 Ulm, Germany. [Kalko, Elisabeth K. V.] Smithsonian Trop Res Inst, Balboa, Panama. RP Estrada-Villegas, S (reprint author), McGill Univ, Dept Biol, Large Scale Ecol Lab, Stewart Biol Bldg,1205 Docteur Penfield, Montreal, PQ H3A 1B1, Canada. EM sergio.estradavillegas@mail.mcgill.ca; cmeyer@fc.ul.pt; elisabeth.kalko@uni-ulm.de RI Meyer, Christoph/A-4363-2012 OI Meyer, Christoph/0000-0001-9958-8913 FU German Science Foundation FX We thank the Smithsonian Tropical Research Institute for logistical support, and the Autoridad del Canal de Panama (ACP) for permission to work on the islands in Gatun Lake. S.E.-V. wants to thank Laura Jara, Christian Ziegler, Janeene Touchton, Sara Pinzon, Sharon Shattuck. Daniel Obando and Kelsey Ellis for help during data collection. We are truly grateful to Kirsten Jung for her assistance during data analysis, comments on species identification and sharing unpublished data. We are thankful to Brock Fenton and J. Touchton and two anonymous reviewers for helpful comments on earlier drafts of the manuscript. Financial support was provided by a grant from the German Science Foundation (DFG) to S.E.V., C.M. and EX NR 74 TC 21 Z9 22 U1 0 U2 55 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 MAR PY 2010 VL 143 IS 3 BP 597 EP 608 DI 10.1016/j.biocon.2009.11.009 PG 12 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 573WQ UT WOS:000275946400009 ER PT J AU Collin, R Salazar, MZ AF Collin, Rachel Salazar, Maricela Z. TI Temperature-mediated plasticity and genetic differentiation in egg size and hatching size among populations of Crepidula (Gastropoda: Calyptraeidae) SO BIOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE evolution of development; maternal effects; offspring size; phylogeography ID SPAWNING MARINE-INVERTEBRATES; LIFE-HISTORY; LATITUDINAL VARIATION; ENERGETIC CONTENT; MATERNAL SIZE; CAPITELLA SP; CELL-SIZE; LARVAE; QUALITY; PROSOBRANCHIA AB Offspring size is a key characteristic in life histories, reflecting maternal investment per offspring and, in marine invertebrates, being linked to mode of development. Few studies have focused explicitly on intraspecific variation and plasticity in developmental characteristics such as egg size and hatching size in marine invertebrates. We measured over 1000 eggs and hatchlings of the marine gastropods Crepidula atrasolea and Crepidula ustulatulina from two sites in Florida. A common-garden experiment showed that egg size and hatching size were larger at 23 degrees C than at 28 degrees C in both species. In C. ustulatulina, the species with significant genetic population structure in cytochrome oxidase I (COI), there was a significant effect of population: Eggs and hatchlings from the Atlantic population were smaller than those from the Gulf. The two populations also differed significantly in hatchling shape. Population effects were not significant in C. atrasolea, the species with little genetic population structure in COI, and were apparent through their marginal interaction with temperature. In both species, 60-65% of the variation in egg size and hatching size was a result of variation among females and, in both species, the population from the Atlantic coast showed greater temperature-mediated plasticity than the population from the Gulf. These results demonstrate that genetic differentiation among populations, plastic responses to variation in environmental temperature, and differences between females all contribute significantly to intraspecific variation in egg size and hatching size. (C) 2010 The Linnean Society of London, Biological Journal of the Linnean Society, 2010, 99, 489-499. C1 [Collin, Rachel; Salazar, Maricela Z.] Smithsonian Trop Res Inst, Balboa, Panama. RP Collin, R (reprint author), Smithsonian Trop Res Inst, MRC 0580-08,Unit 9100 Box 0948, APO, AA 34002 USA. EM collinr@si.edu RI Collin, Rachel/G-2001-2010; OI Collin, Rachel/0000-0001-5103-4460 FU Smithsonian Institution; Marine Science Network FX We thank S. Reed (Smithsonian Marine Station in Fort Pierce) and L. K. Dixon (Mote Marine Laboratory) for providing long-term field temperature data. The Smithsonian Institution's Scholarly Studies program and Marine Science Network provided financial support for this project. M. F. Vinasco, R. Rissanen, M. Venegas, and J. Sartu assisted in animal maintenance and photography and D. Ingrao provided assistance in the field. R. Robertson, H. Lessios, K. McDonald, and J. McAlister commented on previous versions of this manuscript. This is SMS publication #803. NR 54 TC 18 Z9 18 U1 0 U2 14 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0024-4066 J9 BIOL J LINN SOC JI Biol. J. Linnean Soc. PD MAR PY 2010 VL 99 IS 3 BP 489 EP 499 PG 11 WC Evolutionary Biology SC Evolutionary Biology GA 552QD UT WOS:000274307400002 ER PT J AU Sayer, EJ Sutcliffe, LME Ross, RIC Tanner, EVJ AF Sayer, Emma J. Sutcliffe, Laura M. E. Ross, Rebecca I. C. Tanner, Edmund V. J. TI Arthropod Abundance and Diversity in a Lowland Tropical Forest Floor in Panama: The Role of Habitat Space vs. Nutrient Concentrations SO BIOTROPICA LA English DT Article DE arthropod community composition; Barro Colorado Nature Monument; habitat quality; litter addition; litter fauna; Oe horizon; Oi horizon ID HIGHER-TAXON RICHNESS; LITTER DECOMPOSITION; LEAF-LITTER; SPECIES RICHNESS; RAIN-FOREST; PUERTO-RICO; BOTTOM-UP; SOIL; QUALITY; FAUNA AB Tropical forest floor characteristics such as depth and nutrient concentrations are highly heterogeneous even over small spatial scales and it is unclear how these differences contribute to patchiness in forest floor arthropod abundance and diversity. In a lowland tropical forest in Panama we experimentally increased litter standing crop by removing litter from five plots (L-) and adding it to five other plots (L+); we had five control plots. After 32 mo of treatments we investigated how arthropod abundance and diversity were related to differences in forest floor physical (mass, depth, water content) and chemical properties (pH, nutrient concentrations). Forest floor mass and total arthropod abundance were greater in L+ plots compared with controls. There were no treatment differences in nutrient concentrations, pH or water content of the organic horizons. Over all plots, the mass of the fermentation horizon (Oe) was greater than the litter horizon (Oi); arthropod diversity and biomass were also greater in the Oe horizon but nutrient concentrations tended to be higher in the Oi horizon. Arthropod abundance was best explained by forest floor mass, while arthropod diversity was best explained by phosphorus, calcium and sodium concentrations in the Oi horizon and by phosphorus concentrations in the Oe horizon. Differences in arthropod community composition between treatments and horizons correlated with phosphorus concentration and dry mass of the forest floor. We conclude that at a local scale, arthropod abundance is related to forest floor mass ( habitat space), while arthropod diversity is related to forest floor nutrient concentrations (habitat quality). C1 [Sayer, Emma J.; Sutcliffe, Laura M. E.; Ross, Rebecca I. C.; Tanner, Edmund V. J.] Dept Plant Sci, Cambridge CB2 3EA, England. [Sayer, Emma J.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Sayer, EJ (reprint author), Dept Plant Sci, Downing St, Cambridge CB2 3EA, England. EM ejs44@cam.ac.uk RI Sayer, Emma/B-2514-2010 OI Sayer, Emma/0000-0002-3322-4487 FU Mellon Foundation; Smithsonian Tropical Research Institute; Gates Cambridge Trust; Worts' Travelling Scholarship; Cambridge Philosophical Society; Gatsby Charitable Foundation FX We thank W. Foster for help with insect identification, M. Kaspari for helpful comments and the use of the Berlese funnels and two anonymous reviewers for their constructive comments on the manuscript. This study was funded by the Mellon Foundation, and the Smithsonian Tropical Research Institute, E. J. S. was supported by the Gates Cambridge Trust, a Worts' Travelling Scholarship, and a Cambridge Philosophical Society Travel Grant. R. I. C. R. was supported by a studentship from the Gatsby Charitable Foundation. The fieldwork was carried out at the Smithsonian Tropical Research Institute in Panama, to whom we are very grateful. NR 47 TC 19 Z9 20 U1 2 U2 37 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0006-3606 J9 BIOTROPICA JI Biotropica PD MAR PY 2010 VL 42 IS 2 BP 194 EP 200 DI 10.1111/j.1744-7429.2009.00576.x PG 7 WC Ecology SC Environmental Sciences & Ecology GA 564LK UT WOS:000275215700009 ER PT J AU Black, S Butt, Y AF Black, Samuel Butt, Yousaf TI The growing threat of space debris SO BULLETIN OF THE ATOMIC SCIENTISTS LA English DT Article AB The danger to orbiting satellites from space debris has been known for decades, yet accidents and intentional antisatellite weapon tests still pose serious threats. Better rules are needed to govern increasingly busy near-Earth space. C1 [Black, Samuel] Henry L Stimson Ctr, Washington, DC USA. [Butt, Yousaf] Harvard Smithsonian Ctr Astrophys, Div High Energy Astrophys, Cambridge, MA USA. [Butt, Yousaf] NASA, Orbiting Chandra Xray Observ Project, Washington, DC USA. RP Black, S (reprint author), Henry L Stimson Ctr, Washington, DC USA. NR 18 TC 1 Z9 1 U1 0 U2 3 PU SAGE PUBLICATIONS INC PI THOUSAND OAKS PA 2455 TELLER RD, THOUSAND OAKS, CA 91320 USA SN 0096-3402 J9 B ATOM SCI JI Bull. Atom. Scient. PD MAR-APR PY 2010 VL 66 IS 2 BP 1 EP 8 DI 10.2968/066002001 PG 8 WC International Relations; Social Issues SC International Relations; Social Issues GA 624JQ UT WOS:000279814800001 ER PT J AU Ewing, J Gianvito, J Goldstein, B Guest, H Healy, J Jones, K Kardish, L Losier, M Pena, R Quandt, J Schwartz, D Sekuler, A Skolnick, D Vick, T AF Ewing, John Gianvito, John Goldstein, Bruce Guest, Haden Healy, Jim Jones, Kent Kardish, Laurence Losier, Marie Pena, Richard Quandt, James Schwartz, David Sekuler, Adam Skolnick, Dylan Vick, Tom TI Repertory Film Programming A Critical Symposium featuring commentary SO CINEASTE LA English DT Editorial Material C1 [Ewing, John] Cleveland Inst Art Cinematheque, Cleveland, OH USA. [Ewing, John] Cleveland Museum Art, Cleveland, OH USA. [Gianvito, John] Emerson Coll, Boston, MA 02116 USA. [Goldstein, Bruce] Film Forum, New York, NY USA. [Guest, Haden] Harvard Univ, Dept Visual & Environm Studies, Cambridge, MA 02138 USA. [Healy, Jim] George Eastman House, Mot Picture Dept, Rochester, NY USA. [Jones, Kent] Lincoln Ctr, Film Soc, Lincoln, NE USA. [Kardish, Laurence] Carleton Univ, Film Soc, Ottawa, ON K1S 5B6, Canada. [Kardish, Laurence] Canadian Film Inst, Natl Film Theatre, Ottawa, ON, Canada. [Losier, Marie] Alliance Francaise, French Inst, New York, NY USA. [Pena, Richard] Lincoln Ctr, Film Soc, Lincoln, NE USA. [Pena, Richard] Columbia Univ, New York, NY 10027 USA. [Quandt, James] TIFF Cinematheque, Toronto, ON, Canada. [Sekuler, Adam] NW Film Forum, Seattle, WA USA. [Vick, Tom] Smithsonian Inst, Washington, DC 20560 USA. RP Ewing, J (reprint author), Cleveland Inst Art Cinematheque, Cleveland, OH USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU CINEASTE PI NEW YORK PA 200 PARK AVE SOUTH, NEW YORK, NY 10003 USA SN 0009-7004 J9 CINEASTE JI Cineaste PD SPR PY 2010 VL 35 IS 2 BP 38 EP 53 PG 16 WC Film, Radio, Television SC Film, Radio & Television GA 567WD UT WOS:000275477200014 ER PT J AU Ritson-Williams, R Paul, VJ Arnold, SN Steneck, RS AF Ritson-Williams, R. Paul, Valerie J. Arnold, S. N. Steneck, R. S. TI Larval settlement preferences and post-settlement survival of the threatened Caribbean corals Acropora palmata and A. cervicornis SO CORAL REEFS LA English DT Article DE Larval ecology; Settlement; Metamorphosis; Post-settlement survival; Coralline algae; Coral reefs; Threatened species ID ALGAL RIDGE; METAMORPHOSIS; RECRUITMENT; MACROALGAE; REEFS; CONSERVATION; MANAGEMENT; INDUCTION; CAYS AB The settlement specificity of two threatened Caribbean corals, Acropora palmata and A. cervicornis, was tested by measuring their rates of larval metamorphosis in response to crustose coralline algae (CCA) and other substrata. In the no-choice experiments, the coral larvae were placed in six treatments: filtered seawater (FSW), a fragment of biofilmed dead skeleton of A. palmata, or a fragment of one of four species of CCA (Hydrolithon boergesenii, Porolithon pachydermum, Paragoniolithon solubile, and Titanoderma prototypum). Within each CCA treatment, there were three different substrata on which to settle and metamorphose: (1) the CCA surface, (2) the rock under the CCA, or (3) the plastic dish. The 5-day-old larvae of both A. palmata and A. cervicornis had similar rates of total metamorphosis (all substrata combined) in every treatment (excluding FSW) even in the absence of CCA. However, there were differences in larval behavior among the CCA species since the larvae settled and metamorphosed on different substrata in the presence of different CCA species. In the no-choice experiments the larvae of both corals had higher rates of metamorphosis on the top surfaces of H. boergesenii and/or T. prototypum than on P. pachydermum. In the choice experiments, the coral larvae were offered two species of CCA in the same dish. When given a choice, both species of coral larvae had more settlement and metamorphosis on the surface of H. boergesenii or T. prototypum or clean rock than onto the surface of P. solubile. After 6 weeks in the field, transplanted A. palmata recruits had approximately 15% survival on both T. prototypum and H. boergesenii, but A. cervicornis recruits only survived on T. prototypum (13%). Some, but not all, CCA species facilitated the larval settlement and post-settlement survival of these two threatened corals, highlighting the importance of benthic community composition for successful coral recruitment. C1 [Ritson-Williams, R.; Paul, Valerie J.] Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. [Arnold, S. N.; Steneck, R. S.] Univ Maine, Darling Marine Ctr, Sch Marine Sci, Walpole, ME 04573 USA. RP Paul, VJ (reprint author), Smithsonian Marine Stn Ft Pierce, 701 Seaway Dr, Ft Pierce, FL 34949 USA. EM paul@si.edu FU Smithsonian Marine Science Network; Caribbean Coral Reef Ecosystems (CCRE) Program; Connectivity Working Group of the World Bank's Global Environment Facility project FX Special thanks to Klaus Rutzler and Michael Carpenter for facilitating our research at Carrie Bow Cay in Belize. We thank Belize Fisheries Department for providing us with permits and facilitating our research in Belize. Nikki Fogarty and Kathy Morrow were invaluable in providing field assistance. Lee-Ann Hayek provided statistical advice. The manuscript was improved by the comments of two anonymous reviewers. This research was funded by the Smithsonian Marine Science Network and the Caribbean Coral Reef Ecosystems (CCRE) Program. Additional funding for RSS and SNA was from the Connectivity Working Group of the World Bank's Global Environment Facility project, Coral Reef Targeted Research and Capacity Building for Management. This is contribution # 807 of the Smithsonian Marine Station at Fort Pierce and is # 868 of the CCRE program. NR 38 TC 59 Z9 61 U1 4 U2 53 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0722-4028 EI 1432-0975 J9 CORAL REEFS JI Coral Reefs PD MAR PY 2010 VL 29 IS 1 BP 71 EP 81 DI 10.1007/s00338-009-0555-z PG 11 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 552MF UT WOS:000274294200010 ER PT J AU Savage, BD AF Savage, Barbara D. TI An Historian's Historian SO DU BOIS REVIEW-SOCIAL SCIENCE RESEARCH ON RACE LA English DT Editorial Material C1 [Savage, Barbara D.] Univ Penn, Dept Hist, Philadelphia, PA 19104 USA. [Savage, Barbara D.] Harvard Univ, Smithsonian Inst, Radcliffe Inst Adv Studies, Cambridge, MA 02138 USA. [Savage, Barbara D.] Princeton Univ, Ctr Study Relig, Princeton, NJ 08544 USA. [Savage, Barbara D.] New York Publ Lib, Scholars In Residence Program, Schomburg Ctr Black Culture, New York, NY USA. RP Savage, BD (reprint author), Univ Penn, Dept Hist, Coll Hall 208, Philadelphia, PA 19104 USA. EM bdsavage@sas.upenn.edu NR 3 TC 0 Z9 0 U1 0 U2 0 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 1742-058X J9 DU BOIS REV JI Du Bois Rev. PD SPR PY 2010 VL 7 IS 1 BP 10 EP 12 DI 10.1017/S1742058X10000093 PG 3 WC Ethnic Studies; Sociology SC Ethnic Studies; Sociology GA V26NZ UT WOS:000208553600005 ER PT J AU Faaborg, J Holmes, RT Anders, AD Bildstein, KL Dugger, KM Gauthreaux, SA Heglund, P Hobson, KA Jahn, AE Johnson, DH Latta, SC Levey, DJ Marra, PP Merkord, CL Nol, E Rothstein, SI Sherry, TW Sillett, TS Thompson, FR Warnock, N AF Faaborg, John Holmes, Richard T. Anders, Angela D. Bildstein, Keith L. Dugger, Katie M. Gauthreaux, Sidney A., Jr. Heglund, Patricia Hobson, Keith A. Jahn, Alex E. Johnson, Douglas H. Latta, Steven C. Levey, Douglas J. Marra, Peter P. Merkord, Christopher L. Nol, Erica Rothstein, Stephen I. Sherry, Thomas W. Sillett, T. Scott Thompson, Frank R., III Warnock, Nils TI Conserving migratory land birds in the New World: Do we know enough? SO ECOLOGICAL APPLICATIONS LA English DT Article DE breeding season management; conservation; en route bird conservation; global climate change; intratropical migration; land birds; migration; Partners in Flight; source-sink dynamics; winter population limitation ID NORTH-AMERICAN BIRDS; WINTER SITE FIDELITY; CLIMATE-CHANGE; HABITAT USE; NEOTROPICAL MIGRANT; NONBREEDING SEASON; GRASSLAND BIRDS; REGENERATING CLEARCUTS; POPULATION LIMITATION; SETOPHAGA-RUTICILLA AB Migratory bird needs must be met during four phases of the year: breeding season, fall migration, wintering, and spring migration; thus, management may be needed during all four phases. The bulk of research and management has focused on the breeding season, although several issues remain unsettled, including the spatial extent of habitat influences on fitness and the importance of habitat on the breeding grounds used after breeding. Although detailed investigations have shed light on the ecology and population dynamics of a few avian species, knowledge is sketchy for most species. Replication of comprehensive studies is needed for multiple species across a range of areas. Information deficiencies are even greater during the wintering season, when birds require sites that provide security and food resources needed for survival and developing nutrient reserves for spring migration and, possibly, reproduction. Research is needed on many species simply to identify geographic distributions, wintering sites, habitat use, and basic ecology. Studies are complicated, however, by the mobility of birds and by sexual segregation during winter. Stable-isotope methodology has offered an opportunity to identify linkages between breeding and wintering sites, which facilitates understanding the complete annual cycle of birds. The twice-annual migrations are the poorest-understood events in a bird's life. Migration has always been a risky undertaking, with such anthropogenic features as tall buildings, towers, and wind generators adding to the risk. Species such as woodland specialists migrating through eastern North America have numerous options for pausing during migration to replenish nutrients, but some species depend on limited stopover locations. Research needs for migration include identifying pathways and timetables of migration, quality and distribution of habitats, threats posed by towers and other tall structures, and any bottlenecks for migration. Issues such as human population growth, acid deposition, climate change, and exotic diseases arc global concerns with uncertain consequences to migratory birds and even less-certain remedies. Despite enormous gaps in our understanding of these birds, research, much of it occurring in the past 30 years, has provided sufficient information to make intelligent conservation efforts but needs to expand to handle future challenges. C1 [Faaborg, John] Univ Missouri, Div Biol Sci, Columbia, MO 65211 USA. [Holmes, Richard T.] Dartmouth Coll, Dept Biol Sci, Hanover, NH 03755 USA. [Anders, Angela D.] Clancy Environm Consultants, Honolulu, HI 96825 USA. [Bildstein, Keith L.] Acopian Ctr Conservat Learning, Orwigsburg, PA 17961 USA. [Dugger, Katie M.] Oregon State Univ, Dept Fisheries & Wildlife, Corvallis, OR 97331 USA. [Gauthreaux, Sidney A., Jr.] Clemson Univ, Dept Biol Sci, Clemson, SC 29634 USA. [Heglund, Patricia] US Fish & Wildlife Serv, La Crosse, WI 54603 USA. [Hobson, Keith A.] Environm Canada, Saskatoon, SK S7N 3H5, Canada. [Jahn, Alex E.; Levey, Douglas J.] Univ Florida, Dept Biol, Gainesville, FL 32611 USA. [Johnson, Douglas H.] USGS, No Prairie Wildlife Res Ctr, St Paul, MN 55108 USA. [Latta, Steven C.] Natl Aviary, Dept Conservat & Field Res, Pittsburgh, PA 15212 USA. [Marra, Peter P.; Sillett, T. Scott] Natl Zool Pk, Smithsonian Migratory Bird Ctr, Washington, DC 20013 USA. [Merkord, Christopher L.] Univ Missouri, Div Biol Sci, Columbia, MO 65211 USA. [Nol, Erica] Trent Univ, Ecol & Conservat Grp, Environm & Life Sci Grad Program, Peterborough, ON K9J 7B8, Canada. [Nol, Erica] Trent Univ, Dept Biol, Peterborough, ON K9J 7B8, Canada. [Rothstein, Stephen I.] Univ Calif Santa Barbara, Dept Ecol Evolut & Marine Biol, Santa Barbara, CA 93106 USA. [Sherry, Thomas W.] Tulane Univ, Dept Ecol & Evolut Biol, New Orleans, LA 70118 USA. [Thompson, Frank R., III] Univ Missouri, USDA, US Forest Serv, No Res Stn, Columbia, MO 65211 USA. [Warnock, Nils] PRBO Conservat Sci, Petaluma, CA 94954 USA. RP Faaborg, J (reprint author), Univ Missouri, Div Biol Sci, Columbia, MO 65211 USA. EM faaborgj@missouri.edu OI Merkord, Chris/0000-0003-2825-1904 NR 171 TC 119 Z9 124 U1 8 U2 144 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 1051-0761 EI 1939-5582 J9 ECOL APPL JI Ecol. Appl. PD MAR PY 2010 VL 20 IS 2 BP 398 EP 418 DI 10.1890/09-0397.1 PG 21 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA 582YA UT WOS:000276635600007 PM 20405795 ER PT J AU Ryder, TB Reitsma, R Evans, B Marra, PP AF Ryder, Thomas B. Reitsma, Robert Evans, Brian Marra, Peter P. TI Quantifying avian nest survival along an urbanization gradient using citizen- and scientist-generated data SO ECOLOGICAL APPLICATIONS LA English DT Article DE artificial nests; citizen science; land-use matrix; MARK; nest survival; predation pressure; urbanization ID ARTIFICIAL BIRD NESTS; URBAN GRADIENT; REPRODUCTIVE SUCCESS; LAND-USE; PREDATION; LANDSCAPE; SUBURBAN; CONSERVATION; PROGRAM; ECOLOGY AB Despite the increasing pace of urbanization little is known about the factors that limit bird populations (i.e., population-level processes) within the urban/suburban land-use matrix. Here, we report rates of nest survival within the matrix of an urban land-use gradient in the greater Washington, D.C., USA, area for live common songbirds using data collected by scientists and citizens as part of a project called Neighborhood Nestwatch. Using program MARK, we modeled the effects of species, urbanization at multiple spatial scales (canopy cover and impervious surface), and observer (citizen vs. scientist) on nest survival of lour open-cup and one cavity-nesting species. In addition, artificial nests were used to determine the relative impacts of specific predators along the land-use gradient. Our results suggest that predation on nests within the land-use matrix declines with urbanization but that there are species-specific differences. Moreover, variation in nest survival among species was best explained by urbanization metrics measured at larger "neighborhood" spatial scales (e.g., 1000 m). Trends were supported by data from artificial nests and suggest that variable predator communities (avian vs. mammalian) are one possible mechanism to explain differential nest survival. In addition, we assessed the quality of citizen science data and show that citizens had no negative effect on nest survival and provided estimates of nest survival comparable to Smithsonian biologists. Although birds nesting within the urban matrix experienced higher nest survival, individuals also faced a multitude of other challenges such as contaminants and invasive species, all of which could reduce adult survival. C1 [Ryder, Thomas B.; Reitsma, Robert; Evans, Brian; Marra, Peter P.] Natl Zool Pk, Smithsonian Migratory Bird Ctr, Washington, DC 20008 USA. RP Ryder, TB (reprint author), Natl Zool Pk, Smithsonian Migratory Bird Ctr, 3001 Connecticut Ave, Washington, DC 20008 USA. EM rydert@si.edu FU Mills Corporation; Wallace Genetic Foundation; Susan and Frank Mars; National Science Foundation [ESI-0540185] FX The Mills Corporation, Wallace Genetic Foundation, Susan and Frank Mars, and the National Science Foundation (ESI-0540185) provided financial support or this study. We are grateful for the field assistance provided by K. Roux. S. LeClair. A. Ursin. N. Bohlmann, S. Campbell, J. Pickar. N. Diggs. A. Balogh, M. Brady, D. Rauch. G. Kruskall. J. Rutter. J. Dowling. M. Newhouse, and J. Thien. Two anonymous reviewers improved previous drifts of the manuscript. Finally. We thank the Neighborhood Nestwatch participants for access to their property and steadfast data collection. NR 51 TC 29 Z9 29 U1 14 U2 84 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 MAR PY 2010 VL 20 IS 2 BP 419 EP 426 DI 10.1890/09-0040.1 PG 8 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA 582YA UT WOS:000276635600008 PM 20405796 ER PT J AU Gallegos, CL Jordan, TE Hedrick, SS AF Gallegos, Charles L. Jordan, Thomas E. Hedrick, Sharyn S. TI Long-term Dynamics of Phytoplankton in the Rhode River, Maryland (USA) SO ESTUARIES AND COASTS LA English DT Article DE Phytoplankton; Species composition; Rhode River; Chlorophyll concentration; Interannual variability ID CHESAPEAKE-BAY; SPRING BLOOM; MARINE-PHYTOPLANKTON; AQUATIC VEGETATION; COMMUNITY ECOLOGY; COASTAL WATERS; ESTUARY; CHLOROPHYLL; SEA; NUTRIENTS AB We analyzed interannual variability in a long-term record of chlorophyll concentration and phytoplankton species composition in the Rhode River, Maryland (USA). Over the approximately 30-year record, there was no long-term monotonic trend in phytoplankton chlorophyll concentration, though temporary directional trends related to precipitation patterns sometimes persisted for a decade before reversing. From counts on preserved samples, we estimated the dominance by different pigment-bearing groups and size classes. Diatoms, dinoflagellates, and cryptophytes comprised about 80-97% of the annual averaged class-specific biovolume. Cryptophytes dominated the first 2 years in the data set but displayed a long-term decline, after which diatoms dominated in all but four consecutive years in which there were large dinoflagellate blooms. There was a long-term increase in cells with equivalent spherical diameters from 4 to 10 A mu m, accompanied by declines in the proportion of cells in the 2- to 4- and 10- to 20-A mu m size classes. The main cause of these changes in size classes was a long-term increase in Chroomonas sp. and Apedinella radians and long-term decline in Microcystis sp. and an unidentified cryptophyte, respectively. These taxa were cosmopolitan in their seasonal and spatial distributions, and hence the long-term changes in taxa did not conform well with conceptual models based on succession of "life-forms." The segregation of diatoms and dinoflagellates expected on the basis of "life-forms" applied to seasonal and spatial patterns. Characterizing the phytoplankton community in terms of diversity, size, and class-specific biovolume gave results that were consistent with one another and added insight to the broad-scale changes in chlorophyll concentration. Subtle changes in the size distribution of cryptophytes were not apparent from biovolume measures and would not have been apparent without microscopy. Though causes of such shifts may be difficult to identify, identifying the causes and predicting potential consequences cannot even be attempted without awareness of the phenomena. C1 [Gallegos, Charles L.; Jordan, Thomas E.; Hedrick, Sharyn S.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Gallegos, CL (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM gallegosc@si.edu OI Gallegos, Charles/0000-0001-5112-0166 FU Smithsonian Environmental Sciences Program FX We thank Sam Benson, Ann-Marie Hartsig, and Joe Miklas for help with sampling and laboratory analyses. Financial support for this work was provided by the Smithsonian Environmental Sciences Program. We extend our appreciation to J. Johnson, R. Lacouture, H. Marshall, and M. Mallonee in development and recent revisions of the Chesapeake Bay Program Phytoplankton Database. Two anonymous reviewers provided helpful comments on an earlier draft. NR 55 TC 13 Z9 13 U1 0 U2 10 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1559-2723 J9 ESTUAR COAST JI Estuaries Coasts PD MAR PY 2010 VL 33 IS 2 SI SI BP 471 EP 484 DI 10.1007/s12237-009-9172-x PG 14 WC Environmental Sciences; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 567DW UT WOS:000275424300019 ER PT J AU Kaeppler, AL AF Kaeppler, Adrienne L. TI The Beholder's Share: Viewing Music and Dance in a Globalized World SO ETHNOMUSICOLOGY LA English DT Article; Proceedings Paper CT 51st Annual Meeting of the Society-for-Ethnomusicology CY NOV 16-19, 2006 CL Honolulu, HI SP Soc Ethnomusicol C1 Smithsonian Inst, Washington, DC 20560 USA. RP Kaeppler, AL (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 26 TC 5 Z9 5 U1 0 U2 2 PU SOC ETHNOMUSICOLOGY INC PI BLOOMINGTON PA MORRISON HALL, ROOM 005 INDIANA UNIVERSITY, BLOOMINGTON, IN 47405 USA SN 0014-1836 J9 ETHNOMUSICOLOGY JI Ethnomusicology PD SPR-SUM PY 2010 VL 54 IS 2 BP 185 EP 201 PG 17 WC Music SC Music GA 608SE UT WOS:000278605500002 ER PT J AU Foltz, DW Mah, CL AF Foltz, David W. Mah, Christopher L. TI Difference in larval type explains patterns of nonsynonymous substitutions in two ancient paralogs of the histone H3 gene in sea stars SO EVOLUTION & DEVELOPMENT LA English DT Article ID PHYLOGENETIC TREE SELECTION; CODON USAGE; POPULATION-STRUCTURE; DUPLICATE GENES; MODE; EVOLUTION; SEQUENCE; DIVERGENCE; REPRODUCTION; ECHINODERMS AB P>Paralogous genes frequently show differences in patterns and rates of substitution that are typically attributed to different selection regimes, mutation rates, or local recombination rates. Here, two anciently diverged paralogous copies of the histone H3 gene in sea stars, the tandem-repetitive early-stage gene and a newly isolated gene with lower copy number that was termed the "putative late-stage histone H3 gene" were analyzed in 69 species with varying mode of larval development. The two genes showed differences in relative copy number, overall substitution rates, nucleotide composition, and codon usage, but similar patterns of relative nonsynonymous substitution rates, when analyzed by the d(N)/d(S) ratio. Sea stars with a nonpelagic and nonfeeding larval type (i.e., brooding lineages) were observed to have d(N)/d(S) ratios that were larger than for nonbrooders but equal between the two paralogs. This finding suggested that demographic differences between brooding and nonbrooding lineages were responsible for the elevated d(N)/d(S) ratios observed for brooders and refuted a suggestion from a previous analysis of the early-stage gene that the excess nonsynonymous substitutions were due to either (1) gene expression differences at the larval stage between brooders and nonbrooders or (2) the highly repetitive structure of the early-stage histone H3 gene. C1 [Foltz, David W.] Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA. [Mah, Christopher L.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20007 USA. RP Foltz, DW (reprint author), Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA. EM dfoltz@lsu.edu RI Mah, Christopher/B-5771-2008 FU NSF [OPP-0631245]; Office of Research and Economic Development at Louisiana State University FX We thank Dr. Robert Van Syoc for arranging loan of material from the California Academy of Sciences and Dr. Mark A. Batzer for suggestions. Jerilyn A. Walker and Dr. Scott W. Herke provided assistance with the qPCR analyses. James W. Halk, Tap Bui and Caitlyn Blanchard assisted in the laboratory. Financial support was provided by NSF grant OPP-0631245 to C. L. Mah and an award from the Office of Research and Economic Development at Louisiana State University to D. W. Foltz. NR 37 TC 3 Z9 3 U1 0 U2 3 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1520-541X J9 EVOL DEV JI Evol. Dev. PD MAR-APR PY 2010 VL 12 IS 2 BP 222 EP 230 DI 10.1111/j.1525-142X.2010.00406.x PG 9 WC Evolutionary Biology; Developmental Biology; Genetics & Heredity SC Evolutionary Biology; Developmental Biology; Genetics & Heredity GA 574WH UT WOS:000276024400010 PM 20433461 ER PT J AU Bauer, M Hoagland, P Leschine, TM Blount, BG Pomeroy, CM Lampl, LL Scherer, CW Ayres, DL Tester, PA Sengco, MR Sellner, KG Schumacker, J AF Bauer, Marybeth Hoagland, Porter Leschine, Thomas M. Blount, Benjamin G. Pomeroy, Caroline M. Lampl, Linda L. Scherer, Clifford W. Ayres, Dan L. Tester, Patricia A. Sengco, Mario R. Sellner, Kevin G. Schumacker, Joe TI The importance of human dimensions research in managing harmful algal blooms SO FRONTIERS IN ECOLOGY AND THE ENVIRONMENT LA English DT Review ID ECOLOGICAL RESILIENCE; ECOSYSTEM MANAGEMENT; RISK COMMUNICATION; PHYTOPLANKTON; SCIENCE AB Harmful algal blooms (HABs) are natural freshwater and marine hazards that impose substantial adverse impacts on the human use of coastal and marine resources. The socioeconomic and health impacts of HABs can be considerable, thereby making a case for "human dimensions" research to support HAB response. Human dimensions research is multidisciplinary, integrating social science, humanities, and other fields with natural science to enhance resource management by addressing human causes, consequences, and responses to coastal environmental problems. Case studies reported here illustrate the importance of human dimensions research. Incorporating such research into the scientific agenda - as well as into management decisions of public agencies concerned with natural resource management, environmental protection, and public health and welfare - requires the development of both strategic guidance and institutional capacity. The recent development of a multi-agency research strategy for HAB response and a strategic plan for human dimensions research represent two important steps in this direction. C1 [Bauer, Marybeth] NOAA, NOS, NCCOS, Silver Spring, MD USA. [Hoagland, Porter] Woods Hole Oceanog Inst, Marine Policy Ctr, Woods Hole, MA 02543 USA. [Leschine, Thomas M.] Univ Washington, Sch Marine Affairs, Seattle, WA 98195 USA. [Blount, Benjamin G.] SocioEcol Informat, Helotes, TX USA. [Pomeroy, Caroline M.] Calif Sea Grant Extens Program, Watsonville, CA USA. [Lampl, Linda L.] Lampl Herbert Consultants Inc, Tallahassee, FL USA. [Scherer, Clifford W.] Cornell Univ, Ithaca, NY USA. [Ayres, Dan L.] Washington State Dept Fish & Wildlife, Reg Off 6, Montesano, WA USA. [Tester, Patricia A.] NOAA, NOS, NCCOS, Ctr Coastal Fisheries & Habitat Res, Beaufort, NC USA. [Sengco, Mario R.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Sellner, Kevin G.] Chesapeake Res Consortium, Edgewater, MD USA. [Schumacker, Joe] Quinault Dept Nat Resources, Taholah, WA USA. RP Bauer, M (reprint author), NOAA, NOS, NCCOS, Silver Spring, MD USA. EM marybeth.bauer@noaa.gov OI Hoagland, Porter/0000-0003-0744-4184 FU National Institute of Environmental Health Sciences (NIEHS) [P50 ES012762]; NIH; National Science Foundation [OCE-0434087] FX This paper was developed with partial support from NOAA's National Centers for Coastal and Ocean Science. The authors thank G Matlock for comments on a draft. Thortias Leschine's contributions to this Publication were supported by grant number P50 ES012762 from the National Institute of Environmental Health Sciences (NIEHS), NIH, and OCE-0434087 from the National Science Foundation. Its contents are solely the responsibitity of the authors and do not necessarily represent the official views of the NIEHS, NIH, or NSE NR 50 TC 4 Z9 4 U1 2 U2 23 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 1540-9295 J9 FRONT ECOL ENVIRON JI Front. Ecol. Environ. PD MAR PY 2010 VL 8 IS 2 BP 75 EP 83 DI 10.1890/070181 PG 9 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA 567PF UT WOS:000275458400019 ER PT J AU Sucher, SD Attaway, SW Attaway, NL Post, JE AF Sucher, Scott D. Attaway, Stephen W. Attaway, Nancy L. Post, Jeffrey E. TI POSSIBLE "SISTER" STONES OF THE HOPE DIAMOND SO GEMS & GEMOLOGY LA English DT Article ID BLUE AB For more than a century, historians have debated the existence of "sister" stones to the Hope diamond, most notably the Brunswick Blue and the Pine diamonds. The recent discovery of a lead cast of the French Blue, the Hope's precursor, has provided a more accurate model of that diamond, which disappeared in 1792. Computer models of the French Blue and its parent stone, the Tavernier Blue, were used to determine whether other diamonds might have been created when the Tavernier Blue was cut into the French Blue, or when the latter was cut into the Hope. The results show that it was not feasible for other significant diamonds to have been created during any recutting. C1 [Sucher, Scott D.] The Stonecutter, Tijeras, NM USA. [Attaway, Stephen W.; Attaway, Nancy L.] High Country Gems, Tijeras, NM USA. [Post, Jeffrey E.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Sucher, SD (reprint author), The Stonecutter, Tijeras, NM USA. EM scott@museumdiamonds.com NR 17 TC 1 Z9 1 U1 0 U2 4 PU GEMOLOGICAL INST AMER PI CARLSBAD PA 5345 ARMADA DR, CARLSBAD, CA 92008 USA SN 0016-626X J9 GEMS GEMOL JI Gems Gemol. PD SPR PY 2010 VL 46 IS 1 BP 28 EP 35 PG 8 WC Mineralogy SC Mineralogy GA 592LN UT WOS:000277380500003 ER PT J AU Srygley, RB Dudley, R Oliveira, EG Aizprua, R Pelaez, NZ Riveros, AJ AF Srygley, Robert B. Dudley, Robert Oliveira, Evandro G. Aizprua, Rafael Pelaez, Nicole Z. Riveros, Andre J. TI El Nino and dry season rainfall influence hostplant phenology and an annual butterfly migration from Neotropical wet to dry forests SO GLOBAL CHANGE BIOLOGY LA English DT Article DE climate change; El Nino; ENSO; insect flight; insect migration; migratory behavior; resource limitation; tropical rainforest ID WIND DRIFT COMPENSATION; CLIMATE-CHANGE; HERBIVORE OUTBREAK; FLUCTUATIONS; LEPIDOPTERA; ENSO; CONSEQUENCES; ECOSYSTEMS; STRATEGIES; CALIFORNIA AB We censused butterflies flying across the Panama Canal at Barro Colorado Island (BCI) for 16 years and butterfly hostplants for 8 years to address the question: What environmental factors influence the timing and magnitude of migrating Aphrissa statira butterflies? The peak migration date was earlier when the wet season began earlier and when soil moisture content in the dry season preceding the migration was higher. The peak migration date was also positively associated with peak leaf flushing of one hostplant (Callichlamys latifolia) but not another (Xylophragma seemannianum). The quantity of migrants was correlated with the El Nino Southern Oscillation, which influenced April soil moisture on BCI and total rainfall in the dry season. Both hostplant species responded to El Nino with greater leaf flushing, and the number of adults deriving from or laying eggs on those new leaves was greatest during El Nino years. The year 1993 was exceptional in that the number of butterflies migrating was lower than predicted by the El Nino event, yet the dry season was unusually wet for an El Nino year as well. Thus, dry season rainfall appears to be a primary driver of larval food production and population outbreaks for A. statira. Understanding how global climate cycles and local weather influence tropical insect migrations improves the predictability of ecological effects of climate change. C1 [Srygley, Robert B.; Dudley, Robert] Smithsonian Trop Res Inst, Balboa, Panama. [Dudley, Robert] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. [Oliveira, Evandro G.] Ctr Univ UNA, Fac Ciencias Biol & Saude, BR-30180100 Belo Horizonte, MG, Brazil. [Aizprua, Rafael] Univ Panama, Dept Bot, Panama City, Panama. [Pelaez, Nicole Z.] Univ Los Andes, Dept Ciencias Biol, Bogota, Colombia. [Riveros, Andre J.] Univ Nacl Colombia, Dept Biol, Bogota, Colombia. RP Srygley, RB (reprint author), ARS, USDA, NPARL, 1500 N Cent Ave, Sidney, MT 59270 USA. EM robert.srygley@ars.usda.gov FU Smithsonian Institution; National Geographic Society Committee for Research and Exploration FX A Senior Postdoctoral Fellowship to R. B. S. from the Smithsonian Institution and grants from the National Geographic Society Committee for Research and Exploration supported the research. The Autoridad Nacional del Ambiente (ANAM) granted permission to conduct the research in Panama. Hydrological and radiation data were provided by the Terrestrial-Environmental Science Program of the STRI. Season begin and end dates were provided by the Meteorological and Hydrological Branch of the Panama Canal Authority (ACP). For presentational purposes, data were modified from their original form. We thank the meteorologists and their parent institutions for their long-term commitment to these essential programs. We also thank S. Paton for numerous discussions and assistance with BCI climate and its effects, and Joe Wright and Egbert Leigh for commenting on the manuscript. NR 39 TC 19 Z9 19 U1 3 U2 44 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1354-1013 J9 GLOBAL CHANGE BIOL JI Glob. Change Biol. PD MAR PY 2010 VL 16 IS 3 BP 936 EP 945 DI 10.1111/j.1365-2486.2009.01986.x PG 10 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 554EY UT WOS:000274419500004 ER PT J AU Berke, SK Mahon, AR Lima, FP Halanych, KM Wethey, DS Woodin, SA AF Berke, Sarah K. Mahon, Andrew R. Lima, Fernando P. Halanych, Kenneth M. Wethey, David S. Woodin, Sarah A. TI Range shifts and species diversity in marine ecosystem engineers: patterns and predictions for European sedimentary habitats SO GLOBAL ECOLOGY AND BIOGEOGRAPHY LA English DT Article DE Arenicolidae; Bay of Biscay; climate change; Diopatra; molecular phylogenies; polychaetes ID DIOPATRA-CUPREA POLYCHAETA; COMMUNITY STRUCTURE; INTERTIDAL ORGANISMS; LUGWORM EXCLUSION; ARENICOLA-MARINA; ENGLISH-CHANNEL; DISTURBANCE; ONUPHIDAE; ANNELIDA; WORMS AB Aim Ecosystem engineering polychaetes in the genus Diopatra are undergoing range shifts in western Europe. Here we: (1) assess the species diversity underlying these shifts; (2) link biogeographic patterns to sea surface temperature patterns; and (3) predict possible ecosystem-level outcomes of Diopatra's northward expansion. Location Western Europe. Methods We use molecular phylogenetic and morphological evidence to assess species diversity and biogeographic ranges. Using regression tree analyses, we assess thermal limits for two Diopatra species. We compare biogeographic patterns with historical sea surface temperature patterns to draw links between range shifts and climate change. Finally, we review published data to predict potential ecological changes as Diopatra invades new habitats. Results The native Diopatra neapolitana range has contracted 130 km to the south. A cryptogenic species, Diopatra sp. A, has extended the northern limit of the genus 350 km to the southern Brittany Peninsula. Both shifts can be explained by historical sea surface temperature anomalies. The Diopatra sp. A expansion is predicted to continue into the English Channel and the North Sea, introducing large tube structures to sheltered sedimentary habitats that currently lack such structures. Main conclusions As climate change intensifies, the sediment-stabilizing Diopatra sp. A will invade habitats dominated by the bioturbating lugworm Arenicola marina. The resulting interaction between functionally different ecosystem engineers will probably cause ecological changes in northern European coastal waters. Existing data for Diopatra species and arenicolids suggest that the diversity and biomass of macroalgae, vascular plants, infauna and epibenthic fauna may increase, while microbial activity may decrease. Net changes in productivity will depend on the relative rates of these changes. C1 [Berke, Sarah K.; Lima, Fernando P.; Wethey, David S.; Woodin, Sarah A.] Univ S Carolina, Dept Biol Sci, Columbia, SC 29208 USA. [Berke, Sarah K.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Mahon, Andrew R.; Halanych, Kenneth M.] Auburn Univ, Dept Biol Sci, Auburn, AL 36849 USA. [Lima, Fernando P.] Ctr Invest Biodiversidade & Recursos Genet, CIBIO, P-4485661 Vairao, Portugal. RP Berke, SK (reprint author), Univ S Carolina, Dept Biol Sci, 715 Sumter St, Columbia, SC 29208 USA. EM skberke@gmail.com RI Halanych, Ken/A-9480-2009; Wethey, David/K-8063-2014; Woodin, Sarah/K-8481-2014; Lima, Fernando/C-1398-2008 OI Halanych, Ken/0000-0002-8658-9674; Wethey, David/0000-0002-2549-1606; Woodin, Sarah/0000-0001-5615-2212; Lima, Fernando/0000-0001-9575-9834 FU Smithsonian Institution Marine Science Network; ONR [N00014-03-1-0352]; NOAA [NA04NOS4780264]; NASA [NNG04GE43G, NNX07AF20G] FX We are deeply grateful to A. Giangrande and M. C. Gambi for providing Mediterranean specimens of D. neapolitana, G. Bachelet for providing historical specimens from the Gironde region, M. LaBarbera for providing D. cuprea tissue, and K. Fauchald, N. Volkenborn, G. Waldbusser, A. Pires and J. Zanol for insightful conversations. Quatrefages' (1865) and Saint-Joseph's (1898) samples were loaned by the Paris Museum of Natural History; we thank K. Fauchald for procuring the loan and assisting with identifications. We thank S. Santos, Auburn University, for computing assistance. While writing, S.K.B. was supported by a Smithsonian Institution Marine Science Network Fellowship; she thanks R. Osman and A. Hines for their support as well as the Halanych Laboratory at Auburn University for their hospitality and help. This study was funded by ONR (N00014-03-1-0352 to S. A. W. and D. S. W.), NOAA (NA04NOS4780264 to D. S. W. and S. A. W.), and NASA (NNG04GE43G, NNX07AF20G to D. S. W.). This is Auburn University contribution no. 54. NR 58 TC 24 Z9 24 U1 1 U2 29 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1466-822X EI 1466-8238 J9 GLOBAL ECOL BIOGEOGR JI Glob. Ecol. Biogeogr. PD MAR PY 2010 VL 19 IS 2 BP 223 EP 232 DI 10.1111/j.1466-8238.2009.00509.x PG 10 WC Ecology; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA 552VB UT WOS:000274320600007 ER PT J AU Littler, MM Littler, DS Brooks, BL AF Littler, Mark M. Littler, Diane S. Brooks, Barrett L. TI The effects of nitrogen and phosphorus enrichment on algal community development: Artificial mini-reefs on the Belize Barrier Reef sedimentary lagoon SO HARMFUL ALGAE LA English DT Article DE Algae; Belize; Colonization; Reef lagoon; Nitrogen; Phosphorus ID PLANT DEFENSE ASSOCIATIONS; CARIBBEAN CORAL-REEF; NUTRIENT ENRICHMENT; MACROALGAL BLOOMS; SOUTHEAST FLORIDA; GLOVERS REEF; LIMITED PRODUCTIVITY; MARINE-ENVIRONMENT; GRAZING INTENSITY; PRIMARY PRODUCERS AB The experiments to compare DIN and SRP enrichment effects on algal community development were conducted within a lagoonal rubble/sand reef apron west of the back reef flat at Carrie Bow Cay, Belize. Macroalgae dominate (23 taxa, 57% cover), ambient dissolved inorganic nutrient concentrations are above the levels documented for release of macroalgal growth (means of 2.06 mu M DIN = dissolved inorganic nitrogen and 0.12 mu M SRP = soluble reactive phosphorus) and grazing is negligible (1.7% Acanthophora spicifera consumed 6 h(-1)). Mini-reef diffusers containing slow-release fertilizers significantly (P < 0.05) increased DIN in the experimental DIN and SRP + DIN treatments by 2- and 3-fold (means of 4.64 and 6.41 mu M), respectively: while SRP was increased significantly (P < 0.05) in the SRP and SRP + DIN treatments by 5- and 8-fold to means of 0.69 and 0.94 mu M, relative to the control treatments. SRP and SRP + DIN treatments favored colonization by Cyanobacteria such as Spirulina sp. on the mini-reef/diffusers, with an opposite detrimental effect on reef-building crustose coralline algae. The Cyanobacteria bloom further inhibited the long-term settlement and colonization of crustose coralline algae. Conversely, the DIN and control mini-reef treatments showed low Cyanobacteria cover and became colonized by abundant reef-building coralline algae, consisting mostly of Hydrolithon boergesenii and crust stages of Amphiroa fragilissima. After 1 year, the competitively overgrowing macrophytes A. spicifera, Palisada papillosa, Padina sanctae-crucis and Spyridia filamentosa conspicuously dominated all of the treatment- and control-replicates, in accordance with the nutrient-replete ambient waters and negligible herbivory within this habitat. As predicted, nutrient additions to the mini-reef diffusers resulted in significant elevations of tissue nutrients in the most-abundant colonizer and habitat dominant, A. spicifera. Although, the resultant decreases of both the C:N and C:P molar ratios corresponded to the elevated DIN and SRP treatments, this uptake was entirely superfluous, since control population colonization and growth matched that of the experimental nutrient treatments. Published by Elsevier B.V. C1 [Littler, Mark M.; Littler, Diane S.; Brooks, Barrett L.] Smithsonian Inst, Dept Bot, NMNH 166, Washington, DC 20013 USA. RP Littler, MM (reprint author), Smithsonian Inst, Dept Bot, NMNH 166, POB 37012, Washington, DC 20013 USA. EM littlerm@si.edu FU Smithsonian Institution Scholarly Studies Program; Caribbean Coral Reef Ecosystems Program [869]; Smithsonian Marine Station at Ft. Pierce (SMSFP) [808]; National Museum of Natural History FX Support for this study came from the Smithsonian Institution Scholarly Studies Program, Caribbean Coral Reef Ecosystems Program (CCRE Contribution No. 869), the Smithsonian Marine Station at Ft. Pierce (SMSFP Contribution No. 808) and the National Museum of Natural History.[SS] NR 82 TC 12 Z9 13 U1 4 U2 48 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1568-9883 J9 HARMFUL ALGAE JI Harmful Algae PD MAR PY 2010 VL 9 IS 3 BP 255 EP 263 DI 10.1016/j.hal.2009.11.002 PG 9 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 568LG UT WOS:000275523200002 ER PT J AU Hinson, DP Wang, HQ AF Hinson, David P. Wang, Huiqun TI Further observations of regional dust storms and baroclinic eddies in the northern hemisphere of Mars SO ICARUS LA English DT Article DE Mars, Atmosphere; Mars, Climate; Atmospheres, Dynamics ID RADIO OCCULTATION MEASUREMENTS; TES NADIR DATA; MARTIAN ATMOSPHERE; INTERANNUAL VARIABILITY; SPECTRAL-ANALYSIS; GLOBAL SURVEYOR; MGS TES; TRAVELING-WAVES; ORBITER CAMERA; THERMAL TIDES AB We have investigated the near-surface meteorology in the northern hemisphere of Mars through detailed analysis of data obtained with Mars Global Surveyor in January-August 2005. The season in the northern hemisphere ranged from midsummer through winter solstice of Mars Year (MY) 27. We examined composite, wide-angle images from the Mars Orbiter Camera and compiled a catalog of the dust storms that occurred in this interval. As in previous martian years, activity in the northern hemisphere was dominated by regional "flushing" dust storms that sweep southward through the major topographic basins, most frequently in Acidalia Planitia. We also used atmospheric profiles retrieved from radio occultation experiments to characterize eddy activity near the surface at high northern latitudes. There are strong correlations between the two sets of observations, which allowed us to identify three factors that influence the timing and location of the regional dust storms: (1) transitions among baroclinic wave modes, which strongly modulate the intensity of meridional winds near the surface, (2) storms zones, which impose strong zonal variations on the amplitude of some baroclinic eddies, and (3) stationary waves, which further modulate the wind field near the surface. The flushing dust storms ceased abruptly in midautumn, possibly in response to source depletion, CO2 condensation, a shift in the period of the baroclinic eddies, and changes in the tidal wind field near the surface. Our results extend the meteorological record of the northern hemisphere, substantiate the findings of previous investigations, and further illuminate the climatic impact of baroclinic eddies. (C) 2009 Elsevier Inc. All rights reserved. C1 [Hinson, David P.] SETI Inst, Carl Sagan Ctr, Mountain View, CA 94043 USA. [Hinson, David P.] Stanford Univ, Dept Elect Engn, Stanford, CA 94305 USA. [Wang, Huiqun] Smithsonian Astrophys Observ, Atom & Mol Phys Div, Cambridge, MA 02138 USA. RP Hinson, DP (reprint author), SETI Inst, Carl Sagan Ctr, 515 N Whisman Rd, Mountain View, CA 94043 USA. EM dhinson@seti.org FU NASA [NNX08AL24G, NNX07AR10G] FX Funding for this research was provided by NASA under Grants NNX08AL24G (Hinson) and NNX07AR10G (Wang) of the Mars Data Analysis Program. We relied on NASA's Navigation and Ancillary Information Facility (Acton, 1996) in various stages of data analysis. In preparing the manuscript we made use of the SAO/NASA Astrophysics Data System (http://adswww.harvard.edu/) and an Icarus LaTeX template created by R.A. Beyer, D.P. O'Brien, P. Withers, and G. Bart (http://rossbeyer.net/software/). NR 50 TC 22 Z9 22 U1 0 U2 11 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD MAR PY 2010 VL 206 IS 1 BP 290 EP 305 DI 10.1016/j.icarus.2009.08.019 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 560EH UT WOS:000274884300026 ER PT J AU DeVorkin, DH AF DeVorkin, David H. TI In Sputnik's Shadow: The President's Science Advisory Committee and Cold War America SO ISIS LA English DT Book Review C1 [DeVorkin, David H.] Smithsonian Inst, Natl Air & Space Museum, Div Space Hist, Washington, DC 20560 USA. RP DeVorkin, DH (reprint author), Smithsonian Inst, Natl Air & Space Museum, Div Space Hist, 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 0021-1753 J9 ISIS JI Isis PD MAR PY 2010 VL 101 IS 1 BP 268 EP 270 PG 3 WC History & Philosophy Of Science SC History & Philosophy of Science GA 592PG UT WOS:000277390900093 ER PT J AU Deutsch, J AF Deutsch, James TI Mystery, Violence, and Popular Culture SO JOURNAL OF AMERICAN FOLKLORE LA English DT Book Review C1 [Deutsch, James] Smithsonian Inst, Washington, DC 20560 USA. RP Deutsch, J (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 2 PU AMER FOLKLORE SOC PI ARLINGTON PA 4350 NORTH FAIRFAX DR, STE 640, ARLINGTON, VA 22203 USA SN 0021-8715 J9 J AM FOLKLORE JI J. Am. Folk. PD SPR PY 2010 VL 123 IS 488 BP 235 EP 236 PG 2 WC Folklore SC Arts & Humanities - Other Topics GA 586ZQ UT WOS:000276955700012 ER PT J AU Ubelaker, DH AF Ubelaker, Douglas H. TI Reanalysis and Reinterpretation in Southwestern Bioarchaeology 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 1 PU UNIV NEW MEXICO PI ALBUQUERQUE PA DEPT ANTHROPOLOGY, ALBUQUERQUE, NM 87131-1561 USA SN 0091-7710 J9 J ANTHROPOL RES JI J. Anthropol. Res. PD SPR PY 2010 VL 66 IS 1 BP 160 EP 160 PG 1 WC Anthropology SC Anthropology GA 580RY UT WOS:000276468500034 ER PT J AU Rivadeneira, MM Hernaez, P Baeza, JA Boltana, S Cifuentes, M Correa, C Cuevas, A del Valle, E Hinojosa, I Ulrich, N Valdivia, N Vasquez, N Zander, A Thiel, M AF Rivadeneira, Marcelo M. Hernaez, Patricio Baeza, J. Antonio Boltana, Sebastian Cifuentes, Mauricio Correa, Cristian Cuevas, Alejandra del Valle, Erasmo Hinojosa, Ivan Ulrich, Niklas Valdivia, Nelson Vasquez, Nelson Zander, Anke Thiel, Martin TI Testing the abundant-centre hypothesis using intertidal porcelain crabs along the Chilean coast: linking abundance and life-history variation SO JOURNAL OF BIOGEOGRAPHY LA English DT Article DE Abundant-centre hypothesis; Brown's principle; intertidal zone; macroecology; macrophysiology; Porcellanidae; sex ratio; size-temperature rule; Southeast Pacific ID PETROLISTHES-LAEVIGATUS ANOMURA; LIMPET COLLISELLA-SCABRA; THERMAL TOLERANCE LIMITS; GEOGRAPHIC RANGE LIMIT; EASTERN PACIFIC; BIOGEOGRAPHIC PATTERNS; REPRODUCTIVE-BIOLOGY; POPULATION-DYNAMICS; GENUS PETROLISTHES; CINCTIPES ANOMURA AB Aim The abundant-centre hypothesis (ACH) is based on the assumption that physiological constraints limit populations at the edges of their distributional range, yet the geographical variation of physiological performance or life-history traits has rarely been examined. Here we examine the applicability of the ACH in a marine system by testing whether physiological predictions are reflected in large-scale variations of life-history traits. Location The Chilean coast (18 degrees-42 degrees S), encompassing more than 2500 km along the Pacific coast of South America. Methods Five porcelain crab species (Petrolisthes granulosus, Petrolisthes laevigatus, Petrolisthes tuberculatus, Petrolisthes violaceus and Allopetrolisthes angulosus) were sampled on intertidal boulder beaches at 13 sampling sites. For each species and site we evaluated: (1) relative abundance (density), (2) maximum size, (3) size at maturity, (4) sex ratio, (5) proportion of ovigerous females, and (6) presence of recruits. The shape of the spatial distribution of each trait was evaluated statistically against the prediction of four hypothetical models (normal, ramped-south, ramped-north and abundant-edge). Results The relative abundance and life-history traits showed different spatial patterns among species. Relative abundance (across sites) was fitted by a normal model in only two species. No model fitted the spatial variation in body size and size at first maturity, which showed a slight but monotonic poleward increase in all species. Sex ratio showed a prominent hump-shaped pattern, with females prevailing in the centre of the ranges and males dominating towards the range boundaries; this pattern was statistically significant in three of the five studied species. The proportion of ovigerous females showed no clear latitudinal trends, and mature individuals were observed across most of the geographical range of the species. However, recruits tended to be absent towards the southern (poleward) boundaries of the distribution. Main conclusions The ACH does not apply to all species equally. The link between abundance and life-history traits is complex and variable among the porcelain crab species studied. Overall, the observed patterns were consistent with the idea that equatorward boundaries might be controlled by physiological restrictions mainly affecting adult survival, whereas poleward boundaries might be shaped by limitations in reproductive output and larval survival. Our results underline the importance of incorporating ecological, physiological and life-history studies in future tests of the ACH. C1 [Rivadeneira, Marcelo M.] Univ Catolica Norte, Fac Ciencias Mar, CEAZA, Coquimbo 1781412, Chile. [Rivadeneira, Marcelo M.] Pontificia Univ Catolica Chile, Fac Ciencias Biol, Dept Ecol, CASEB, Santiago, Chile. [Hernaez, Patricio] Univ Arturo Prat, Museo Mar, Iquique, Chile. [Hernaez, Patricio] Univ Costa Rica, UNIP CIMAR, Unidad Invest Pesquera & Acuicultura, San Jose, Costa Rica. [Baeza, J. Antonio] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Baeza, J. Antonio] Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. [Boltana, Sebastian; Cifuentes, Mauricio; Correa, Cristian; Cuevas, Alejandra; del Valle, Erasmo; Hinojosa, Ivan; Ulrich, Niklas; Valdivia, Nelson; Vasquez, Nelson; Zander, Anke; Thiel, Martin] Univ Catolica Norte, Fac Ciencias Mar, Dept Biol Marina, Coquimbo 1781412, Chile. RP Rivadeneira, MM (reprint author), Univ Catolica Norte, Fac Ciencias Mar, CEAZA, Larrondo 1281, Coquimbo 1781412, Chile. EM mrivadeneira@ucn.cl RI Valdivia, Nelson/C-3613-2009; Hernaez Bove, Patricio Alejandro/E-6375-2011; Hinojosa, Ivan Andres/B-6250-2013; Hinojosa, Ivan/P-1572-2016; OI Valdivia, Nelson/0000-0002-5394-2072; Hernaez Bove, Patricio Alejandro/0000-0002-3785-2050; Hinojosa, Ivan/0000-0002-9752-4374; Boltana, Sebastian/0000-0002-5195-0490; Baeza, Juan Antonio/0000-0002-2573-6773 FU FONDECYT [3980002, 11070147]; FONDAP-FONDECYT [1501-0001] FX We appreciate the logistical help provided by Catalina Correa during some of the field samplings, and the constructive comments from Bernardo Broitman, Esteban Emparanza and two anonymous referees. This research was funded by FONDECYT 3980002 (to M.T.), FONDECYT 11070147 (to M.M.R.) and FONDAP-FONDECYT 1501-0001. This is contribution number 804 from the Smithsonian Marine Station at Fort Pierce. NR 75 TC 20 Z9 20 U1 2 U2 24 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0305-0270 J9 J BIOGEOGR JI J. Biogeogr. PD MAR PY 2010 VL 37 IS 3 BP 486 EP 498 DI 10.1111/j.1365-2699.2009.02224.x PG 13 WC Ecology; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA 548GZ UT WOS:000273949700010 ER PT J AU DeBose, JL Nevitt, GA Dittman, AH AF DeBose, Jennifer L. Nevitt, Gabrielle A. Dittman, Andrew H. TI Rapid Communication: Experimental Evidence that Juvenile Pelagic Jacks (Carangidae) Respond Behaviorally to DMSP SO JOURNAL OF CHEMICAL ECOLOGY LA English DT Article DE Caranx hippos; Caranx melampygus; Chemical ecology; Dimethylsulfoniopropionate (DMSP); Foraging behavior; Pelagic fish; Sensory ecology ID GREAT-BARRIER-REEF; DIMETHYLSULFONIOPROPIONATE; FISH AB Dimethylsulfoniopropionate (DMSP) is produced by marine algae and released during foraging activity by zooplankton and fish. Pelagic fishes depend on patchily distributed foraging opportunities, and DMSP may be an important signaling molecule for these events. We have previously shown that the abundance of carangid jacks is positively associated with elevated DMSP levels over coral reefs in the Gulf of Mexico, suggesting that these fishes may use spatial and temporal variation in DMSP to locate foraging opportunities. Here, we extend this work by demonstrating that juveniles of two species of pelagic jack, crevalle jack, Caranx hippos, and bluefin trevally, C. melampygus, detect and respond to DMSP in a flow-through tank in the laboratory. Juveniles of these species showed elevated swimming activity in response to ecologically relevant concentrations of DMSP (10(-9) M). These results provide further evidence that this chemical may serve as a chemosensory cue for carangid species. C1 [DeBose, Jennifer L.; Nevitt, Gabrielle A.] Univ Calif Davis, Dept Neurobiol Physiol & Behav, Davis, CA 95616 USA. [Dittman, Andrew H.] NOAA Fisheries, NW Fisheries Sci Ctr, Seattle, WA USA. RP DeBose, JL (reprint author), Smithsonian Marine Stn, Ft Pierce, FL USA. EM debosej@si.edu FU PEO Scholar Award; NSF-GRF; NOAA Fisheries FX We thank the Oceanic Institute, specifically C. Laidley and staff, for providing bluefin trevally. We also thank P. Swanson, M. Havey, D. May, M. Rust, T. Scott, P. Plesha, and F. Sommers, of the Northwest Fisheries Science Center, NOAA, for help in acquiring and maintaining trevally. Thanks to Moody Gardens Aquarium, especially R. Drinnen, B. Christie and staff, B. Dailey, and M. Weber, for collecting and housing crevalle jacks. We also thank S. Strom (Shannon PointMarine Center) for GC use. Experiments were conducted under UCD ACUC #12050. Funding was provided by a PEO Scholar Award and by a NSFGRF (JLD) and by a grant from NOAA Fisheries (AHD). NR 10 TC 8 Z9 9 U1 0 U2 15 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0098-0331 J9 J CHEM ECOL JI J. Chem. Ecol. PD MAR PY 2010 VL 36 IS 3 BP 326 EP 328 DI 10.1007/s10886-010-9755-9 PG 3 WC Biochemistry & Molecular Biology; Ecology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology GA 568RI UT WOS:000275539800010 PM 20177745 ER PT J AU Bernasconi, MP Stanley, JD Caruso, C AF Bernasconi, Maria Pia Stanley, Jean-Daniel Caruso, Claudia TI Sybaris-Thuri-Copia Deltaic Settings in Calabria, Italy: Molluscs, Associated Biogenic Components, and Ecobiostratigraphy Applied to Archaeology SO JOURNAL OF COASTAL RESEARCH LA English DT Article DE Biofacies; biogenic components; Calabria; Copia; Crati Delta; ecobiostratigraphy; geoarchaeology; lithofacies; molluscs; port facilities; progradation; Sybaris; Thuri ID HARBOR AB The Greek and Roman coastal sites of Sybaris, Thuri, and Copia in Calabria, Italy, active from similar to 727 BC to about the third century AD, were buried by Crati Delta sediments and are now positioned inland similar to 2.5 km west of the present Gulf of Taranto coast. This study identifies biogenic components in two sediment cores of mid-Holocene to the present age, recovered in the Casa Bianca sector of the Sybaris archaeological park. Three biofacies are identified using primarily molluscs, along with associated faunas and vegetal components. The lower biofacies (older than 3600 BC to similar to 2700 BC, Neolithic), with moderate to well-represented faunas, indicates an open marine inner shelf environment. A midcore transitional biofacies (from similar to 2700 to similar to 2000 BC, late Neolithic), with meagre faunas and poorly preserved specimens, mixed with plant matter, was deposited in very high energy conditions close to shore. The upper biofacies (from similar to 2000 BC, early Bronze age to present) comprises even less fauna, mostly terrestrial, and was increasingly influenced by fluviodeltaic conditions; it includes the strata with Greek and Roman artefacts. The up-core sequence records evolution from marine to coastal, wetland, and then terrestrial environments, associated with active progradation seaward of the Crati Delta's coastal margin through time. This ecobiostratigraphic approach can assist archaeologists studying this region by identifying faunas that serve to interpret paleogeographic conditions that prevailed before, during, and after occupation of the three sites. C1 [Bernasconi, Maria Pia; Caruso, Claudia] Univ Calabria, Dipartimento Sci Terra, I-87036 Arcavacata Di Rende, CS, Italy. [Stanley, Jean-Daniel] Smithsonian Inst, MRC 121, Cities Sea Program, NMNH E 205, Washington, DC 20013 USA. RP Bernasconi, MP (reprint author), Univ Calabria, Dipartimento Sci Terra, I-87036 Arcavacata Di Rende, CS, Italy. EM bernasconi@unical.it; stanleyd@si.edu FU National Museum of Natural History, Smithsonian Institution, Washington, DC FX We are indebted to Eng. P. Mercuri (LAGIC Laboratory) for the successful recovery of the cores and to Drs. F. Scarciglia and S. Storino, both of the University of Calabria, for valuable advice concerning interpretations. of soil types and for laboratory assistance with core samples. We also express our appreciation to Dr. S. Luppino, Calabrian Antiquities Authority (Soprintendenza), for authorizations and kind encouragement to conduct research at the archaeological site. Constructive suggestions were given by two anonymous reviewers on an earlier version of the manuscript. Partial funding for the field work was provided by a grant from the National Museum of Natural History, Smithsonian Institution, Washington, DC. NR 24 TC 7 Z9 7 U1 0 U2 1 PU COASTAL EDUCATION & RESEARCH FOUNDATION PI LAWRENCE PA 810 EAST 10TH STREET, LAWRENCE, KS 66044 USA SN 0749-0208 J9 J COASTAL RES JI J. Coast. Res. PD MAR PY 2010 VL 26 IS 2 BP 377 EP 390 DI 10.2112/JCOASTRES-D-09-00091.1 PG 14 WC Environmental Sciences; Geography, Physical; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Physical Geography; Geology GA 578WV UT WOS:000276328400017 ER PT J AU Sekiguchi, T Ichikawa, K Takahashi, T Greenhill, L AF Sekiguchi, Toyokazu Ichikawa, Kazuhide Takahashi, Tomo Greenhill, Lincoln TI Neutrino mass from cosmology: impact of high-accuracy measurement of the Hubble constant SO JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS LA English DT Article DE neutrino masses from cosmology; cosmological parameters from CMBR; cosmological neutrinos; baryon acoustic oscillations ID ANGULAR POWER SPECTRUM; LENS TIME DELAYS; 2003 FLIGHT; SPACE-TELESCOPE; GALAXY NGC-4258; ANISOTROPY; PROBE; BOOMERANG; DISTANCE; CONSTRAINTS AB Non-zero neutrino mass would affect the evolution of the Universe in observable ways, and a strong constraint on the mass can be achieved using combinations of cosmological data sets. We focus on the power spectrum of cosmic microwave background (CMB) anisotropies, the Hubble constant H-0, and the length scale for baryon acoustic oscillations (BAO) to investigate the constraint on the neutrino mass, m(nu). We analyze data from multiple existing CMB studies (WMAP5, ACBAR, CBI, BOOMERANG, and QUAD), recent measurement of H-0 (SHOES), with about two times lower uncertainty (5%) than previous estimates, and recent treatments of BAO from the Sloan Digital Sky Survey (SDSS). We obtained an upper limit of m(nu) < 0.2 eV (95 % CL.), for a flat ACDM model. This is a 40% reduction in the limit derived from previous H-0 estimates and one-third lower than can be achieved with extant CMB and BAO data. We also analyze the impact of smaller uncertainty on measurements of H-0 as may be anticipated in the near term, in combination with CMB data from the Planck mission, and BAO data from the SDSS/BOSS program. We demonstrate the possibility of a 5 sigma detection for a fiducial neutrino films of 0.1 eV or a 95% upper limit of 0.04 eV for a fiducial of m(nu) = 0 eV. These constraints are about 50 % better than those achieved without external constraint. We further investigate the impact on modeling where the dark-energy equation of state is constant but not necessarily -1, or where a non-flat universe is allowed. In these cases, the next-generation accuracies of Planck, BOSS, and 1 % measurement of H-0 would all be required to obtain the limit m(nu) < 0.05 - 0.06 eV (95 % CL.) for the fiducial of m(nu) = 0 eV. The independence of systematics argues for pursuit of both BAO and H-0 measurements. C1 [Sekiguchi, Toyokazu] Univ Tokyo, Inst Cosm Ray Res, Kashiwa, Chiba 2778582, Japan. [Ichikawa, Kazuhide] Kyoto Univ, Dept Micro Engn, Kyoto 6068501, Japan. [Takahashi, Tomo] Saga Univ, Dept Phys, Saga 8408502, Japan. [Greenhill, Lincoln] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Sekiguchi, T (reprint author), Univ Tokyo, Inst Cosm Ray Res, Kashiwa, Chiba 2778582, Japan. EM sekiguti@icrr.u-tokyo.ac.jp; kazuhide@me.kyoto-u.ac.jp; tomot@cc.saga-u.ac.jp; greenhill@cfa.harvard.edu FU Japan Society for the Promotion of Science; Ministry of Education, Science, Sports, and Culture, Japan [19740145] FX We are very grateful to Ingyin Zaw and Marc Anera for useful comments on the draft. T.S. would like to thank the Japan Society for the Promotion of Science for financial support. This work is partially supported by Grant-in-Aid for Scientific research from the Ministry of Education, Science, Sports, and Culture, Japan, No. 19740145 (T.T.). NR 46 TC 14 Z9 14 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 1475-7516 J9 J COSMOL ASTROPART P JI J. Cosmol. Astropart. Phys. PD MAR PY 2010 IS 3 AR 015 DI 10.1088/1475-7516/2010/03/015 PG 21 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 575XG UT WOS:000276103000019 ER PT J AU Mozdzer, TJ Zieman, JC AF Mozdzer, Thomas J. Zieman, Joseph C. TI Ecophysiological differences between genetic lineages facilitate the invasion of non-native Phragmites australis in North American Atlantic coast wetlands SO JOURNAL OF ECOLOGY LA English DT Article DE chlorophyll; conspecific; genotype; invasive; N; native; photosynthesis; Phragmites; physiology; SLA ID SOLIDAGO-GIGANTEA ASTERACEAE; CLONE-SPECIFIC DIFFERENCES; COMMON REED; PHOTOSYNTHETIC CHARACTERISTICS; PHENOTYPIC PLASTICITY; CRYPTIC INVASION; TIDAL MARSHES; PLOIDY LEVEL; NITROGEN; POPULATIONS AB 1. Over the last century, native Phragmites australis lineages have been almost completely replaced along the North American Atlantic coast by an aggressive lineage originating from Eurasia. Understanding the mechanisms that facilitate biological invasions is critical to better understand what makes an invasive species successful. 2. Our objective was to determine what makes the introduced lineage so successful in the study area by specifically investigating if morphological and ecophysiological differences exist between native and introduced genetic lineages of P. australis. We hypothesized a priori that due to phenotypic differences and differences in plant nitrogen (N) content between lineages, the introduced lineage would have a greater photosynthetic potential. 3. In situ ecophysiological and morphological data were collected for 2 years in a mid-Atlantic tidal marsh and in a glasshouse experiment. We measured photosynthetic parameters (A(max), water use efficiency, stomatal conductance) using infrared gas analysis, in conjunction with ecophysiological and morphological parameters [specific leaf area (SLA), leaf area, chlorophyll content, N content]. 4. Introduced P. australis maintained 51% greater rates of photosynthesis and up to 100% greater rates of stomatal conductance which are magnified by its 38-83% greater photosynthetic canopy compared to the native type. The introduced lineage also had a significantly greater SLA and N content. Glasshouse-grown plants and naturally occurring populations demonstrated similar trends in ecophysiological characteristics, verifying the heritability of these differences. These ecophysiological differences, when combined with an extended growing season, provide the mechanism to explain the success of introduced P. australis in North America. 5. Our findings suggest the native type is a low-nutrient specialist, with a more efficient photosynthetic mechanisms and lower N demand, whereas the introduced type requires nearly four times more N than the native type to be an effective competitor. 6. Synthesis. Our study is the first to combine field and laboratory data to explain a biological invasion attributed to ecophysiological differences between genetic lineages. Our data corroborates earlier work suggesting anthropogenic modification of wetland environments has provided the state change necessary for the success of introduced P. australis. Finally, our results suggest that genotypic differences within species merit further investigations, especially when related to biological invasions. C1 [Mozdzer, Thomas J.; Zieman, Joseph C.] Univ Virginia, Dept Environm Sci, Charlottesville, VA 22904 USA. RP Mozdzer, TJ (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM mozdzert@si.edu RI Mozdzer, Thomas/G-4372-2011; Mozdzer, Thomas/A-3599-2014 OI Mozdzer, Thomas/0000-0002-1053-0967 FU NSF [DEB 0621014] FX We would like to thank the NSF grant DEB 0621014 for funding, J. W. Snyder, M. Takahashi and B. C. Curtis for field and laboratory assistance, as well as T. M. Smith, M. Lerdau, J. A. Langley and two anonymous referees for their critical review of an earlier version of the manuscript. NR 56 TC 55 Z9 56 U1 5 U2 50 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 MAR PY 2010 VL 98 IS 2 BP 451 EP 458 DI 10.1111/j.1365-2745.2009.01625.x PG 8 WC Plant Sciences; Ecology SC Plant Sciences; Environmental Sciences & Ecology GA 548HF UT WOS:000273950400020 ER PT J AU Altshuler, DL Dudley, R Heredia, SM McGuire, JA AF Altshuler, D. L. Dudley, R. Heredia, S. M. McGuire, J. A. TI Allometry of hummingbird lifting performance SO JOURNAL OF EXPERIMENTAL BIOLOGY LA English DT Article DE allometry; body size; elevation; flight; load-lifting; maximum performance; muscle power output ID FLIGHT PERFORMANCE; ELEVATIONAL GRADIENTS; HOVERING PERFORMANCE; REVOLVING WINGS; METABOLIC-RATES; GAS-MIXTURES; POWER OUTPUT; TAKE-OFF; AERODYNAMICS; PHYSIOLOGY AB Vertical lifting performance in 67 hummingbird species was studied across a 4000 m elevational gradient. We used the technique of asymptotic load-lifting to elicit maximum sustained muscle power output during loaded hovering flight. Our analysis incorporated direct measurements of maximum sustained load and simultaneous wingbeat kinematics, together with aerodynamic estimates of mass-specific mechanical power output, all within a robust phylogenetic framework for the Trochilidae. We evaluated key statistical factors relevant to estimating slopes for allometric relationships by performing analyses with and without phylogenetic information, and incorporating species-specific measurement error. We further examined allometric relationships at different elevations because this gradient represents a natural experiment for studying physical challenges to animal flight mechanics. Maximum lifting capacity (i.e. vertical force production) declined with elevation, but was either isometric or negatively allometric with respect to both body and muscle mass, depending on elevational occurrence of the corresponding taxa. Maximum relative muscle power output exhibited a negative allometry with respect to muscle mass, supporting theoretical predictions from muscle mechanics. C1 [Altshuler, D. L.] Univ Calif Riverside, Dept Biol, Riverside, CA 92521 USA. [Dudley, R.; McGuire, J. A.] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. [Dudley, R.] Smithsonian Trop Res Inst, Balboa, Panama. [Heredia, S. M.] Univ Calif Riverside, Dept Bot & Plant Sci, Riverside, CA 92521 USA. [McGuire, J. A.] Univ Calif Berkeley, Museum Vertebrate Zool, Berkeley, CA 94720 USA. RP Altshuler, DL (reprint author), Univ Calif Riverside, Dept Biol, 900 Univ Ave, Riverside, CA 92521 USA. EM douga@ucr.edu OI Altshuler, Douglas/0000-0002-1364-3617 FU National Institutes of Health [F32 NS46221]; National Science Foundation [DEB 0330750, DEB 0543556] FX We thank Ted Garland and Tony Ives for advice on statistical procedures, and Chris Barber, Richard Gibbons and numerous volunteers from the Earthwatch Institute for field assistance. Robbie Buchwald, Chris Clark, Maria Jose Fernandez, Jim Marden, Kenneth Welch and Chris Witt kindly commented on the manuscript. This research was supported by a fellowship from the National Institutes of Health (F32 NS46221) and by grants from the National Science Foundation (DEB 0330750 and DEB 0543556). Deposited in PMC for release after 12 months. NR 49 TC 27 Z9 27 U1 3 U2 25 PU COMPANY OF BIOLOGISTS LTD PI CAMBRIDGE PA BIDDER BUILDING CAMBRIDGE COMMERCIAL PARK COWLEY RD, CAMBRIDGE CB4 4DL, CAMBS, ENGLAND SN 0022-0949 J9 J EXP BIOL JI J. Exp. Biol. PD MAR 1 PY 2010 VL 213 IS 5 BP 725 EP 734 DI 10.1242/jeb.037002 PG 10 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 554OL UT WOS:000274444200015 PM 20154187 ER PT J AU Gunasekera, SP Miller, MW Kwan, JC Luesch, H Paul, VJ AF Gunasekera, Sarath P. Miller, Margaret W. Kwan, Jason C. Luesch, Hendrik Paul, Valerie J. TI Molassamide, a Depsipeptide Serine Protease Inhibitor from the Marine Cyanobacterium Dichothrix utahensis SO JOURNAL OF NATURAL PRODUCTS LA English DT Article ID ELASTASE INHIBITORS; NATURAL-PRODUCTS; DOLASTATIN-13; N-GREATER-THAN-3; SPECTRA; ANALOG AB A new dolastatin 13 analogue, molassamide (1), was isolated from cyanobacterial assemblages of Dichothrix utahliensis collected from the Molasses Reef, Key Largo, Florida, and from Brewer's Bay, St. Thomas, U.S. Virgin Islands. This is the first peptide reported from the cyanobacterial genus Dichothrix and the first natural product isolated from marine Dichothrix spp. Its planar structure was determined by NNR spectroscopic techniques, and the configurations of the asymmetric centers, were assigned after chiral HPLC analysis of the hydrolysis products. The depsipeptide I exhibited protease-inhibitory activity, with IC(50) values of 0.032 and 0.234 mu M against elastase and chymotrypsin, respectively. There was no apparent inhibition of trypsin at 10 mu M the highest concentration tested. C1 [Gunasekera, Sarath P.; Paul, Valerie J.] Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. [Miller, Margaret W.] NOAA, SE Fisheries Sci Ctr, Miami, FL 33149 USA. [Kwan, Jason C.; Luesch, Hendrik] Univ Florida, Dept Med Chem, Gainesville, FL 32610 USA. RP Paul, VJ (reprint author), Smithsonian Marine Stn Ft Pierce, 701 Seaway Dr, Ft Pierce, FL 34949 USA. EM paul@si.edu RI Kwan, Jason/F-9589-2010 OI Kwan, Jason/0000-0001-9933-1536 FU National Oceanic and Atmospheric Administration [NA05NOS4781194]; U.S. Geological Survey [07ERAG0079] FX This research was supported in part by the National Oceanic and Atmospheric Administration's ECOHAB program (the Ecology and Oceanography of Harmful Algae Blooms), Project NA05NOS4781194, and Coral Reef Conservation Program Research in the USVI was supported by the U.S. Geological Survey Cooperative Agreement No. 07ERAG0079 with funding from the Eastern Region State Partnership Program. NR 18 TC 25 Z9 25 U1 3 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 MAR PY 2010 VL 73 IS 3 SI SI BP 459 EP 462 DI 10.1021/np900603f PG 4 WC Plant Sciences; Chemistry, Medicinal; Pharmacology & Pharmacy SC Plant Sciences; Pharmacology & Pharmacy GA 573CC UT WOS:000275885000030 PM 20020755 ER PT J AU Kwan, JC Teplitski, M Gunasekera, SP Paul, VJ Luesch, H AF Kwan, Jason C. Teplitski, Max Gunasekera, Sarath P. Paul, Valeric J. Luesch, Hendrik TI Isolation and Biological Evaluation of 8-epi-Malyngamide C from the Floridian Marine Cyanobacterium Lyngbya majuscula SO JOURNAL OF NATURAL PRODUCTS LA English DT Article ID HARE STYLOCHEILUS-LONGICAUDA; SECONDARY METABOLITES; JUVENILE RABBITFISH; FEEDING PREFERENCES; BURSATELLA-LEACHII; CHEMICAL DEFENSES; MALYNGAMIDE-X; COLLECTION; ACID; CONSTRUCTION AB A new stereoisomer of malyngamide C, 8-epi-malynoamide C (1), and the known compound lyngbic acid 1(4E,7S)-7methoxytetradec-4-enoic acid] were isolated front I sample of Lyngbya majuscula collected near Bush Key, Dry Tortugas, Florida. The structure of I was determined by NMR and MS experiments. The absolute configuration of I was determined by Selective Mitsunobu inverstion of C-8 to give malyngamide C, as determined by NMR, MS, and comparison of specific rotation. Roth I and malyngamide C were found to be cytotoxic to HT29 colon cancer cells (IC(50) 1 5.4 and 5.2 mu M, respectively) and to inhibit bacterial quorum sensing in a reporter gene assay. C1 [Kwan, Jason C.; Luesch, Hendrik] Univ Florida, Dept Med Chem, Gainesville, FL 32610 USA. [Teplitski, Max] Univ Florida, Dept Soil & Water Sci, Inst Food & Agr Sci, Genet Inst, Gainesville, FL 32610 USA. [Gunasekera, Sarath P.; Paul, Valeric 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 Kwan, Jason/F-9589-2010 OI Kwan, Jason/0000-0001-9933-1536 FU National Institutes of Health, NIGMS [P41GN1806210]; University of Florida College of Pharmacy FX This research was supported by the National Institutes of Health, NIGMS Grant P41GN1806210, and the University of Florida College of Pharmacy. NR 34 TC 39 Z9 39 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 MAR PY 2010 VL 73 IS 3 SI SI BP 463 EP 466 DI 10.1021/np900614n PG 4 WC Plant Sciences; Chemistry, Medicinal; Pharmacology & Pharmacy SC Plant Sciences; Pharmacology & Pharmacy GA 573CC UT WOS:000275885000031 PM 20166701 ER PT J AU MacFadden, BJ Kirby, MX Rincon, A Montes, C Moron, S Strong, N Jaramillo, C AF MacFadden, Bruce J. Kirby, Michael X. Rincon, Aldo Montes, Camilo Moron, Sara Strong, Nikki Jaramillo, Carlos TI EXTINCT PECCARY "CYNORCA" OCCIDENTALE (TAYASSUIDAE, TAYASSUINAE) FROM THE MIOCENE OF PANAMA AND CORRELATIONS TO NORTH AMERICA SO JOURNAL OF PALEONTOLOGY LA English DT Article ID MIDDLE MIOCENE; MAMMALS; ATLANTIC AB Recently collected specimens of the extinct tayassuine peccary "Cynorca" occidentale (and another indeterminant tayassuid) are described from new excavations along the southern reaches of the Panama Canal. Fossil peccaries were previously unknown from Panama, and these new tayassuid specimens therefore add to the extinct mammalian biodiversity in this region. "Cynorea" occidentale Occurs ill situ in the Centenario Fauna (new name) from both the upper part of the Culebra Formation and overlying Cucaracha Formation, thus encompassing a stratigraphic interval that includes both of these formations and the previously described and more restricted Gaillard Cut Local Fauna. "Cynorca" occidentale is a primitive member of the clade that gives rise to modern tayassuines in the New World. Diagnostic characters for "C." occidentale include a retained primitive M 1, reduced M3, and shallow mandible, and this species is small relative to most other extinct and modern tayassiune peccaries. Based oil the closest biostratigraphic comparisions (Maryland, Florida, Texas, and California), the presence of "C." occidentale indicates an interval Of uncertain duration within the early Hemingfordian (He1) to early Barstovian (Ba 1) land mammal ages (early to middle Miocene) for the Centenario Fauna, between about 19 and 14.8 million years ago. Based on what is known of the modern ecology of tayassuines and previous paleoecological interpretations for Panama, "C." occidentale likely Occupied a variety of environments, ranging from forested to open Country habitat mosaics and fed oil the diverse array of available plants. C1 [MacFadden, Bruce J.] Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA. [MacFadden, Bruce J.] Natl Sci Fdn, Div Res Learning, EHR, Arlington, VA 22230 USA. [Kirby, Michael X.] EPG Inc, Phoenix, AZ 85018 USA. [Rincon, Aldo; Montes, Camilo; Moron, Sara; Strong, Nikki; Jaramillo, Carlos] Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archaeol, Balboa, Ancon, Panama. RP MacFadden, BJ (reprint author), Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA. EM bmacfadd@flmnh.ufl.edu OI Montes, Camilo/0000-0002-3553-0787 FU UF 2007 Research Opportunity; National Science Foundation [OISE 0638810, EAR 0642528, EAR 0824299]; STRI-Tupper Paleontological Fund; STRI-Panama Canal Authority Fund; Ricardo Toyota, Panama; Secretaria Nacional de Ciencia, Tecnologia e Innovacion (SENACYT), Panama FX We thank J. Bourque, J. Mason, and J. Mathis (UF) who prepared the specimens in the laboratory, D. Bohaska (USNM), J.. Galkin (AMNH), and C. McCaffrey (UF-M) for access to relevant research collections, and J. Hermanson (Cornell University) and S. K. Bell (AMNH) for help with, respectively, anatomical terminology and taxonomic nomenclature. K. Church and R. Hulbert, Jr., read ail earlier version of the manuscript and made helpful comments for its improvement. We thank the Autoridad del Canal de Panama (ACP) for assess to relevant fossil sites. This research was Supported by UF 2007 Research Opportunity Grant; National Science Foundation grants OISE 0638810, EAR 0642528, and EAR 0824299; STRI-Tupper Paleontological Fund; STRI-Panama Canal Authority Fund; Ricardo Toyota, Panama; and Secretaria Nacional de Ciencia, Tecnologia e Innovacion (SENACYT), Panama. This is UF Contribution to Paleobiology number 612. Any opinions, findings, conclusions, or recommendations expressed in this paper are those of the authors and do not necessarily reflect the views of the National Science Foundation. NR 52 TC 20 Z9 22 U1 1 U2 8 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 MAR PY 2010 VL 84 IS 2 BP 288 EP 298 PG 11 WC Paleontology SC Paleontology GA 570PA UT WOS:000275689000007 ER PT J AU O'dea, A Ostrovsky, AN Rodriguez, F AF O'dea, Aaron Ostrovsky, Andrew N. Rodriguez, Felix TI Embryonic brooding and clonal propagation in tropical eastern Pacific cupuladriid bryozoans SO JOURNAL OF THE MARINE BIOLOGICAL ASSOCIATION OF THE UNITED KINGDOM LA English DT Article DE embryonic brooding; clonal propagation; tropical eastern Pacific; cupuladriid bryozoans ID FOSSIL LUNULITIDAE BRYOZOA; LIFE-HISTORY VARIATION; NEOGENE CUPULADRIIDAE; SELENARIA BRYOZOA; LIVING COLONIES; OPPOSITE SIDES; CHEILOSTOMATA; PANAMA; ISTHMUS; AMERICA AB Colonial invertebrates often mix sexual and asexual methods of propagation, and a comprehensive understanding of both is required for life history study. The asexual cloning of new colonies in cupuladriid bryozoans is much better studied than the formation of new colonies by sexual reproduction. As such, the relative investments of sexual and asexual modes of propagation remain uncertain. This preliminary study explores patterns of embryonic brooding as a measure of investment into sexual reproduction. We conduct a survey of quantity and arrangement of embryos in tropical eastern Pacific cupuladriid colonies and compare this to the frequency of cloning. Species populations show considerable variation in embryonic brooding. Patterns of brooding, both across and within species strongly support the hypothesis that as cloning increases, investment into sexual reproduction decreases. We find preliminary evidence that individual cupuladriid colonies that propagate sexually may senesce like solitary organisms, while species that regularly clone only appear to experience senescence at the level of the zooid. C1 [O'dea, Aaron; Rodriguez, Felix] Smithsonian Trop Res Inst, Panama City, Panama. [Ostrovsky, Andrew N.] St Petersburg State Univ, Fac Biol & Soil Sci, Dept Invertebrate Zool, St Petersburg 199034, Russia. [Ostrovsky, Andrew N.] Univ Vienna, Dept Palaeontol, Fac Earth Sci Geog & Astron, Geozentrum, A-1090 Vienna, Austria. RP O'dea, A (reprint author), Smithsonian Trop Res Inst, MRC 0580-01,Apartado 0843-03092, Panama City, Panama. EM odeaa@si.edu RI O'Dea, Aaron/D-4114-2011; Ostrovsky, Andrew/D-6439-2012 OI Ostrovsky, Andrew/0000-0002-3646-9439 FU Secretaria Nacional de Ciencia, Tecnologia e Innovacion (SENACYT); National Science Foundation [EAR03-45471]; Smithsonian Tropical Research Institute; Austrian Science Fund [P19337-B17]; Russian Foundation for Basic Research (RFBR) [07-04-00928a]; STRI FX The Secretaria Nacional de Ciencia, Tecnologia e Innovacion (SENACYT) funded the project. A. O'Dea was supported by the Tupper fellowship programme at STRI and National Science Foundation grant EAR03-45471. F. Rodriguez was supported by the Smithsonian Tropical Research Institute. A. Ostrovsky would like to thank Austrian Science Fund (FWF, grant P19337-B17) and Russian Foundation for Basic Research (RFBR, grant 07-04-00928a) for financial support. We would also like to thank Eldredge Bermingham and Harilaos Lessios from STRI for additional funds. NR 33 TC 2 Z9 2 U1 0 U2 2 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0025-3154 J9 J MAR BIOL ASSOC UK JI J. Mar. Biol. Assoc. U.K. PD MAR PY 2010 VL 90 IS 2 BP 291 EP 299 DI 10.1017/S0025315409000940 PG 9 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 584PP UT WOS:000276765000010 ER PT J AU Bravo, A Harms, KE Emmons, LH AF Bravo, Adriana Harms, Kyle E. Emmons, Louise H. TI Puddles created by geophagous mammals are potential mineral sources for frugivorous bats (Stenodermatinae) in the Peruvian Amazon SO JOURNAL OF TROPICAL ECOLOGY LA English DT Article DE Amazonia; bats; geophagy; mineral-rich water sources; licks; sodium; Stenodermatinae ID BIG BROWN BATS; FRUIT BATS; ELEMENTAL COMPOSITION; SOIL CHARACTERISTICS; EPTESICUS-FUSCUS; AVIAN GEOPHAGY; CALCIUM; PHYLLOSTOMIDAE; AVAILABILITY; REPRODUCTION AB Natural licks are activity hotspots for frugivorous bats in the Peruvian Amazon. Large numbers of frugivorous bats congregate at licks to drink water. Because most Amazonian soils are relatively poor in nutrients, plants may contain low concentrations of some nutrients; consequently, frugivorous bats may face nutrient limitations. Accordingly, a potential explanation for lick visitation by bats is to obtain key limited resources. We assessed this hypothesis by comparing concentrations of cations (Ca, K, Mg, Na) in water at three licks and associated non-lick sites across years and seasons at Los Amigos Conservation Concession in south-eastern Peru. We also examined bat activity patterns between lick and non-lick sites. Regardless of the season, at licks > 10 bats per net h(-1) were captured compared with forest and gap sites where < 1 bat per net h(-1) was capture. At licks bats belonged primarily to the subfamily Stenodermatinae and over 70% were reproductive females. Although calcium magnesium and potassium concentrations varied across water sources sodium concentrations were consistently higher inn lick water (> 500 ppm) compared with creeks and oxbow lakes (<2 ppm) across seasons. Therefore, since sodium is one of the most limiting nutrients for vertebrates in the tropics, licks may function as sources of sodium (or other elements) for bats. In any case, licks are reliable potential sources of sodium in the south-eastern Peruvian Amazon an otherwise mineral-poor landscape. C1 [Bravo, Adriana; Harms, Kyle E.] Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA. [Harms, Kyle E.] Smithsonian Trop Res Inst, Balboa, Panama. [Emmons, Louise H.] Smithsonian Inst, Div Mammals NHB390, Washington, DC 20013 USA. RP Bravo, A (reprint author), Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA. EM abravo1@tigers.lsu.edu FU Amazon Conservation Association; American Society of Bat Conservation International; Graduate Student Association - Biograds of Louisiana State University (LSU); Idea Wild; Louisiana Office of Environmental Education; LSU Graduate School; Rufford Small Grants; U.S. National Science Foundation FX We extend our gratitude to the Peruvian Institute Of Natural Resources (INRENA) for providing the research permits to do this study. For help in the field we thank the ACCA rangers, Y. Arteaga. R. Baez, M. Bravo. N. Castro, F. Carrasco, M. Cruz, Z. Ordonez, J. Ramos, A. L. Rodales, M, Rodriguez, K. Salas. W. Torres and especially J. Rios. We also thank J. Eberhard, M. Hafner, J. Janovec. C. Meyer. N. Pitman, K. Stevens, M. Tobler and J. Yavitt for their comments on the proposal or for help with logistics of the study. We are grateful to S. Claramunt. J. Myers, L. Reid. C. Voigt and two anonymous reviewers for their comments on the manuscript. Financial support was provided by the Amazon Conservation Association (graduate student grant and seed grant award), American Society of Bat Conservation International, Graduate Student Association - Biograds of Louisiana State University (LSU), Idea Wild, Louisiana Office of Environmental Education, LSU Graduate School, Rufford Small Grants and the U.S. National Science Foundation. NR 55 TC 16 Z9 16 U1 1 U2 13 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0266-4674 J9 J TROP ECOL JI J. Trop. Ecol. PD MAR PY 2010 VL 26 BP 173 EP 184 DI 10.1017/S0266467409990472 PN 2 PG 12 WC Ecology SC Environmental Sciences & Ecology GA 561NZ UT WOS:000274986000005 ER PT J AU Dorsey, CL Dennis, P Fascetti, AJ Wood, T Brown, JL AF Dorsey, Candice L. Dennis, Patricia Fascetti, Andrea J. Wood, Thomas Brown, Janine L. TI HYPONMINOACIDEMIA IS NOT ASSOCIATED WITH ULCERATIVE LESIONS IN BLACK RHINOCEROSES, DICEROS BICORNIS SO JOURNAL OF ZOO AND WILDLIFE MEDICINE LA English DT Article DE Amino acids; black rhinoceros; Diceros bicornis; hypoaminoacidemia; skin lesions; superficial necrolytic dermatitis ID SUPERFICIAL NECROLYTIC DERMATITIS; MIGRATORY ERYTHEMA; HEPATOCUTANEOUS SYNDROME; DOGS; DISEASE AB Ulcerative oral and skin lesions have become an issue of concern for the health of the managed black rhinoceros (rhino) (Diceros bicornis) populations. Lesions exhibited by the black rhino are clinically similar to those observed in other species with superficial necrolytic dermatitis (SND). One biochemical alteration in dogs with SND is severe hypoaminoacidemia, and nearly all cases are fatal. The objective of this study was to determine if black rhinos with analogous lesions exhibit a similar hypoaminoacidemia. Amino acid concentrations were measured in monthly plasma samples collected for 1 yr from black rhinos with (n = 4) and without (n = 34) lesions clinically consistent with SND. The rhinos with skin and/or oral lesions were zoo born males, ages 2, 6, 17, and 23 yr, from four different facilities. Three rhinos recovered from skin (n = 2) and oral lesions (n = 1). However, the one male with both skin and oral lesions died with the disease. None of the affected black rhinos exhibited a decrease in any of the amino acids evaluated or for total amino acid concentrations (P > 0.05). Based on the absence of hypoaminoacidemia and the comparatively low mortality rate in rhinos with lesions, it appears that this syndrome is not entirely consistent with SND observed in other species. These data will be useful for future assessments of rhino nutritional status and other potential metabolic diseases. C1 [Dorsey, Candice L.; Brown, Janine L.] Smithsonian Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA 22630 USA. [Dorsey, Candice L.; Wood, Thomas] George Mason Univ, Dept Environm Sci & Publ Policy, Fairfax, VA 22030 USA. [Dennis, Patricia] Cleveland Metropk Zoo, Cleveland, OH 44109 USA. [Fascetti, Andrea J.] Univ Calif Davis, Sch Vet Med, Dept Mol Biosci, Davis, CA 95616 USA. RP Dorsey, CL (reprint author), Smithsonian Natl Zool Pk, Conservat & Res Ctr, Smithsonian Natl Zool Pk,1500 Remount Dr, Front Royal, VA 22630 USA. EM cdorsey@aza.org RI Dennis, Patricia/A-2081-2015 FU Conservation Endowment Fund of the Association of Zoos and Aquariums; International Rhino Foundation FX The authors wish to thank the keepers and veterinarians at the following institutions who collected plasma samples for this study: Brookfield Zoological Park, Busch Gardens Tampa Bay, Cincinnati Zoo and Botanical Garden, Cleveland Metroparks Zoo, Dallas Zoo, Disney's Animal Kingdom, Denver Zoological Park, The Kansas City Zoo, Lee Richardson Zoo, Miami Metrozoo, Milwaukee County Zoo, Pittsburgh Zoo and Aquarium, Potter Park Zoo, Racine Zoological Park, San Antonio Zoo, and St. Louis Zoo. The authors would also like to thank Dr. Zengshou Yu from the Amino Acid Laboratory, Department of Molecular Biosciences, School of Veterinary Medicine at the University of California, Davis, for plasma sample analyses. Funding for this study was generously provided by the Conservation Endowment Fund of the Association of Zoos and Aquariums and the International Rhino Foundation. NR 22 TC 2 Z9 2 U1 1 U2 5 PU AMER ASSOC ZOO VETERINARIANS PI YULEE PA 581705 WHITE OAK ROAD, YULEE, FL 32097 USA SN 1042-7260 J9 J ZOO WILDLIFE MED JI J. Zoo Wildl. Med. PD MAR PY 2010 VL 41 IS 1 BP 22 EP 27 DI 10.1638/2008-0188.1 PG 6 WC Veterinary Sciences SC Veterinary Sciences GA 580QL UT WOS:000276464200004 PM 20722250 ER PT J AU Sheehy, D AF Sheehy, Daniel TI The "invention" of the indigenous music of Mexico: Anthropology and history of the cultural politics of the twentieth century SO LATIN AMERICAN MUSIC REVIEW-REVISTA DE MUSICA LATINOAMERICANA LA English DT Book Review C1 [Sheehy, Daniel] Smithsonian Inst, Washington, DC 20560 USA. RP Sheehy, D (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 3 PU UNIV TEXAS PRESS PI AUSTIN PA JOURNAL DIV, 2100 COMAL, AUSTIN, TX 78722 USA SN 0163-0350 J9 LAT AM MUSIC REV JI Lat. Am. Music Rev.-Rev. Music Latinoam. PD SPR-SUM PY 2010 VL 31 IS 1 BP 131 EP 135 PG 5 WC Music SC Music GA 653GN UT WOS:000282077300008 ER PT J AU Freeman, EW Abbondanza, FN Meyer, JM Schulte, BA Brown, JL AF Freeman, Elizabeth W. Abbondanza, F. Nicole Meyer, Jordana M. Schulte, Bruce A. Brown, Janine L. TI A simplified method for monitoring progestagens in African elephants under field conditions SO METHODS IN ECOLOGY AND EVOLUTION LA English DT Article DE enzyme immunoassay; faeces; hormone extraction; Loxodonta africana; non-invasive; progestagens ID LOXODONTA-AFRICANA; OVARIAN-FUNCTION; PREGNANCY; URINARY; ENDOCRINOLOGY; HORMONE; MUSTH; IMMUNOCONTRACEPTION; CONTRACEPTION; PROGESTERONE AB 1. Hormone analyses are frequently used to support management of wildlife; however, current techniques are not very field-friendly. In situ hormone monitoring is often expensive, time consuming and logistically difficult. Thus, a new method for assessing ovarian cycle activity non-invasively in free-ranging African elephants was developed. 2. The technique involves handshaking faecal samples in common organic solvents, use of environmentally stable antibody-coated microtitre plates and assessment of progestagen concentrations based on a visual colour change. 3. Studies using ex situ African elephants determined that handshaking faeces in a solution of isopropyl alcohol was effective for extracting the faecal progestagens (efficiency > 90%). 4. Antibody-coated plates were stable for up to 3 months under a range of temperatures (4 to > 38 degrees C) and the resulting faecal oestrous cycle progestagen profiles corresponded significantly to those of serum(r = 0.89, P < 0.01). 5. This field-friendly technique provided qualitative hormone data without the need for expensive equipment. Although developed for progestagen analyses in elephants, this approach should be adaptable to other steroids in a myriad of species. As such, it could facilitate how hormones are measured in species under field conditions and provide new tools for making sensible conservation management decisions. C1 [Freeman, Elizabeth W.; Abbondanza, F. Nicole; Meyer, Jordana M.; Brown, Janine L.] Conservat & Res Ctr, Ctr Species Survival, Front Royal, VA 22630 USA. [Freeman, Elizabeth W.] George Mason Univ, New Century Coll, Fairfax, VA 22030 USA. [Meyer, Jordana M.; Schulte, Bruce A.] Georgia So Univ, Dept Biol, Statesboro, GA 30460 USA. [Schulte, Bruce A.] Western Kentucky Univ, Dept Biol, Bowling Green, KY 42101 USA. RP Freeman, EW (reprint author), Conservat & Res Ctr, Ctr Species Survival, Natl Zool Pk, Front Royal, VA 22630 USA. EM efreeman@gmu.edu FU Association of Zoos and Aquarium; International Elephant Foundation; Smithsonian's Walcott Endowment; Siemens Medical Solutions Diagnostics FX We thank the staff at Indianapolis Zoo, Maryland Zoo at Baltimore, Nashville Zoo at Grassmere, Riddle's Elephant & Wildlife Sanctuary, Virginia Zoo, and Wildlife Safari for collecting samples for this study. Funding was generously provided by the Association of Zoos and Aquarium's Conservation Endowment Fund/Disney Wildlife Conservation Fund, International Elephant Foundation, Smithsonian's Walcott Endowment and Siemens Medical Solutions Diagnostics. This research adhered to the ASAB/ABS Guidelines for the Use of Animals in Research and met with IACUC approval at the National Zoological Park's Conservation & Research Center and at each facility which collected samples. NR 25 TC 10 Z9 10 U1 0 U2 7 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 2041-210X J9 METHODS ECOL EVOL JI Methods Ecol. Evol. PD MAR PY 2010 VL 1 IS 1 BP 86 EP 91 DI 10.1111/j.2041-210X.2009.00004.x PG 6 WC Ecology SC Environmental Sciences & Ecology GA 742BS UT WOS:000288913700010 ER PT J AU Gaither, MR Bowen, BW Toonen, RJ Planes, S Messmer, V Earle, J Robertson, DR AF Gaither, Michelle R. Bowen, Brian W. Toonen, Robert J. Planes, Serge Messmer, Vanessa Earle, John Robertson, D. Ross TI Genetic consequences of introducing allopatric lineages of Bluestriped Snapper (Lutjanus kasmira) to Hawaii SO MOLECULAR ECOLOGY LA English DT Article DE alien species; bottleneck; introductions; invasion biology; mtDNA; Marquesas; nuclear DNA; Papahanaumokuakea; Society Islands ID ALLELE FREQUENCY DATA; CORAL-REEF FISH; REPRODUCTIVE ISOLATION; POPULATION-GENETICS; BIOLOGICAL INVASIONS; PROPAGULE PRESSURE; SPECIES INVASIONS; COMPUTER-PROGRAM; MULTIPLE SOURCES; DIFFERENTIATION AB A half century ago the State of Hawaii began a remarkable, if unintentional, experiment on the population genetics of introduced species, by releasing 2431 Bluestriped Snappers (Lutjanus kasmira) from the Marquesas Islands in 1958 and 728 conspecifics from the Society Islands in 1961. By 1992 L. kasmira had spread across the entire archipelago, including locations 2000 km from the release site. Genetic surveys of the source populations reveal diagnostic differences in the mtDNA control region (d = 3.8%; phi(ST) = 0.734, P < 0.001) and significant allele frequency differences at nuclear DNA loci (F(ST) = 0.49; P < 0.001). These findings, which indicate that source populations have been isolated for approximately half a million years, set the stage for a survey of the Hawaiian Archipelago (N = 385) to determine the success of these introductions in terms of genetic diversity and breeding behaviour. Both Marquesas and Society mtDNA lineages were detected at each survey site across the Hawaiian Archipelago, at about the same proportion or slightly less than the original 3.4:1 introduction ratio. Nuclear allele frequencies and parentage tests demonstrate that the two source populations are freely interbreeding. The introduction of 2431 Marquesan founders produced only a slight reduction in mtDNA diversity (17%), while the 728 Society founders produced a greater reduction in haplotype diversity (41%). We find no evidence of genetic bottlenecks between islands of the Hawaiian Archipelago, as expected under a stepping-stone model of colonization, from the initial introduction site. This species rapidly colonized across 2000 km without loss of genetic diversity, illustrating the consequences of introducing highly dispersive marine species. C1 [Gaither, Michelle R.; Bowen, Brian W.; Toonen, Robert J.] Univ Hawaii, Hawaii Inst Marine Biol, Kaneohe, HI 96744 USA. [Planes, Serge; Messmer, Vanessa] CRIOBE, CNRS EPHE, UMS 2978, Moorea 98729, Fr Polynesia. [Earle, John] Bernice P Bishop Museum, Honolulu, HI 96817 USA. [Robertson, D. Ross] Smithsonian Trop Res Inst, Panama Unit 9100, Dpo, AA 34002 USA. RP Gaither, MR (reprint author), Univ Hawaii, Hawaii Inst Marine Biol, POB 1346, Kaneohe, HI 96744 USA. EM gaither@hawaii.edu RI Toonen, Rob/K-2891-2012; Messmer, Vanessa/B-5459-2015 OI Toonen, Rob/0000-0001-6339-4340; Messmer, Vanessa/0000-0002-5604-6273 FU National Geographic Society [7269-02]; Papahanaumokuakea Marine National Monument; U.S. Fish and Wildlife Service (USFWS); State of Hawaii; NOAA National Marine Sanctuaries Program [2005-008/66882]; Hawaii Sea [NA05OAR4171048, NA09OAR4170060]; National Science Foundation [OIA0554657, OCE-0453167, OCE-0929031, OCE-0623678]; University of Hawaii; Hawaii Institute of Marine Biology [7829]; School of Ocean and Earth Science and Technology [JC-06-30]; University of Hawaii Sea Grant Program FX This study began with support from the National Geographic Society (grant No. NGS 7269-02 to DRR), and was further supported by research expeditions funded and staffed by the Papahanaumokuakea Marine National Monument. We thank Monument co-trustees NOAA Marine Sanctuaries, U.S. Fish and Wildlife Service (USFWS), and the State of Hawaii. This research was supported by NOAA National Marine Sanctuaries Program MOA No. 2005-008/66882 (BWB & RJT), Hawaii Sea Grant Nos. NA05OAR4171048 and NA09OAR4170060 (BWB), National Science Foundation (NSF) grants No. OIA0554657, OCE-0453167, OCE-0929031 (BWB), and OCE-0623678 (RJT), and the Evolution, Ecology, and Conservation Biology (EECB) specialization at the University of Hawaii. The views expressed herein are those of the authors and do not necessarily reflect the views of NSF, NOAA USFWS, the State of Hawaii, or any of their sub-agencies. Greg Concepcion, Matt Craig, Jonathan Dale, Toby Daly-Engel, Jeff Eble, Matt Iacchei, Stephen Karl, Randall Kosaki, Carl Meyer, Yannis Papastamatiou, Luiz Rocha, Zoli Szabo, Jill Zamzow, Joshua Reece, and the crew of the R.V. Hi'ialakai helped collect specimens. Aulani Wilhelm, Jo-Ann Leong, Hoku Johnson, Danielle Carter, Daniel Polhemus, Randall Kosaki, Ann Mooney, Elizabeth Keenen, and Kelly Gleason provided crucial logistic assistance to this project. We thank Marc Crepeau for valuable laboratory assistance and protocol development, Sarah Daley, Rajesh Shrestha and Mindy Mizobe of the HIMB EPSCoR core facility for their assistance with DNA sequencing, and Shelley Jones and all the members of the ToBo lab and staff at HIMB for their assistance, support and feedback throughout this project. This is contribution #1371 from the Hawaii Institute of Marine Biology, #7829 from the School of Ocean and Earth Science and Technology and #JC-06-30 from the University of Hawaii Sea Grant Program. NR 82 TC 23 Z9 23 U1 0 U2 24 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 MAR PY 2010 VL 19 IS 6 BP 1107 EP 1121 DI 10.1111/j.1365-294X.2010.04535.x PG 15 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 560ME UT WOS:000274906000006 PM 20163550 ER PT J AU Bonaccorso, E Peterson, AT Navarro-Siguenza, AG Fleischer, RC AF Bonaccorso, Elisa Peterson, A. Townsend Navarro-Sigueenza, Adolfo G. Fleischer, Robert C. TI Molecular systematics and evolution of the Cyanocorax jays SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Cyanocorax; Psilorhinus; Calocitta; Neotropics; New World jays; Biogeography; Taxonomy ID CONTROL REGION SEQUENCES; MITOCHONDRIAL-DNA; PHYLOGENETIC ANALYSIS; COMBINING DATA; AVES; BIRDS; MTDNA; GENE; BIOGEOGRAPHY; CONSEQUENCES AB Phylogenetic relationships were studied in the genus Cyanocorax (Aves: Corvidae) and related genera, Psilorhinus and Calocitta, a diverse group of New World jays distributed from the Southern United States South to Argentina. Although the ecology and behavior of some species ill the group have been Studied extensively, lack of a molecular phylogeny has precluded rigorous interpretations in all evolutionary framework. Given the diverse combinations of plumage coloration, size, and morphology, the taxonomy of the group has been inconsistent and understanding of biogeographic patterns problematic. Moreover, plumage similarity between two geographically disjuct species, the Tufted jay (Cyanocorax dickeyi) from western Mexico and the White-tailed jay (C. mystacalis) from western Ecuador and Peru, has puzzled ornithologists for decades. Here, a phylogeny of all species in the three genera is presented, based on study of two mitochondrial and three nuclear genes. Phylogenetic trees revealed the non-monophyly of Cyanocorax, and the division of the whole assemblage ill two groups: "Clade A" containing Psilorhinus morio, both species in Calocitta, Cyanocorax violaceus, C caeruleus, C cristatellus, and C. cyanomelas, and "Clade B" consisting of the remaining species in Cyanocorax. Relationships among species in Clade A were ambiguous and, in general, not well resolved. Within Clade B, analyses revealed the monophyly of the "Cissilopho" jays and showed no evidence for a sister relationship between C mystacalis and C dickeyi. The phylogenetic complexity of lineages in the group suggests several complications for the understanding biogeographic patterns, as well as for proposing a taxonomy that is consistent with morphological variation. Although multiple taxonomic arrangements are possible, recommendations are for recognizing only one genus, Cyanocorax, with Psilorhinus and Calocitta as synonyms. (C) 2009 Elsevier Inc. All rights reserved. C1 [Bonaccorso, Elisa] Pontificia Univ Catolica Ecuador, Fac Ciencias Exactas & Nat, Museo Zool Vertebrados QCAZ, Quito, Ecuador. [Bonaccorso, Elisa; Peterson, A. Townsend] Univ Kansas, Nat Hist Museum, Lawrence, KS 66045 USA. [Navarro-Sigueenza, Adolfo G.] Univ Nacl Autonoma Mexico, Fac Ciencias, Museo Zool Alfonso L Herrera, Mexico City 04510, DF, Mexico. [Fleischer, Robert C.] Smithsonian Inst, Natl Museum Nat Hist, Genet Program, Washington, DC 20008 USA. [Fleischer, Robert C.] Smithsonian Inst, Natl Zool Pk, Washington, DC 20008 USA. [Fleischer, Robert C.] Smithsonian Inst, Natl Museum Nat Hist, Div Birds, Washington, DC 20526 USA. RP Bonaccorso, E (reprint author), Pontificia Univ Catolica Ecuador, Fac Ciencias Exactas & Nat, Museo Zool Vertebrados QCAZ, Av 12 Octubre 1076, Quito, Ecuador. EM elisab@ku.edu OI Navarro-Siguenza, Adolfo G./0000-0003-2652-7719; Peterson, A. Townsend/0000-0003-0243-2379 NR 87 TC 6 Z9 6 U1 1 U2 14 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 MAR PY 2010 VL 54 IS 3 BP 897 EP 909 DI 10.1016/j.ympev.2009.11.014 PG 13 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 563YM UT WOS:000275176500018 PM 19931623 ER PT J AU Bendo, GJ Wilson, CD Warren, BE Brinks, E Butner, HM Chanial, P Clements, DL Courteau, S Irwin, J Israel, FP Knapen, JH Leech, J Matthews, HE Muhle, S Petitpas, G Serjeant, S Tan, BK Tilanus, RPJ Usero, A Vaccari, M van der Werf, P Vlahakis, C Wiegert, T Zhu, M AF Bendo, G. J. Wilson, C. D. Warren, B. E. Brinks, E. Butner, H. M. Chanial, P. Clements, D. L. Courteau, S. Irwin, J. Israel, F. P. Knapen, J. H. Leech, J. Matthews, H. E. Muhle, S. Petitpas, G. Serjeant, S. Tan, B. K. Tilanus, R. P. J. Usero, A. Vaccari, M. van der Werf, P. Vlahakis, C. Wiegert, T. Zhu, M. TI The JCMT Nearby Galaxies Legacy Survey - III. Comparisons of cold dust, polycyclic aromatic hydrocarbons, molecular gas and atomic gas in NGC 2403 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Review DE galaxies: individual: NGC 2403; galaxies: ISM; galaxies: spiral; infrared: galaxies; radio lines: galaxies ID SPITZER-SPACE-TELESCOPE; SPECTRAL ENERGY-DISTRIBUTION; STAR-FORMING GALAXIES; MULTIBAND IMAGING PHOTOMETER; INFRARED-RADIO CORRELATION; COMPACT DWARF GALAXIES; 160 MU-M; SPIRAL GALAXIES; ABSOLUTE CALIBRATION; ABSORPTION-COEFFICIENT AB We used Spitzer Space Telescope 3.6, 8.0, 70 and 160 mu m data, James Clerk Maxwell Telescope HARP-B CO J = (3-2) data, National Radio Astronomy Observatory 12 m telescope CO J = (1-0) data and Very Large Array H i data to investigate the relations among polycyclic aromatic hydrocarbons (PAHs), cold (similar to 20 K) dust, molecular gas and atomic gas within NGC 2403, an SABcd galaxy at a distance of 3.13 Mpc. The dust surface density is mainly a function of the total (atomic and molecular) gas surface density and galactocentric radius. The gas-to-dust ratio monotonically increases with radius, varying from similar to 100 in the nucleus to similar to 400 at 5.5 kpc. The slope of the gas-to-dust ratio is close to that of the oxygen abundance, suggesting that metallicity strongly affects the gas-to-dust ratio within this galaxy. The exponential scale length of the radial profile for the CO J = (3-2) emission is statistically identical to the scale length for the stellar continuum-subtracted 8 mu m (PAH 8 mu m) emission. However, CO J = (3-2) and PAH 8 mu m surface brightnesses appear uncorrelated when examining sub-kpc-sized regions. C1 [Bendo, G. J.; Chanial, P.; Clements, D. L.] Univ London Imperial Coll Sci Technol & Med, Astrophys Grp, Blackett Lab, London SW7 2AZ, England. [Wilson, C. D.; Warren, B. E.] McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1, Canada. [Warren, B. E.] Univ Western Australia, ICRAR, Crawley, WA 6009, Australia. [Brinks, E.; Usero, A.] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Butner, H. M.] James Madison Univ, Dept Phys & Astron, Harrisonburg, VA 22807 USA. [Chanial, P.] Univ Paris Diderot, Lab AIM, CEA, DSM,CNRS,Irfu SAp, F-91191 Gif Sur Yvette, France. [Courteau, S.; Irwin, J.] Queens Univ, Dept Phys Engn Phys & Astron, Kingston, ON K7L 3N6, Canada. [Israel, F. P.; van der Werf, P.; Vlahakis, C.] Leiden Univ, NL-2300 RA Leiden, Netherlands. [Knapen, J. H.] Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Tenerife, Spain. [Knapen, J. H.] Univ La Laguna, Dept Astrofis, E-38205 Tenerife, Spain. [Leech, J.; Tan, B. K.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Matthews, H. E.; Zhu, M.] Natl Res Council Canada, Herzberg Inst Astrophys, DRAO, Penticton, BC V2A 69J, Canada. [Muhle, S.] Joint Inst VLBI Europe, NL-7990 AA Dwingeloo, Netherlands. [Petitpas, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Serjeant, S.] Open Univ, Dept Phys & Astron, Milton Keynes M57 6AA, Bucks, England. [Tilanus, R. P. J.; Zhu, M.] Joint Astron Ctr, Hilo, HI 96720 USA. [Tilanus, R. P. J.] Netherlands Org Sci Res, NL-2509 AC The Hague, Netherlands. [Usero, A.] Observ Madrid, OAN, E-28014 Madrid, Spain. [Vaccari, M.] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy. [Wiegert, T.] Univ Manitoba, Dept Phys & Astron, Winnipeg, MB R3T 2N2, Canada. RP Bendo, GJ (reprint author), Univ London Imperial Coll Sci Technol & Med, Astrophys Grp, Blackett Lab, Prince Consort Rd, London SW7 2AZ, England. EM g.bendo@imperial.ac.uk RI Vaccari, Mattia/R-3431-2016; OI Vaccari, Mattia/0000-0002-6748-0577; Butner, Harold/0000-0003-4899-2064; Brinks, Elias/0000-0002-7758-9699 FU STFC; NSERC (Canada); UK Science & Technology Facilities Council; National Research Council (Canada); National Aeronautics and Space Administration FX We thank the reviewer for his/her comments on this paper. The JCMT 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. GJB and DLC were funded by STFC. The research of JI and CDW is supported by grants from NSERC (Canada). AU has been supported through a Post-Doctoral Research Assistantship from the UK Science & Technology Facilities Council. Travel support for BEW and TW was supplied by the National Research Council (Canada). 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 112 TC 45 Z9 45 U1 0 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAR 1 PY 2010 VL 402 IS 3 BP 1409 EP 1425 DI 10.1111/j.1365-2966.2009.16043.x PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 555CA UT WOS:000274483500001 ER PT J AU Keto, E Caselli, P AF Keto, Eric Caselli, Paola TI Dynamics and depletion in thermally supercritical starless cores SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE hydrodynamics; line: profiles; radiative transfer; ISM: clouds; ISM: molecules ID COLLAPSING PRESTELLAR CORES; MAGNETIZED MOLECULAR CLOUDS; GRAIN-SURFACE-REACTIONS; PROTOSTELLAR COLLAPSE; INITIAL CONDITIONS; ISOTHERMAL SPHERE; LINE-PROFILES; DARK CLOUDS; GRAVITATIONAL COLLAPSE; INTERSTELLAR CLOUDS AB In previous studies, we identified two classes of starless cores, thermally subcritical and supercritical, distinguished by different dynamical behaviour and internal structure. Here, we study the evolution of the dynamically unstable, thermally supercritical cores by means of a numerical hydrodynamic simulation that includes radiative equilibrium and simple molecular chemistry. From an initial state as an unstable Bonnor-Ebert (BE) sphere, a contracting core evolves towards the configuration of a singular isothermal sphere by inside-out collapse. We follow the gas temperature and abundance of CO during the contraction. The temperature is predominantly determined by radiative equilibrium, but in the rapidly contracting centre of the core compressive heating raises the gas temperature by a few degrees over its value in static equilibrium. The time-scale for the equilibration of CO depends on the gas density and is everywhere shorter than the dynamical time-scale. The result is that the dynamics do not much affect the abundance of CO which is always close to that of a static sphere of the same density profile, and CO cannot be used as a chemical clock in starless cores. We use our non-local thermodynamic equilibrium (non-LTE) radiative transfer code mollie to predict observable CO and N2H+ line spectra, including the non-LTE hyperfine ratios of N2H+, during the contraction. These are compared against observations of the starless core L1544. The comparison indicates that the dust in L1544 has an opacity consistent with ice-covered rather than bare grains, the cosmic ray ionization rate is about 1 x 10-17 s-1 and the density structure of L1544 is approximately that of a BE sphere with a maximum central density of 2 x 107 cm-3, equivalent to an average density of 3 x 106 cm-3 within a radius of 500 au. The observed CO linewidths and intensities are reproduced if the CO desorption rate is about 30 times higher than the rate expected from cosmic ray strikes alone, indicating that other desorption processes are also active. C1 [Keto, Eric] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02420 USA. [Caselli, Paola] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. RP Keto, E (reprint author), Harvard Smithsonian Ctr Astrophys, 160 Garden St, Cambridge, MA 02420 USA. EM keto@cfa.harvard.edu; p.caselli@leeds.ac.uk NR 73 TC 51 Z9 51 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAR 1 PY 2010 VL 402 IS 3 BP 1625 EP 1634 DI 10.1111/j.1365-2966.2009.16033.x PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 555CA UT WOS:000274483500017 ER PT J AU Hopkins, PF Younger, JD Hayward, CC Narayanan, D Hernquist, L AF Hopkins, Philip F. Younger, Joshua D. Hayward, Christopher C. Narayanan, Desika Hernquist, Lars TI Mergers, active galactic nuclei and 'normal' galaxies: contributions to the distribution of star formation rates and infrared luminosity functions SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Review DE galaxies: active; galaxies: evolution; galaxies: formation; cosmology: theory ID SUPERMASSIVE BLACK-HOLES; DIGITAL-SKY-SURVEY; HUBBLE-SPACE-TELESCOPE; DUST-OBSCURED GALAXIES; HIGH-REDSHIFT GALAXIES; TULLY-FISHER RELATION; SPITZER MIDINFRARED SPECTROSCOPY; INITIAL MASS FUNCTION; SIMILAR-TO 2; DEPENDENT QUASAR LIFETIMES AB We use a novel method to predict the contribution of normal star-forming galaxies, merger-induced bursts and obscured active galactic nuclei (AGN), to infrared luminosity functions (LFs) and global star formation rate (SFR) densities. We use empirical halo occupation constraints to populate haloes with galaxies and determine the distribution of normal and merging galaxies. Each system can then be associated with high-resolution hydrodynamic simulations. We predict the distribution of observed luminosities and SFRs, from different galaxy classes, as a function of redshift from z = 0 to 6. We provide fitting functions for the predicted LFs, quantify the uncertainties, and compare with observations. At all redshifts, 'normal' galaxies dominate the LF at moderate luminosities similar to L(*) (the 'knee'). Merger-induced bursts increasingly dominate at L L(*); at the most extreme luminosities, AGN are important. However, all populations increase in luminosity at higher redshifts, owing to increasing gas fractions. Thus, the 'transition luminosity' between normal and merger-dominated sources increases from the luminous infrared galaxy (LIRG)-ultraluminous infrared galaxy threshold at z similar to 0 to bright Hyper-LIRG thresholds at z similar to 2. The transition to dominance by obscured AGN evolves similarly, at factor of several higher L(IR). At all redshifts, non-merging systems dominate the total luminosity/SFR density, with merger-induced bursts constituting similar to 5-10 per cent and AGN similar to 1-5 per cent. Bursts contribute little to scatter in the SFR-stellar mass relation. In fact, many systems identified as 'ongoing' mergers will be forming stars in their 'normal' (non-burst) mode. Counting this as 'merger-induced' star formation leads to a stronger apparent redshift evolution in the contribution of mergers to the SFR density. We quantify how the evolution in LFs depends on evolution in galaxy gas fractions, merger rates, and possible evolution in the Schmidt-Kennicutt relation. We discuss areas where more detailed study, with full radiative transfer treatment of complex three-dimensional clumpy geometries in mixed AGN-star-forming systems, is necessary. C1 [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. [Younger, Joshua D.] Inst Adv Study, Princeton, NJ 08540 USA. [Hayward, Christopher C.; Narayanan, Desika; Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Hopkins, PF (reprint author), Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. EM phopkins@astro.berkeley.edu RI Hayward, Christopher/I-4756-2012 OI Hayward, Christopher/0000-0003-4073-3236 FU NASA [HF-51266.01, NAS 5-26555]; Space Telescope Science Institute; Association of Universities for Research in Astronomy, Inc.; FAS Research Computing Group at Harvard University FX We thank Eliot Quataert, Lin Yan, Dave Sanders, Nick Scoville and Kevin Bundy for helpful discussions throughout the development of this manuscript. Support for PFH was provided by the Miller Institute for Basic Research in Science, University of California Berkeley. JDY 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. Many of the computations in this paper were run on the Odyssey cluster supported by the FAS Research Computing Group at Harvard University. NR 245 TC 80 Z9 80 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 MAR 1 PY 2010 VL 402 IS 3 BP 1693 EP 1713 DI 10.1111/j.1365-2966.2009.15990.x PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 555CA UT WOS:000274483500024 ER PT J AU Zapata, LA Schilke, P Ho, PTP AF Zapata, Luis A. Schilke, Peter Ho, Paul T. P. TI A contracting circumbinary molecular ring around Ori 139-409 with an inner cavity of about 140 au SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE binaries: general; stars: pre-main-sequence; ISM: individual: Orion-S; ISM: individual: M42; ISM: molecules; radio continuum: ISM; submillimetre ID OMC-1 SOUTH; SUBMILLIMETER ARRAY; GG TAURI; DISKS; OUTFLOW; CIRCUMSTELLAR; CALIBRATION; CLUSTER; BINARY; NEBULA AB We present sensitive and subarcsecond resolution (similar to 0.7 arcsec) CH(3)OH(7(-2,6)-6(-2,5)) line and 890-mu m continuum observations, made with the Submillimeter Array (SMA), towards the hot molecular circumbinary ring associated with the young multiple star Ori 139-409. The CH(3)OH(7(-2,6)-6(-2,5)) emission from the ring is well resolved at this angular resolution, revealing an inner cavity with a size of about 140 au. A local thermodynamic equilibrium model of a Keplerian disc with an inner cavity of the same size confirms the presence of this cavity. Additionally, this model suggests that the circumbinary ring is contracting with a velocity of V(inf) similar to 1.5 km s(-1) towards the binary central compact circumstellar discs reported at a wavelength of 7 mm. The inner central cavity seems to be formed by the tidal effects of the young stars in the middle of the ring. The ring does not appear to be a stationary object. Furthermore, the infall velocity we determine is about a factor of 3 slower than the free-fall velocity corresponding to the dynamical mass. This would correspond to a mass accretion rate of about 10(-5) M(circle dot) yr(-1). We have found that the dust emission associated with Ori 139-409 appears to be arising from the circumstellar discs, with no strong contribution from the molecular gas ring. Furthermore, a simple comparison with other classical molecular dusty rings (e. g. GG Tau, UZ Tau and UY Aur) suggests that Ori 139-409 could be one of the youngest circumbinary rings reported to date. Finally, our results confirm that the circumbinary rings are actively funnelling fresh gas material to the central compact binary circumstellar discs (i.e. to the protostars in the very early phases of their evolution). C1 [Zapata, Luis A.; Schilke, Peter] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Schilke, Peter] Univ Cologne, Inst Phys, D-50937 Cologne, Germany. [Ho, Paul T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ho, Paul T. P.] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan. RP Zapata, LA (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. EM lzapata@mpifr-bonn.mpg.de NR 24 TC 3 Z9 3 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 MAR PY 2010 VL 402 IS 4 BP 2221 EP 2227 DI 10.1111/j.1365-2966.2009.16051.x PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 563DJ UT WOS:000275107400006 ER PT J AU Steinhardt, CL Elvis, M AF Steinhardt, Charles L. Elvis, Martin TI The quasar mass-luminosity plane - I. A sub-Eddington limit for quasars 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 DIGITAL-SKY-SURVEY; BLACK-HOLE MASSES; ACTIVE GALACTIC NUCLEI; SELECTION; EVOLUTION; GALAXIES; RELEASE; SAMPLE AB We use 62 185 quasars from the Sloan Digital Sky Survey Data Release 5 sample to explore the relationship between black hole mass and luminosity. Black hole masses were estimated based on the widths of their H beta, Mg II and C IV lines and adjacent continuum luminosities using standard virial mass estimate scaling laws. We find that, over the range 0.2 < z < 4.0, the most luminous low-mass quasars are at their Eddington luminosity, but the most luminous high-mass quasars in each redshift bin fall short of their Eddington luminosities, with the shortfall of the order of 10 or more at 0.2 < z < 0.6. We examine several potential sources of measurement uncertainty or bias and show that none of them can account for this effect. We also show the statistical uncertainty in virial mass estimation to have an upper bound of similar to 0.15 dex, smaller than the 0.4 dex previously reported. We also examine the highest mass quasars in every redshift bin in an effort to learn more about quasars that are about to cease their luminous accretion. We conclude that the quasar mass-luminosity locus contains a number of new puzzles that must be explained theoretically. 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 (Chandra X-ray Center) [G07-8136A] FX The authors would like to thank Mihail Amarie, Forrest Collman, Doug Finkbeiner, Margaret Geller, Lars Hernquist, Gillian Knapp, Avi Loeb, Ramesh Narayan, Jerry Ostriker and Michael Strauss for valuable comments. This work was supported in part by Chandra grant number G07-8136A (Chandra X-ray Center). NR 33 TC 56 Z9 56 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 MAR PY 2010 VL 402 IS 4 BP 2637 EP 2648 DI 10.1111/j.1365-2966.2009.16084.x PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 563DJ UT WOS:000275107400041 ER PT J AU Hill, T Longmore, SN Pinte, C Cunningham, MR Burton, MG Minier, V AF Hill, T. Longmore, S. N. Pinte, C. Cunningham, M. R. Burton, M. G. Minier, V. TI Physical characterization of southern massive star-forming regions using Parkes NH3 observations SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE line: profiles; masers; stars: early-type; stars: formation; stars: fundamental parameters; ISM: molecules ID MILLIMETER CONTINUUM OBSERVATIONS; ULTRACOMPACT HII-REGIONS; INFRARED DARK CLOUDS; METHANOL MASERS; MULTIWAVELENGTH OBSERVATIONS; PROTOSTELLAR CANDIDATES; INTERSTELLAR AMMONIA; COLD CORES; EMISSION; OBJECTS AB We have undertaken a Parkes ammonia spectral line study, in the lowest two inversion transitions, of southern massive star formation regions, including young massive candidate protostars, with the aim of characterizing the earliest stages of massive star formation. 138 sources from the submillimetre continuum emission studies of Hill et al. were found to have robust (1,1) detections, including two sources with two velocity components, and 102 in the (2,2) transition. We determine the ammonia line properties of the sources: linewidth, flux density, kinetic temperature, NH3 column density and opacity, and revisit our spectral energy distribution modelling procedure to derive the mass for 52 of the sources. By combining the continuum emission information with ammonia observations we substantially constrain the physical properties of the high-mass clumps. There is clear complementarity between ammonia and continuum observations for derivations of physical parameters. The MM-only class, identified in the continuum studies of Hill et al., displays smaller sizes, mass and velocity dispersion and/or turbulence than star-forming clumps, suggesting a quiescent prestellar stage and/or the formation of less massive stars. C1 [Hill, T.; Pinte, C.] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England. [Longmore, S. N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Cunningham, M. R.; Burton, M. G.] Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia. [Minier, V.] CEA, DSM, IRFU, Serv Astrophys, F-91191 Gif Sur Yvette, France. [Minier, V.] Univ Paris Diderot, Lab AIM, CEA DSM, CNRS,IRFU Serv Astrophys,CEA Saclay, F-91191 Gif Sur Yvette, France. RP Hill, T (reprint author), Univ Exeter, Sch Phys, Stocker Rd, Exeter EX4 4QL, Devon, England. EM thill@astro.ex.ac.uk OI Cunningham, Maria/0000-0001-7020-6176; Burton, Michael/0000-0001-7289-1998 FU European Commission [PIEF-GA-2008-220891]; Commonwealth of Australia FX The authors would like to thank S. Mader for observational support and J. Reynolds & E. Carretti for help with calibration of the observations and derivation of the gain elevation correction. We also extend thanks to an anonymous referee whose comments served to improve the manuscript. C. Pinte acknowledges funding support of the European Commission's Seventh Framework Program as a Marie Curie Intra-European Fellow (PIEF-GA-2008-220891). The Parkes telescope is part of the Australia Telescope which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. NR 43 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 MAR PY 2010 VL 402 IS 4 BP 2682 EP 2702 DI 10.1111/j.1365-2966.2009.16101.x PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 563DJ UT WOS:000275107400046 ER PT J AU Di Stefano, R Kong, A Primini, FA AF Di Stefano, Rosanne Kong, Albert Primini, Francis A. TI Ten facts of life for distant supersoft sources SO NEW ASTRONOMY REVIEWS LA English DT Article ID X-RAY SOURCES; QUASI-SOFT; EXTERNAL GALAXIES; WHITE-DWARF; XMM-NEWTON; CHANDRA; M31; POPULATION; DISCOVERY; REMNANTS AB First discovered in the Magellanic Clouds and in the Milky Way, the largest pools of luminous supersoft Xray sources (SSSs) now known lie in M31 and in more distant galaxies. Hundreds of newly-discovered SSSs are helping us to test models for Type la supernovae and to identify SSSs that may represent a wider range of physical systems, including accreting intermediate-mass black holes. In this short report we list ten intriguing facts about distant SSSs. (C) 2010 Published by Elsevier B.V. C1 [Di Stefano, Rosanne; Primini, Francis A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kong, Albert] MIT, Kavli Inst, Cambridge, MA 02139 USA. RP Di Stefano, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rdistefano@cfa.harvard.edu OI Primini, Francis/0000-0002-6077-0643 NR 24 TC 10 Z9 10 U1 0 U2 0 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1387-6473 J9 NEW ASTRON REV JI New Astron. Rev. PD MAR-JUN PY 2010 VL 54 IS 3-6 BP 72 EP 74 DI 10.1016/j.newar.2010.09.006 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 698BY UT WOS:000285567700009 ER PT J AU Nelemans, G Jonker, PG AF Nelemans, G. Jonker, P. G. TI Ultra-compact (X-ray) binaries SO NEW ASTRONOMY REVIEWS LA English DT Article ID GLOBULAR-CLUSTER M15; DOUBLE WHITE-DWARFS; AM CVN STARS; LOW-MASS; OPTICAL SPECTROSCOPY; PERIOD BINARY; DONOR STARS; SPIN-UP; 2S-0918-549; 4U-1543-624 AB A short year 2005 review of ultra-compact binaries, focused on ultra-compact X-ray binaries, is followed by a discussion of results of our VLT campaign to obtain optical spectra of (candidate) ultra-compact Xray binaries. We find evidence for carbon/oxygen as well as helium/nitrogen discs and no evidence for (traces) of hydrogen. This suggests that the donors in the observed systems are white dwarfs. However, we also find large differences between the two C/O discs of which we have good spectra, which highlights the need for a better understanding of the optical spectra. (C) 2010 Elsevier B.V. All rights reserved. C1 [Nelemans, G.; Jonker, P. G.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, Nijmegen, Netherlands. [Jonker, P. G.] SRON Netherlands Inst Space Res, Utrecht, NL, Netherlands. [Jonker, P. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. RP Nelemans, G (reprint author), Radboud Univ Nijmegen, Dept Astrophys IMAPP, Nijmegen, Netherlands. EM nelemans@astro.ru.nl RI Nelemans, Gijs/D-3177-2012 OI Nelemans, Gijs/0000-0002-0752-2974 NR 42 TC 16 Z9 16 U1 0 U2 0 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1387-6473 J9 NEW ASTRON REV JI New Astron. Rev. PD MAR-JUN PY 2010 VL 54 IS 3-6 BP 87 EP 92 DI 10.1016/j.newar.2010.09.021 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 698BY UT WOS:000285567700012 ER PT J AU Billet, G Orliac, M Antoine, PO Jaramillo, C AF Billet, Guillaume Orliac, Maeva Antoine, Pierre-Olivier Jaramillo, Carlos TI NEW OBSERVATIONS AND REINTERPRETATION ON THE ENIGMATIC TAXON COLOMBITHERIUM (?PYROTHERIA, MAMMALIA) FROM COLOMBIA SO PALAEONTOLOGY LA English DT Article DE bilophodont; Eocene; maxillary; ungulate; anatomy; systematics ID OLIGOCENE; BOLIVIA; EOCENE; TEETH AB The controversial taxon Colombitherium tolimense ( Mammalia) ( probably Late Eocene in age) from Colombia, although known for nearly 40 years, still bears much mystery. Aside from the problematic ordinal attribution of the holotype and only specimen, its determination as an upper or lower jaw remains a highly debated issue. New observations include the presence of a contact facet on the distal face of the most posterior tooth, which indicates that the fragmentary jaw preserves three premolars and two molars; the M3, unpreserved but present, being most probably reduced. This new interpretation completely fits the morphology of the teeth. Furthermore, the shape of these latter and the deeper wear encompassed by their lingual part relative to the labial one is typical of upper dentition. This is in agreement with the internal curving of the roots of the anterior premolars and with several other arguments that lead interpreting the holotype of C. tolimense as a maxillary bearing P2-M2. This new interpretation deepens the morphological gap between Colombitherium and other pyrotherians (except Proticia) and challenges further its referral to Pyrotheria. The peculiar morphology of Colombitherium relative to other pyrotherians is indeed striking. In fact, Colombitherium has nothing in common with pyrotherians but bilophodont cheek teeth, a feature largely widespread in placental mammals. It is here referred to ? Pyrotheria until additional evidence of its relationships is known. Associated with the putative removal of Proticia from Pyrotheria as argued by some authors, the hypothetical removal of Colombitherium from the order would adjust the widely accepted assumption that the pyrotherian bilophodont cheek teeth originated from bunodont cheek teeth. It would also make an origin from lophodont forms plausible. This in turn would have critical relevance, especially to the hypothesis that pyrotherians are notoungulates. C1 [Billet, Guillaume] Univ Poitiers, IPHEP, CNRS, UMR 6046,Fac Sci Fondamentales & Appliquees, F-86022 Poitiers, France. [Orliac, Maeva] Univ Montpellier 2, Inst Sci Evolut, CNRS, UMR 5554, F-34095 Montpellier 5, France. [Antoine, Pierre-Olivier] Univ Toulouse, F-31400 Toulouse, France. [Antoine, Pierre-Olivier] UPS, SVT OMP, F-31400 Toulouse, France. [Antoine, Pierre-Olivier] LMTG, F-31400 Toulouse, France. [Antoine, Pierre-Olivier] CNRS, F-31400 Toulouse, France. [Antoine, Pierre-Olivier] IRD, F-31400 Toulouse, France. [Jaramillo, Carlos] Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archeol, Balboa, Ancon, Panama. RP Billet, G (reprint author), Univ Poitiers, IPHEP, CNRS, UMR 6046,Fac Sci Fondamentales & Appliquees, 40 Ave Recteur Pineau, F-86022 Poitiers, France. EM guillaume.billet@univ-poitiers.fr; maeva.orliac@univ-montp2.fr; poa@lmtg.obs-mip.fr; jaramilloC@si.edu NR 32 TC 3 Z9 3 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0031-0239 J9 PALAEONTOLOGY JI Paleontology PD MAR PY 2010 VL 53 BP 319 EP 325 DI 10.1111/j.1475-4983.2010.00936.x PN 2 PG 7 WC Paleontology SC Paleontology GA 570KE UT WOS:000275673200006 ER PT J AU Kuznetsova, E Gacesa, M Yelin, SF Cote, R AF Kuznetsova, Elena Gacesa, Marko Yelin, Susanne F. Cote, Robin TI Phase gate and readout with an atom-molecule hybrid platform SO PHYSICAL REVIEW A LA English DT Article ID OPTICAL LATTICES; POLAR-MOLECULES; QUANTUM; GAS AB In order to optimize quantum information processing in individual traps such as optical lattices, we propose a combined atom-molecule system. In particular, gates, initialization, and readout are suggested, using two atoms of different species-one atom carrying the qubit and the other enabling interaction. We describe in some detail the implementation of a two-qubit phase gate in which a pair of atoms is transferred into the ground rovibrational state of a polar molecule with a large dipole moment, thus allowing molecules in adjacent sites to interact via their dipole-dipole interaction. We also discuss how the reverse process could be used as a nondestructive readout tool. C1 [Kuznetsova, Elena; Gacesa, Marko; Yelin, Susanne F.; Cote, Robin] Univ Connecticut, Dept Phys, Storrs, CT 06269 USA. [Kuznetsova, Elena; Yelin, Susanne F.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Kuznetsova, E (reprint author), Univ Connecticut, Dept Phys, Storrs, CT 06269 USA. RI Gacesa, Marko/F-8027-2011 OI Gacesa, Marko/0000-0001-5145-051X FU ARO; NSF FX The authors gratefully acknowledge fruitful discussions with M. Lukin and financial support from ARO and NSF. NR 33 TC 12 Z9 12 U1 0 U2 0 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 MAR PY 2010 VL 81 IS 3 AR 030301 DI 10.1103/PhysRevA.81.030301 PG 4 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 577ZK UT WOS:000276262500001 ER PT J AU Zhao, L Yelin, SF AF Zhao, L. Yelin, S. F. TI Proposal for graphene-based coherent buffers and memories SO PHYSICAL REVIEW B LA English DT Article ID BILAYER GRAPHENE; BERRYS PHASE; QUANTUM DOTS; FILMS AB We theoretically show that it is possible to coherently control the group velocity of graphene quasiparticles based on tunable electric field effects in both single layer and bilayer graphene p-n-p waveguides, whereby graphene-based coherent buffers and memories could be proposed. We also find that the essential mechanism for the coherent buffering and trapping of quasiparticles can be attributed to interband tunneling through p-n interfaces. C1 [Zhao, L.; Yelin, S. F.] Univ Connecticut, Dept Phys, Storrs, CT 06269 USA. [Zhao, L.] Tsinghua Univ, Dept Phys, Beijing 100084, Peoples R China. [Yelin, S. F.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Zhao, L (reprint author), Univ Connecticut, Dept Phys, Storrs, CT 06269 USA. FU NSF FX We would like to acknowledge funding from NSF. L.Z. thanks J. Javanainen, W. Duan, R. Zhou, T. Wang, and F. Peng for helpful discussions. NR 33 TC 26 Z9 27 U1 0 U2 6 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1098-0121 J9 PHYS REV B JI Phys. Rev. B PD MAR PY 2010 VL 81 IS 11 AR 115441 DI 10.1103/PhysRevB.81.115441 PG 4 WC Physics, Condensed Matter SC Physics GA 577UF UT WOS:000276248800154 ER PT J AU Olson, JR Cooper, SJ Swanson, DL Braun, MJ Williams, JB AF Olson, Jennifer R. Cooper, Sheldon J. Swanson, David L. Braun, Michael J. Williams, Joseph B. TI The Relationship of Metabolic Performance and Distribution in Black-Capped and Carolina Chickadees SO PHYSIOLOGICAL AND BIOCHEMICAL ZOOLOGY LA English DT Review ID MITOCHONDRIAL PROTON LEAK; MUSCLE AEROBIC CAPACITY; C-OXIDASE ACTIVITY; HYBRID ZONE; OXYGEN-CONSUMPTION; PARUS-ATRICAPILLUS; SEASONAL ACCLIMATIZATION; AVIAN DISTRIBUTIONS; PASSERINE BIRDS; INTERPOPULATION HYBRIDS AB In endotherms, metabolic performance is associated with a wide array of ecological traits, including species distribution. Researchers have suggested that the northern boundaries of North American passerines are limited by their ability to sustain the high metabolic rates required for thermoregulation. Black-capped chickadees (Poecile atricapillus; BC) are year-round residents in most of Canada and the northern half of the United States, whereas Carolina chickadees (Poecile carolinensis; CA) are found exclusively in the southeastern United States. These species hybridize along a narrow contact zone that has been moving northward at a rate of about 1.6 km per decade, coincident with warming temperatures in Ohio. The location of the chickadee hybrid zone in Ohio closely matches air temperature isotherms, further suggesting that metabolic rate may correlate with distribution in these species. We tested the hypothesis that distribution patterns of chickadees are linked with their rate of metabolism. For populations of BC and CA chickadees, we measured basal metabolic rates (BMRs) and cold-induced peak metabolic rates from areas that differ in winter temperatures and supplemented this information with data from other studies. Although our findings suggest a general relationship between lower air temperatures and higher metabolic rate among black-capped chickadee populations, this trend was not robust across all locations. There was no significant relationship between lower air temperatures and metabolism in Carolina chickadees. Within Ohio, hybrids had a significantly higher mass-corrected BMR than either parental species. We suggest that the mtDNA-nDNA mismatch of hybrids may produce less efficient mitochondrial protein complexes, which in turn affects the efficiency of ATP production, thereby increasing rate of oxygen consumption to meet ATP demands. C1 [Olson, Jennifer R.; Williams, Joseph B.] Ohio State Univ, Dept Ecol Evolut & Organismal Biol, Columbus, OH 43210 USA. [Cooper, Sheldon J.] Univ Wisconsin Oshkosh, Dept Biol & Microbiol, Oshkosh, WI 54901 USA. [Swanson, David L.] Univ S Dakota, Dept Biol, Vermillion, SD 57069 USA. [Braun, Michael J.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Suitland, MD 20746 USA. [Braun, Michael J.] Univ Maryland, Behav Ecol Evolut & Systemat Program, College Pk, MD 20742 USA. RP Olson, JR (reprint author), Ohio State Univ, Dept Ecol Evolut & Organismal Biol, 318 W 12th Ave, Columbus, OH 43210 USA. EM olson.133@osu.edu FU National Science Foundation [IBN-0212587] FX We thank the landowners in Ohio and Tennessee, especially Steve Humrichauser and Judy Varner, who allowed us to capture birds on their properties. We would also like to acknowledge Sue Chaplin for going beyond the call of duty to find New York chickadee data that were covered in dust; Chris Huddleston and Sarah Kingston for their assistance and advice in our genetic identification of chickadees; theWilliams Lab group for their comments on earlier drafts of this manuscript; Thomas Grubb for his role in initially suggesting this project; and the comments of three anonymous reviewers. This study was supported in part by National Science Foundation IBN-0212587 to J. B. W. NR 101 TC 21 Z9 21 U1 3 U2 28 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 1522-2152 J9 PHYSIOL BIOCHEM ZOOL JI Physiol. Biochem. Zool. PD MAR-APR PY 2010 VL 83 IS 2 BP 263 EP 275 DI 10.1086/648395 PG 13 WC Physiology; Zoology SC Physiology; Zoology GA 554OD UT WOS:000274443400007 PM 20151817 ER PT J AU Martin, KC Bruhn, D Lovelock, CE Feller, IC Evans, JR Ball, MC AF Martin, Katherine C. Bruhn, Dan Lovelock, Catherine E. Feller, Ilka C. Evans, John R. Ball, Marilyn C. TI Nitrogen fertilization enhances water-use efficiency in a saline environment SO PLANT CELL AND ENVIRONMENT LA English DT Article DE Avicennia marina; mangroves; nutrient limitation; phosphorus; photosynthesis; salinity; stomatal conductance ID CARBON-ISOTOPE DISCRIMINATION; MANGROVE RHIZOPHORA-MANGLE; VS. PHOSPHORUS LIMITATION; GAS-EXCHANGE; AVICENNIA-MARINA; NUTRIENT ENRICHMENT; LEAF-AREA; PHOTOSYNTHETIC CAPACITY; AEGICERAS-CORNICULATUM; HYDRAULIC CONDUCTANCE AB Effects of salinity and nutrients on carbon gain in relation to water use were studied in the grey mangrove, Avicennia marina, growing along a natural salinity gradient in south-eastern Australia. Tall trees characterized areas of seawater salinities (fringe zone) and stunted trees dominated landward hypersaline areas (scrub zone). Trees were fertilized with nitrogen (+N) or phosphorus (+P) or unfertilized. There was no significant effect of +P on shoot growth, whereas +N enhanced canopy development, particularly in scrub trees. Scrub trees maintained greater CO(2) assimilation per unit water transpired (water-use efficiency, WUE) and had lower nitrogen-use efficiency (NUE; CO(2) assimilation rate per unit leaf nitrogen) than fringe trees. The CO(2) assimilation rates of +N trees were similar to those in other treatments, but were achieved at lower transpiration rates, stomatal conductance and intercellular CO(2) concentrations. Maintaining comparable assimilation rates at lower stomatal conductance requires greater ribulose 1 center dot 5-bisphosphate carboxylase/oxygenase activity, consistent with greater N content per unit leaf area in +N trees. Hence, +N enhanced WUE at the expense of NUE. Instantaneous WUE estimates were supported by less negative foliar delta 13C values for +N trees and scrub control trees. Thus, nutrient enrichment may alter the structure and function of mangrove forests along salinity gradients. C1 [Martin, Katherine C.; Bruhn, Dan; Evans, John R.; Ball, Marilyn C.] Australian Natl Univ, Res Sch Biol, Div Plant Sci, Canberra, ACT 0200, Australia. [Lovelock, Catherine E.] Univ Queensland, Ctr Marine Studies, St Lucia, Qld 4072, Australia. [Lovelock, Catherine E.] Univ Queensland, Sch Biol Sci, St Lucia, Qld 4072, Australia. [Feller, Ilka C.] Smithsonian Environm Res Ctr, Smithsonian Inst, Edgewater, MD 21037 USA. RP Martin, KC (reprint author), Australian Natl Univ, Res Sch Biol, Div Plant Sci, GPO Box 4, Canberra, ACT 0200, Australia. EM katherine.martin@anu.edu.au RI Ball, Marilyn/D-1180-2009; Lovelock, Catherine/G-7370-2012; Evans, John/C-8424-2009; OI Lovelock, Catherine/0000-0002-2219-6855; Evans, John/0000-0003-1379-3532; Feller, Ilka/0000-0002-6391-1608 FU Australian Postgraduate Award; Kioloa Joy London Foundation; American Association for the Advancement of Science; National Science Foundation [DEB-9981535]; Johnston Fund of the Smithsonian Institution FX The authors thank Jack Egerton and Wayne Pippen for field assistance, Adrienne Nicotra for loan of equipment, Stephanie McCaffery for assistance with nutrient analyses, and the Berkhouts at Kioloa Research Station. K.C.M. was supported by an Australian Postgraduate Award, and received a Kioloa Joy London Foundation Research Support Grant. C.E.L. and I.C.F. received a WISC Travel Grant from the American Association for the Advancement of Science, and support from the National Science Foundation DEB-9981535 and the Johnston Fund of the Smithsonian Institution. NR 85 TC 16 Z9 16 U1 3 U2 41 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0140-7791 J9 PLANT CELL ENVIRON JI Plant Cell Environ. PD MAR PY 2010 VL 33 IS 3 BP 344 EP 357 DI 10.1111/j.1365-3040.2009.02072.x PG 14 WC Plant Sciences SC Plant Sciences GA 554CG UT WOS:000274412500004 PM 19906150 ER PT J AU Abad-Franch, F Ferraz, G Campos, C Palomeque, FS Grijalva, MJ Aguilar, HM Miles, MA AF Abad-Franch, Fernando Ferraz, Goncalo Campos, Ciro Palomeque, Francisco S. Grijalva, Mario J. Marcelo Aguilar, H. Miles, Michael A. TI Modeling Disease Vector Occurrence when Detection Is Imperfect: Infestation of Amazonian Palm Trees by Triatomine Bugs at Three Spatial Scales SO PLOS NEGLECTED TROPICAL DISEASES LA English DT Article ID RURAL NORTHWESTERN ARGENTINA; RECORD SYSTEMS ESTIMATION; ESTIMATING SITE OCCUPANCY; CHAGAS-DISEASE; CAPTURE-RECAPTURE; RISK-FACTORS; NUTRITIONAL-STATUS; RHODNIUS-PROLIXUS; LATIN-AMERICA; POPULATIONS AB Background: Failure to detect a disease agent or vector where it actually occurs constitutes a serious drawback in epidemiology. In the pervasive situation where no sampling technique is perfect, the explicit analytical treatment of detection failure becomes a key step in the estimation of epidemiological parameters. We illustrate this approach with a study of Attalea palm tree infestation by Rhodnius spp. (Triatominae), the most important vectors of Chagas disease (CD) in northern South America. Methodology/Principal Findings: The probability of detecting triatomines in infested palms is estimated by repeatedly sampling each palm. This knowledge is used to derive an unbiased estimate of the biologically relevant probability of palm infestation. We combine maximum-likelihood analysis and information-theoretic model selection to test the relationships between environmental covariates and infestation of 298 Amazonian palm trees over three spatial scales: region within Amazonia, landscape, and individual palm. Palm infestation estimates are high (40-60%) across regions, and well above the observed infestation rate (24%). Detection probability is higher (similar to 0.55 on average) in the richest-soil region than elsewhere (similar to 0.08). Infestation estimates are similar in forest and rural areas, but lower in urban landscapes. Finally, individual palm covariates (accumulated organic matter and stem height) explain most of infestation rate variation. Conclusions/Significance: Individual palm attributes appear as key drivers of infestation, suggesting that CD surveillance must incorporate local-scale knowledge and that peridomestic palm tree management might help lower transmission risk. Vector populations are probably denser in rich-soil sub-regions, where CD prevalence tends to be higher; this suggests a target for research on broad-scale risk mapping. Landscape-scale effects indicate that palm triatomine populations can endure deforestation in rural areas, but become rarer in heavily disturbed urban settings. Our methodological approach has wide application in infectious disease research; by improving eco-epidemiological parameter estimation, it can also significantly strengthen vector surveillance-control strategies. C1 [Abad-Franch, Fernando; Ferraz, Goncalo; Campos, Ciro] Fiocruz Amazonia, Inst Leonidas & Maria Deane, Manaus, Amazonas, Brazil. [Abad-Franch, Fernando; Miles, Michael A.] London Sch Hyg & Trop Med, Pathogen Mol Biol Unit, Dept Infect & Trop Dis, London WC1, England. [Ferraz, Goncalo] Inst Nacl de Pesquisas da Amazonia, Smithsonian Trop Res Inst, Biol Dynam Forest Fragments Project, Manaus, Amazonas, Brazil. [Palomeque, Francisco S.] Emory Univ, Rollins Sch Publ Hlth, Atlanta, GA 30322 USA. [Palomeque, Francisco S.; Grijalva, Mario J.] Pontificia Univ Catolica Ecuador, Ctr Invest Enfermedades Infecciosas, Quito, Ecuador. [Grijalva, Mario J.] Ohio Univ, Coll Osteopath Med, Trop Dis Inst, Dept Biomed Sci, Athens, OH 45701 USA. [Marcelo Aguilar, H.] Fdn Int Ciencias Sociales & Salud, Inst Juan Cesar Garcia, Quito, Ecuador. [Marcelo Aguilar, H.] Minist Salud Publ Ecuador, Quito, Ecuador. RP Abad-Franch, F (reprint author), Fiocruz Amazonia, Inst Leonidas & Maria Deane, Manaus, Amazonas, Brazil. EM fernando@amazonia.fiocruz.br RI Ferraz, Goncalo/C-3860-2008; Abad-Franch, Fernando/L-4741-2013; OI Ferraz, Goncalo/0000-0001-8748-0462; Grijalva, Mario/0000-0003-1964-1425 FU UNICEF/UNDP/World Bank/WHO TDR [A20441, 970195]; Fiocruz-CNPq; Fiocruz-Fapeam (Brazil); Tropical Disease Institute, Ohio University FX Funding was received from the UNICEF/UNDP/World Bank/WHO TDR Special Programme (grants A20441 and 970195), with additional support from the Fiocruz-CNPq and Fiocruz-Fapeam agreements (Brazil). This work also benefited from international collaboration through the ECLAT Network. Fieldwork in Ecuador was partially supported by the Tropical Disease Institute, Ohio University. Funding agencies had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 64 TC 33 Z9 34 U1 3 U2 15 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1935-2735 J9 PLOS NEGLECT TROP D JI Plos Neglect. Trop. Dis. PD MAR PY 2010 VL 4 IS 3 AR e620 DI 10.1371/journal.pntd.0000620 PG 11 WC Infectious Diseases; Parasitology; Tropical Medicine SC Infectious Diseases; Parasitology; Tropical Medicine GA 578RG UT WOS:000276312200033 PM 20209149 ER PT J AU Azpurua, J De La Cruz, D Valderama, A Windsor, D AF Azpurua, Jorge De La Cruz, Dianne Valderama, Anayansi Windsor, Donald TI Lutzomyia Sand Fly Diversity and Rates of Infection by Wolbachia and an Exotic Leishmania Species on Barro Colorado Island, Panama SO PLOS NEGLECTED TROPICAL DISEASES LA English DT Article ID POLYMERASE-CHAIN-REACTION; CUTANEOUS LEISHMANIASIS; CYTOPLASMIC INCOMPATIBILITY; PHLEBOTOMINE SANDFLIES; DNA BARCODES; MITOCHONDRIAL-DNA; KINETOPLAST DNA; CULEX-PIPIENS; FLIES DIPTERA; PSYCHODIDAE AB Background: Sand flies ( Diptera, Psychodidae, Phlebotominae) in the genus Lutzomyia are the predominant vectors of the protozoan disease leishmaniasis in the New World. Within the watershed of the Panama Canal, the cutaneous form of leishmaniasis is a continuous health threat for residents, tourists and members of an international research community. Here we report the results of screening a tropical forest assemblage of sand fly species for infection by both Leishmania and a microbe that can potentially serve in vector population control, the cytoplasmically transmitted rickettsia, Wolbachia pipientis. Knowing accurately which Lutzomyia species are present, what their evolutionary relationships are, and how they are infected by strains of both Leishmania and Wolbachia is of critical value for building strategies to mitigate the impact of this disease in humans. Methodology and Findings: We collected, sorted and then used DNA sequences to determine the diversity and probable phylogenetic relationships of the Phlebotominae occurring in the understory of Barro Colorado Island in the Republic of Panama. Sequence from CO1, the DNA barcoding gene, supported 18 morphology-based species determinations while revealing the presence of two possible "cryptic'' species, one (Lu. sp. nr vespertilionis) within the Vespertilionis group, the other ( Lu. gomezi) within the Lutzomyia-cruciata series. Using ITS-1 and "minicircle'' primers we detected Leishmania DNA in 43.3% of Lu. trapidoi, 26.3% of Lu. gomezi individuals and in 0% of the other 18 sand fly species. Identical ITS-1 sequence was obtained from the Leishmania infecting Lu. trapidoi and Lu. gomezi, sequence which was 93% similar to Leishmania ( viannia) naiffi in GenBank, a species previously unknown in Panama, but recognized as a type of cutaneous leishmaniasis vectored broadly across northern and central South America. Distinct strains of the intracellular bacterium Wolbachia were detected in three of 20 sand fly species, including Lu. trapidoi, in which it frequently co-occurred with Leishmania. Conclusions: Both morphological and molecular methods were used to examine an assemblage of 20 sand fly species occurring in the forests of the Panama Canal area. Two of these species, members of separate clades, were found to carry Leishmania at high frequency and hence are likely vectors of leishmaniasis to humans or other mammal species. A single Leishmania species, identified with high confidence as Le. naiffi, was carried by both species. That Le. naiffi is known to cause cutaneous lesions in South America but has hitherto not been reported or implicated in Panama opens the possibility that its range has recently expanded to include the Isthmus or that it occurs as a recent introduction. The occurrence of Leishmania and Wolbachia in Lu. trapidoi identifies one important vector of the disease as a potential target for gene introductions using Wolbachia population sweeps. C1 [Azpurua, Jorge; De La Cruz, Dianne; Windsor, Donald] Smithsonian Trop Res Inst, Panama City, Panama. [Valderama, Anayansi] Inst Conmemorat Gorgas Estudios Salud, Panama City, Panama. RP Azpurua, J (reprint author), Smithsonian Trop Res Inst, Panama City, Panama. EM windsord@si.edu FU NSF [EF-0328363] FX NSF (http://www.nsf.gov/) grant EF-0328363. Fundacion Gabriel Lewis Galindo (http://www.fglg.org.pa/), Republic of Panama. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 64 TC 36 Z9 38 U1 0 U2 8 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 185 BERRY ST, STE 1300, SAN FRANCISCO, CA 94107 USA SN 1935-2727 J9 PLOS NEGLECT TROP D JI Plos Neglect. Trop. Dis. PD MAR PY 2010 VL 4 IS 3 AR e627 DI 10.1371/journal.pntd.0000627 PG 9 WC Infectious Diseases; Parasitology; Tropical Medicine SC Infectious Diseases; Parasitology; Tropical Medicine GA 578RG UT WOS:000276312200025 PM 20231892 ER PT J AU Fonseca, AC Guzman, HM Cortes, J Soto, C AF Fonseca, A. C. Guzman, Hector M. Cortes, Jorge Soto, Carlomagno TI Marine habitats map of "Isla del Cano", Costa Rica, comparing Quickbird and Hymap images classification results SO REVISTA DE BIOLOGIA TROPICAL LA English DT Article DE marine habitat map; coral reef; Costa Rica; Isla del Cano; Hymap; Quickbird ID CORAL-REEFS; SOUTH-PACIFIC; IKONOS; ENVIRONMENTS; DISTURBANCE; RESILIENCE; PANAMA AB Isla del Carlo is a marine protected area on the south Pacific coast of Costa Rica, surrounded by coral reefs and coral communities. The ecology of these coral reefs has been studied for over 20 years, but they have not been mapped. Maps are considered a great research, planning, management and monitoring tool. Medium to high resolution images (HyMap 2005 and Quickbird 2007 respectively) were processed and classified in order to test and compare their accuracy in producing a marine habitat map. Manta tow surveys were performed in the field for identification of 7 marine habitats 1. Coral community; 2. Coral reef; 3. Bed rock; 4. Sand; 5. Sand with boulders; 6. Sand with rodolyths; and 7. Deep water. The overall accuracy was slightly higher using Quickbird (87%) than using Hymap (60%), however the difference was not significant. The map produced using Quickbird was selected to represent the marine habitats of Isla del Cano. This map will help to analyze the adequate size and zoning of the marine protected area. Rev. Biol. Trop. 58(1): 373-381. Epub 2010 March 01. C1 [Fonseca, A. C.; Cortes, Jorge] Univ Costa Rica, Ctr Invest Ciencias Mar & Limnol CIMAR, San Jose 115012060, Costa Rica. [Fonseca, A. C.; Cortes, Jorge] Univ Costa Rica, Escuela Biol, San Jose 115012060, Costa Rica. [Guzman, Hector M.] Smithsonian Trop Res Inst, Ancon, Panama. [Fonseca, A. C.; Cortes, Jorge] Nature Conservancy, San Jose 2301225, Costa Rica. [Soto, Carlomagno] Ctr Nacl Alta Tecnol, San Jose 1174, Costa Rica. RP Fonseca, AC (reprint author), Univ Costa Rica, Ctr Invest Ciencias Mar & Limnol CIMAR, San Jose 115012060, Costa Rica. EM ana.fonsecaescalante@ucr.ac.cr; guzmanh@si.edu; jorge.cortes@ucr.ac.cr; csoto@conare.ac.cr RI Soto Castro, Carlomagno/G-6510-2014 OI Soto Castro, Carlomagno/0000-0002-1916-9549 FU Smithsonian Tropical Research Institute; TNC [CR-OSA0038S] FX Thanks to O. Breedy, J.J. Alvarado, C. Fernandez, A. Segura, E. Ruiz, C. Sevilla, M. Montero, C. Benavidez, D. Torres and the crew of the Phoenix for their help. We also thank L. Handley, from USGS, for the meticulous revision of the English language and content of this manuscript. This study was elaborated by CIMAR and the Smithsonian Tropical Research Institute, under contract #CR-OSA0038S from TNC, as part of their conservation activities in ACOSA. NR 31 TC 4 Z9 4 U1 0 U2 5 PU REVISTA DE BIOLOGIA TROPICAL PI SAN JOSE PA UNIVERSIDAD DE COSTA RICA CIUDAD UNIVERSITARIA, SAN JOSE, COSTA RICA SN 0034-7744 J9 REV BIOL TROP JI Rev. Biol. Trop. PD MAR PY 2010 VL 58 IS 1 BP 373 EP 381 PG 9 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 585VU UT WOS:000276859100027 PM 20411729 ER PT J AU Clough, GW AF Clough, G. Wayne TI Becoming Us 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 MAR PY 2010 VL 40 IS 12 BP 16 EP 16 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 557YE UT WOS:000274705600012 ER PT J AU Turner, BL Romero, TE AF Turner, Benjamin L. Romero, Tania E. TI Stability of hydrolytic enzyme activity and microbial phosphorus during storage of tropical rain forest soils SO SOIL BIOLOGY & BIOCHEMISTRY LA English DT Article DE Panama; Phosphatase; Phosphomonoesterase; Phosphodiesterase; beta-Glucosidase; N-Acetyl-beta-D-glucosaminidase; Tropical forest soil; Enzymes; Microbial phosphorus ID SIZE FRACTIONS; PHOSPHATASE; PASTURE; BIOMASS; TEMPERATURE; NUTRIENTS; COMMUNITY; SUCROSE; DROUGHT; STARCH AB Storage can markedly influence microbial and biochemical properties in soils, yet recommendations for sample storage are based on studies of temperate soils that regularly experience extended cold periods. We assessed the influence of storage conditions on microbial phosphorus and the activity of four hydrolytic enzymes (phosphomonoesterase, phosphodiesterase, beta-glucosidase, and N-acetyl-beta-D-glucosaminidase) in three lowland tropical forest soils from the Republic of Panama that experience a constant warm temperature. The soils spanned a strong rainfall gradient and contained contrasting physical and chemical properties (pH 3.6-5.9; total carbon 26-50 g C kg(-1); clay 33-62%: total phosphorus 0.30-0.60 g P kg(-1)). Storage treatments were: (i) room temperature (22 degrees C in the dark), (ii) refrigerated (4 degrees C in the dark), (iii) air-dried (10 d, 22 degrees C) and (iv) frozen (-35 degrees C). There were significant changes in enzyme activities and microbial phosphorus during refrigerated and room temperature storage, although changes were relatively small during the first two weeks. An initial marked decline in enzyme activities for one soil analyzed within 2 h of sampling was attributed to a flush of activity caused by sampling and soil preparation (sieving, etc.). For longer-term storage (>2 weeks), ambient laboratory temperature appeared preferable to freezing and cold storage, because one month of storage caused a marked decline in enzyme activities and microbial phosphorus in one soil. Freezing preserved the activities of some enzymes in some soils at rates comparable to cold or room temperature storage, but caused a marked decline in microbial phosphorus in two soils. Air-drying caused a marked decline in microbial phosphorus and the activity of all enzymes. We therefore conclude that enzyme assays and microbial phosphorus should be determined in tropical forest soils after no more than two weeks storage in the dark at ambient laboratory temperature. Published by Elsevier Ltd. C1 [Turner, Benjamin L.; Romero, Tania E.] 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 35 TC 28 Z9 29 U1 3 U2 41 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0038-0717 J9 SOIL BIOL BIOCHEM JI Soil Biol. Biochem. PD MAR PY 2010 VL 42 IS 3 BP 459 EP 465 DI 10.1016/j.soilbio.2009.11.029 PG 7 WC Soil Science SC Agriculture GA 559PX UT WOS:000274839400008 ER PT J AU Scarbrough, AG Perez-Gelabert, DE AF Scarbrough, A. G. Perez-Gelabert, Daniel E. TI A new species of Martintella Artigas, 1996 from the islands of Tobago and Trinidad (Diptera: Asilidae) SO TRANSACTIONS OF THE AMERICAN ENTOMOLOGICAL SOCIETY LA English DT Article DE Diptera; Asilidae; Martintella; new species; Tobago; Trinidad AB The genus Martintella Artigas, 1996, is recorded from the islands of Tobago and Trinidad for the first time. M. elliptica sp. nov from Tobago and Trinidad is described and illustrated. M. elliptica is compared to M. testes (Williston). C1 [Perez-Gelabert, Daniel E.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. RP Scarbrough, AG (reprint author), Univ Arizona, Dept Entomol, Insect Museum, Forbes 410, Tucson, AZ 85721 USA. NR 11 TC 1 Z9 1 U1 0 U2 0 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 MAR-JUN PY 2010 VL 136 IS 1-2 BP 193 EP 198 DI 10.3157/061.136.0206 PG 6 WC Entomology SC Entomology GA 620EH UT WOS:000279481300006 ER PT J AU Soltis, J Brown, JL AF Soltis, Joseph Brown, Janine L. TI Special Issue-The Care and Welfare of Elephants in AZA Institutions SO ZOO BIOLOGY LA English DT Editorial Material C1 [Brown, Janine L.] Smithsonian Inst, Ctr Species Survival, Conservat & Res Ctr, Front Royal, VA USA. [Soltis, Joseph] Disneys Anim Kingdom, Educ & Sci, Lake Buena Vista, FL USA. RP Brown, JL (reprint author), Smithsonian Inst, Ctr Species Survival, Conservat & Res Ctr, Natl Zool Pk, Front Royal, VA USA. EM brownjan@si.edu NR 0 TC 3 Z9 3 U1 1 U2 22 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0733-3188 J9 ZOO BIOL JI Zoo Biol. PD MAR-APR PY 2010 VL 29 IS 2 SI SI BP 85 EP 86 DI 10.1002/zoo.20297 PG 2 WC Veterinary Sciences; Zoology SC Veterinary Sciences; Zoology GA 592CD UT WOS:000277351700001 PM 20014013 ER PT J AU Proctor, CM Freeman, EW Brown, JL AF Proctor, Christine M. Freeman, Elizabeth W. Brown, Janine L. TI Results of a Second Survey to Assess the Reproductive Status of Female Asian and African Elephants in North America SO ZOO BIOLOGY LA English DT Article DE hormones; ovarian cyclicity; estrous cycle; ultrasound; progestagens ID LOXODONTA-AFRICANA; MANAGEMENT; SUPPRESSION; CORTISOL; MAXIMUS; POPULATION; MARMOSETS; BEHAVIOR; FAILURE; FAMILY AB Surveys are being conducted to monitor the reproductive health of elephants managed by the TAG/SSP. This study summarizes results of a 2005 survey and compares data to one conducted in 2002. Surveys were returned for 100% and 79.0% of Asian and African elephants, respectively. Of those, 79.3% of Asian and 92.1% of African elephants had weekly progestagen data to assess ovarian cyclicity. For Asian elephants, acyclicity rates were similar between the 2002 and 2005 surveys (13.3% versus 10.9%), whereas irregular cycling increased in 2005 (2.6% versus 7.6%), respectively. For African elephants, the percentages of both acyclicity (22.0% versus 31.2%) and irregular cycling females (5.2% versus 11.8%) increased. In both species, ovarian inactivity was more prevalent in the older age categories (>30 years of age), but for African elephants also occurred in the reproductive aged groups. Reproductive tract pathologies did not account for the majority of acyclicity problems. Several females changed cyclicity status between the two surveys, including from noncycling to cycling, suggesting this is not an irreversible condition. However, seven African females went from cycling to abnormal or no cyclic activity. In summary, the incidence of ovarian acyclicity in Asian elephants is low and stable, but appears to be increasing in African females. These findings reinforce the need for long-term reproductive monitoring programs and continuous reproductive surveys, even for females not being considered for breeding. With more data we hope to determine what factors are related to changes in ovarian status and how to reverse the trend towards acyclicity. Zoo Biol 29:127-139, 2010. (C) 2009 Wiley-Liss, Inc. C1 [Proctor, Christine M.; Freeman, Elizabeth W.; Brown, Janine L.] Smithsonian Natl Zool Pk, Dept Reprod Sci, Conservat & Res Ctr, Front Royal, CA 22630 USA. RP Brown, JL (reprint author), Smithsonian Natl Zool Pk, Dept Reprod Sci, Conservat & Res Ctr, 1500 Remount Rd, Front Royal, CA 22630 USA. EM brownjan@si.edu FU Siemens Medical Diagnostic Solutions; International Elephant Foundation; Morris Animal Foundation; National Zoo FX The authors would like to thank Karen Lewis, Mike Keele, and Debbie Olson for their assistance in collecting survey results as well as taking on the arduous task of maintaining the North American elephant studbooks. The authors would also like to thank Nicole Abbondanza for technical assistance. This project was funded in part by Siemens Medical Diagnostic Solutions, International Elephant Foundation, Morris Animal Foundation, Shared Earth Foundation and Friends of the National Zoo. NR 30 TC 17 Z9 17 U1 0 U2 17 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0733-3188 J9 ZOO BIOL JI Zoo Biol. PD MAR-APR PY 2010 VL 29 IS 2 SI SI BP 127 EP 139 DI 10.1002/zoo.20238 PG 13 WC Veterinary Sciences; Zoology SC Veterinary Sciences; Zoology GA 592CD UT WOS:000277351700005 PM 20391465 ER PT J AU Freeman, EW Schulte, BA Brown, JL AF Freeman, Elizabeth W. Schulte, Bruce A. Brown, Janine L. TI Investigating the Impact of Rank and Ovarian Activity on the Social Behavior of Captive Female African Elephants SO ZOO BIOLOGY LA English DT Article DE Loxodonta africana; African elephant; acyclicity; social rank; behavior ID NAKED MOLE-RATS; LOXODONTA-AFRICANA; CHEMICAL COMMUNICATION; HETEROCEPHALUS-GLABER; ASIAN ELEPHANTS; SUPPRESSION; ENDOCRINOLOGY; CYCLICITY; DOMINANCE; STATE AB Over a third of captive female African elephants in North America fail to exhibit normal estrous cycles based on long-term serum progestagen analyses. Why acyclicity occurs is unknown; however, the majority of noncycling females are ranked by keepers as the dominant individual within the group. To investigate the relationship between ovarian cyclicity status and keeper-determined social rank, observations were conducted on 33 female African elephants (18 cycling, 15 noncycling). Based on keeper evaluations, five cycling elephants were ranked dominant, seven in the middle and six as subordinate. In contrast, 10 noncycling elephants were ranked as dominate and five as subordinate with none ranked as middle. When comparing the behavior of the elephants by their keeper-determined rank, the dominant females dominant were significantly more likely to approach, displace and push. Similarly, keeper-determined subordinate females more frequently presented their hind end and held their ears erect. Behaviors initiated by one elephant toward another did not vary between cycling and noncycling females, except when the interaction with social rank was tested. Dominant, noncycling females initiated a higher percentage of "approach" and "displace" behaviors than both cycling and noncycling, subordinate elephants. Subordinate, noncycling elephants displayed the highest percentage of "ears erect." Social rank drives the interactions of ex situ female African elephants more than ovarian cyclicity status. Thus, behavioral interactions cannot be used to predict which cycling elephants are most likely to become acyclic. Zoo Biol 29:154-167, 2010. (C) 2009 Wiley-Liss, Inc. C1 [Freeman, Elizabeth W.] George Mason Univ, New Century Coll, Dept Environm Sci & Policy, Fairfax, VA 22030 USA. [Schulte, Bruce A.] Georgia So Univ, Dept Biol, Statesboro, GA 30460 USA. [Freeman, Elizabeth W.; Brown, Janine L.] Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA USA. RP Freeman, EW (reprint author), George Mason Univ, New Century Coll, Dept Environm Sci & Policy, 4400 Univ Dr,Ms 5D3, Fairfax, VA 22030 USA. EM efreeman@gmu.edu FU Robison Family Foundation; Smithsonian Scholarly Studies program; Smithsonian Women's Committee; Siemens Medical Diagnostics Corporation; National Zoo; George Mason University; National Science Foundation [NSF-DBI-02-17062]; Georgia Southern University FX Grant sponsors: The Robison Family Foundation; The Smithsonian Scholarly Studies program; The Smithsonian Women's Committee; The Siemens Medical Diagnostics Corporation; The National Zoo; George Mason University; The National Science Foundation; Grant number: NSF-DBI-02-17062; Grant sponsor: Georgia Southern University. NR 42 TC 8 Z9 8 U1 1 U2 22 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0733-3188 J9 ZOO BIOL JI Zoo Biol. PD MAR-APR PY 2010 VL 29 IS 2 SI SI BP 154 EP 167 DI 10.1002/zoo.20235 PG 14 WC Veterinary Sciences; Zoology SC Veterinary Sciences; Zoology GA 592CD UT WOS:000277351700007 PM 20391466 ER PT J AU Proctor, CM Freeman, EW Brown, JL AF Proctor, Christine M. Freeman, Elizabeth W. Brown, Janine L. TI Influence of Dominance Status on Adrenal Activity and Ovarian Cyclicity Status in Captive African Elephants SO ZOO BIOLOGY LA English DT Article DE dominance; ovarian cyclicity; cortisol ID LOXODONTA-AFRICANA; REPRODUCTIVE PROBLEMS; LUTEINIZING-HORMONE; ASIAN ELEPHANTS; STRESS; CORTISOL; BEHAVIOR; POPULATION; HEALTH; DETERMINANTS AB The North American African (Loxodonta africana) elephant population is not self-sustaining, in part because of a high rate of abnormal ovarian activity. About 12% of adult females exhibit irregular cycles and 31% do not cycle at all. Our earlier work revealed a relationship between dominance status and ovarian acyclicity. with dominant females being more likely to not cycle normally. One theory is that dominant females may be expending more energy to maintaining peace within the captive herd than for supporting reproduction. The goal of this study was to determine if there was a relationship among dominance status, serum cortisol concentrations, and ovarian acyclicity. We hypothesized that adrenal glucocorticoid activity would be increased in dominant, noncycling elephants as compared with subdominant individuals. Blood samples were collected weekly over a 2-year period in 81 females of known dominance and cyclicity status, and analyzed for cortisol. Based on a path analysis model (Reticular Action Model Or Near Approximation [RAMONA]), noncycling, dominant African elephant females did not have higher mean serum cortisol concentrations, or exhibit more variability (i.e., coefficient of variation, standard deviation) in cortisol secretion. This study suggests that alterations in adrenal activity are not related to dominance status nor contribute directly to acyclicity in captive African elephants. Zoo Biol 29:168-178, 2010. (C) 2009 Wiley-Liss, Inc. C1 [Proctor, Christine M.; Brown, Janine L.] Smithsonian Natl Zool Pk, Conservat & Res Ctr, Dept Reprod Sci, Front Royal, VA 22630 USA. [Freeman, Elizabeth W.] George Mason Univ, New Century Coll, Fairfax, VA 22030 USA. RP Brown, JL (reprint author), Smithsonian Natl Zool Pk, Conservat & Res Ctr, Dept Reprod Sci, 1500 Remount Rd, Front Royal, VA 22630 USA. EM brownjan@si.edu FU Siemens Medical Solutions Diagnostics; Shared Earth Foundation; National ZooMorris Animal Foundation FX Grant sponsors: Siemens Medical Solutions Diagnostics; Shared Earth Foundation; National Zoo; Morris Animal Foundation. NR 64 TC 8 Z9 8 U1 1 U2 11 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0733-3188 J9 ZOO BIOL JI Zoo Biol. PD MAR-APR PY 2010 VL 29 IS 2 SI SI BP 168 EP 178 DI 10.1002/zoo.20292 PG 11 WC Veterinary Sciences; Zoology SC Veterinary Sciences; Zoology GA 592CD UT WOS:000277351700008 PM 20033989 ER PT J AU Plotnik, JM de Waal, FBM Moore, D Reiss, D AF Plotnik, Joshua M. de Waal, Frans B. M. Moore, Donald, III Reiss, Diana TI Self-Recognition in the Asian Elephant and Future Directions for Cognitive Research With Elephants in Zoological Settings SO ZOO BIOLOGY LA English DT Article DE elephants; cognition; mirror self-recognition; animal behavior ID BOTTLE-NOSED DOLPHINS; CHIMPANZEES PAN-TROGLODYTES; TOOL-USE; CULTURAL TRANSMISSION; CAPTIVE ELEPHANTS; PONGO-PYGMAEUS; EVOLUTION; BEHAVIOR; MAXIMUS; MIRROR AB The field of animal cognition has grown steadily for nearly four decades, but the primary focus has centered on easily kept lab animals of varying cognitive capacity, including rodents, birds and primates. Elephants (animals not easily kept in a laboratory) are generally thought of as highly social, cooperative, intelligent animals, yet few studies with the exception of long-term behavioral field studies have been conducted to directly support this assumption. In fact, there has been remarkably little cognitive research conducted on Asian (Elephas maximus) or African (Lexodonta africana or L. cyclotis) elephants. Here, we discuss the opportunity and rationale for conducting such research on elephants in zoological facilities, and review some of the recent developments in the field of elephant cognition, including our recent study on mirror self-recognition in E. maximus. Zoo Biol 29:179-191, 2010. (C) 2009 Wiley-Liss. Inc. C1 [Plotnik, Joshua M.; de Waal, Frans B. M.] Emory Univ, Dept Psychol, Atlanta, GA 30322 USA. [Plotnik, Joshua M.; de Waal, Frans B. M.] Emory Univ, Yerkes Natl Primate Res Ctr, Atlanta, GA 30322 USA. [Moore, Donald, III] Smithsonian Inst, Natl Zool Pk, Washington, DC 20008 USA. [Reiss, Diana] CUNY Hunter Coll, Dept Psychol, New York, NY 10021 USA. RP Plotnik, JM (reprint author), Emory Univ, Dept Psychol, 532 N Kilgo Circle, Atlanta, GA 30322 USA. EM Joshua.Plotnik@emory.edu NR 88 TC 11 Z9 11 U1 16 U2 110 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0733-3188 J9 ZOO BIOL JI Zoo Biol. PD MAR-APR PY 2010 VL 29 IS 2 SI SI BP 179 EP 191 DI 10.1002/zoo.20257 PG 13 WC Veterinary Sciences; Zoology SC Veterinary Sciences; Zoology GA 592CD UT WOS:000277351700009 PM 19514017 ER PT J AU Brown, JL Kersey, DC Freeman, EW Wagener, T AF Brown, Janine L. Kersey, David C. Freeman, Elizabeth W. Wagener, Tarren TI Assessment of Diurnal Urinary Cortisol Excretion in Asian and African Elephants Using Different Endocrine Methods SO ZOO BIOLOGY LA English DT Article DE immunoassay; adrenal activity; glucocorticoids; diurnal ID DEER CERVUS-ELAPHUS; LOXODONTA-AFRICANA; CIRCADIAN-RHYTHM; STRESS; MAXIMUS; SLEEP; TEMPERATURE; SECRETION; BEHAVIOR; PLASMA AB Longitudinal urine samples were collected from Asian and African elephants to assess sample processing and immunoassay techniques for monitoring adrenal activity. Temporal profiles of urinary cortisol measured by RIA and EIA, with and without dichloromethane extraction, were similar; all correlation coefficients were >0.90. However, based on regression analyses, cortisol immunoactivity in extracted samples was only 72-81% of that of unextracted values. Within assay technique, RIA values were only 74-81% of El A values. Collection of 24-hr urine samples demonstrated a clear diurnal pattern of glucocorticoid excretion, with the lowest concentrations observed just before midnight and peak concentrations occurring around 0600-0800 hr. These results indicate that elephants fit the pattern of a diurnal species, and that glucocorticoid production is affected by a sleep-wake cycle similar to that described for other terrestrial mammals. Cortisol can be measured in both extracted and unextracted urine using RIA and EIA methodologies. However, unexplained differences in quantitative results suggest there may be sample matrix effects and that data generated using different techniques may not be directly comparable or interchangeable. Zoo Biol 29:274-283, 2010. (C) 2009 Wiley-Liss, Inc. C1 [Brown, Janine L.; Kersey, David C.; Freeman, Elizabeth W.] Smithsonians Natl Zool Pk, Dept Reprod Sci, Conservat & Res Ctr, Front Royal, VA USA. [Freeman, Elizabeth W.] George Mason Univ, New Century Coll, Fairfax, VA 22030 USA. [Wagener, Tarren] Ft Worth Zoo, Ft Worth, TX USA. RP Brown, JL (reprint author), Smithsonians Natl Zool Pk, Dept Reprod Sci, Conservat & Res Ctr, 1500 Remount Rd, Front Royal, VA USA. EM brownjan@si.edu FU Friends of the National Zoo; International Elephant Foundation; Siemens Medical Diagnostic Solutions FX Grant sponsors: Friends of the National Zoo; International Elephant Foundation; Siemens Medical Diagnostic Solutions. NR 34 TC 12 Z9 12 U1 1 U2 14 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0733-3188 J9 ZOO BIOL JI Zoo Biol. PD MAR-APR PY 2010 VL 29 IS 2 SI SI BP 274 EP 283 DI 10.1002/zoo.20268 PG 10 WC Veterinary Sciences; Zoology SC Veterinary Sciences; Zoology GA 592CD UT WOS:000277351700015 PM 19670316 ER PT J AU Kim, G Lee, CW Kim, J Lee, Y Ballesteros-Paredes, J Myers, PC Kurtz, S AF Kim, Gwanjeong Lee, Chang Won Kim, Jongsoo Lee, Youngung Ballesteros-Paredes, Javier Myers, Philip C. Kurtz, S. TI ASSOCIATION OF INFRARED DARK CLOUD CORES WITH YSOS: STARLESS OR STARRED IRDC CORES SO JOURNAL OF THE KOREAN ASTRONOMICAL SOCIETY LA English DT Article DE catalogs; dust, extinction; galaxy: general; infrared: ISM; ISM: clouds; ISM: structure ID MIDCOURSE-SPACE-EXPERIMENT; SPITZER C2D SURVEY; NEARBY DENSE CORES; MASSIVE STARS; PHYSICAL-PROPERTIES; MOLECULAR CLOUDS; COLD CORES; POPULATION; CATALOG; DISCOVERY AB In this paper we examined the association of InfraRed Dark Cloud (IRDC) cores with YSOs and the geometric properties of the IRDC cores. For this study a total of 13,650 IRDC cores were collected mainly from the catalogs of the IRDC cores published from other studies and partially from our catalog of IRDC cores containing new 789 IRDC core candidates. The YSO candidates were searched for using the GLIMPSE, MSX, and IRAS point sources by the shape of their SED or using activity of water or methanol maser. The association of the IRDC cores with these YSOs was checked by their line-of-sight coincidence within the dimension of the IRDC core. This work found that a total of 4,110 IRDC cores have YSO candidates while 9,540 IRDC cores have no indication of the existence of YSOs. Considering the 12,200 IRDC cores within the GLIMPSE survey region for which the YSO candidates were determined with better sensitivity, we found that 4,098 IRDC cores (34%) have at least one YSO candidate and 1,072 cores among them seem to have embedded YSOs, while the rest; 8,102 (66%) have no YSO candidate. Therefore, the ratio of [N(IRDC core with protostars)]/[N(IRDC core without YSO)] for 12,200 IRDC cores is about 0.13. Taking into account this ratio and typical lifetime of high-mass embedded YSOs, we suggest that the IRDC cores would spend about 10(4)similar to 10(5) years to form high-mass stars. However, we should note that the GLIMPSE point sources have a. minimum detectable luminosity lof about 1.2 L(circle dot) at a typical IRDC core's distance of similar to 4 kpc. Therefore, the ratio given here should be a, lower limit and the estimated lifetime of starless IRDC cores can be an upper limit. The physical parameters of the IRDC cores somewhat vary depending on how many YSO candidates the IRDC cores contain. The IRDC cores with more YSOs tend to be larger, more elongated, and have better darkness contrast than the IRDC cores with fewer or no YSOs. C1 [Kim, Gwanjeong; Lee, Chang Won; Kim, Jongsoo; Lee, Youngung] Korea Astron & Space Sci Inst, Int Ctr Astrophys, Taejon 305348, South Korea. [Kim, Gwanjeong; Lee, Chang Won; Kim, Jongsoo] Univ Sci & Technol, Dept Astron & Space Sci, Taejon 305333, South Korea. [Ballesteros-Paredes, Javier; Kurtz, S.] Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico. [Myers, Philip C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kim, G (reprint author), Korea Astron & Space Sci Inst, Int Ctr Astrophys, 61-1 Hwaam Dong, Taejon 305348, South Korea. EM archer81@kasi.re.kr; cwl@kasi.re.kr FU Korea Science [KOSEF R01-2003-000-10513-0]; UNAM-PAPIIT [110606]; National Aeronautics and Space Administration FX This research was supported by the Basic Research Program (KOSEF R01-2003-000-10513-0) of the Korea Science. J.B.P acknowledges support from UNAM-PAPIIT grant 110606. This research has made use of the NASA/IPAC InfraRed Science Archive (MSX, IRAS, and Spitzer), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research also has made use of Arcetri Catalog of water masers (Valadettaro et al. 2001) and the General Catalog of 6.7 GHz methanol masers (Pestalozzi &, Minnier 2003). NR 52 TC 4 Z9 4 U1 0 U2 4 PU KOREAN ASTRONOMICAL SOCIETY PI TAEJON PA 61-1 HWA-AM DONG, YUSUNG KU, TAEJON, 305-348, SOUTH KOREA SN 1225-4614 J9 J KOREAN ASTRON SOC JI J. Korean Astron. Soc. PD FEB 28 PY 2010 VL 43 IS 1 BP 9 EP 23 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 565MZ UT WOS:000275299100002 ER PT J AU Lada, CJ AF Lada, Charles J. TI The physics and modes of star cluster formation: observations SO PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY A-MATHEMATICAL PHYSICAL AND ENGINEERING SCIENCES LA English DT Review DE star formation; star clusters; cluster formation ID INITIAL MASS FUNCTION; INFRARED DARK CLOUDS; YOUNG STELLAR OBJECTS; SCUTUM-CRUX ARM; X-RAY-EMISSION; MOLECULAR CLOUDS; EMBEDDED CLUSTERS; GALACTIC CLUSTERS; RED SUPERGIANTS; DISK EVOLUTION AB Stellar clusters are born in cold and dusty molecular clouds and the youngest clusters are embedded to various degrees in a dusty dark molecular material. Such embedded clusters can be considered protocluster systems. The most deeply buried examples are so heavily obscured by dust that they are only visible at infrared wavelengths. These embedded protoclusters constitute the nearest laboratories for a direct astronomical investigation of the physical processes of cluster formation and early evolution. I review the present state of empirical knowledge concerning embedded-cluster systems and discuss the implications for understanding their formation and subsequent evolution to produce bound stellar clusters. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Lada, CJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM clada@cfa.harvard.edu NR 59 TC 26 Z9 26 U1 0 U2 0 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 1364-503X J9 PHILOS T R SOC A JI Philos. Trans. R. Soc. A-Math. Phys. Eng. Sci. PD FEB 28 PY 2010 VL 368 IS 1913 BP 713 EP 731 DI 10.1098/rsta.2009.0264 PG 19 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 544ZY UT WOS:000273702000002 PM 20083503 ER PT J AU Robbins, RK Busby, R Duarte, M AF Robbins, Robert K. Busby, Robert Duarte, Marcelo TI Phylogeny and Taxonomy of the Neotropical Thepytus (Lepidoptera: Lycaenidae: Theclinae) SO ARTHROPOD SYSTEMATICS & PHYLOGENY LA English DT Article DE Andes; Beatheclus; biological control; colonization of lowlands; implied weighting ID BUTTERFLIES LEPIDOPTERA; EUMAEINI; DIVERSIFICATION; PATTERNS; HUBNER; GENUS AB The Neotropical lycaenid hairstreak genus Thepytus Robbins and its eight species are revised. Species treatments summarize nomenclature, distribution, habitat, behavior, and diagnostic traits, as well as noting why each species is considered distinct under a biological species concept. An identification key for males and a checklist are included. Beatheclus Balint & Dahners new synonym is synonymized with Thepytus, and Theppus beatrizae (Balint & Dahners) is a new combination. Other nomenclatural actions include the description of Thepytus jennifer Busby & Robbins new species. Thepytus nancyana Busby & Robbins new species, and Thepytus carmen Robbins & Duarte new species. A lectotype is designated or Thecla thyrea Hewitson, 1867, to ensure stability of this name. A phylogenetic analysis based on 22 coded morphological characters yields one equal weight most parsimonious 39-step tree. Implied weighting does not change the tree topology. Unambiguous changes in elevation optimized on the cladogram show that a montane lineage of Thepytus colonized the lowlands in at least one instance. The use of T. echelta (Hewitson) as a biological control agent for Psittacanthus (Loranthaceae) is discussed. C1 [Robbins, Robert K.] Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA. [Duarte, Marcelo] Univ Sao Paulo, Museu Zool, BR-04263000 Sao Paulo, Brazil. RP Robbins, RK (reprint author), Smithsonian Inst, Dept Entomol, POB 37012,NHB Stop 105, Washington, DC 20013 USA. EM RobbinsR@SI.edu; rc.busby@comcast.net; mduartes@usp.br RI Duarte, Marcelo/K-7633-2012; Museu de Zoologia da USP, MZ-USP/Q-2192-2016 FU Fundacao de Amparo iPesquisa do Estado de Sao Paulo/FAPESP [02/13898-0, 03/139853]; Pro-Reitoria de Pesquisa da Universidade de Sao Paulo/USP/Projeto 1 FX We acknowledge the curators of public collections and the owners of private collections listed in the methods section for allowing us the opportunity to examine specimens under their care. Olaf Mielke, Gerardo Lamas, Christophe Faynel. and Jane Costa were especially helpful, and we are grateful to them. For help and Support of many kinds, WC gratefully acknowledge for this paper Curtis Callaghan. Astrid Caldas, Jason Hall. Gerardo Lamas, Andrea Martinson, and Marcio Zikan. We thank the Hennig Society, which makes TNT software freely available. We are grateful to Vichai Malikul and Glaucia Marconato for illustrating genitalia so expertly; to Kane Darrow for her mind-boggling graphics expertise: and to Brian Harris for technical support of many kinds. For supporting travel by both Duarte and Robbins and for substantial funds, we thank Fundacao de Amparo iPesquisa do Estado de Sao Paulo/FAPESP (as part of the project "Systematics, Bionomy, and Evolution of Neotropical Lepidoptera": process numbers 02/13898-0 and 03/139853) and Pro-Reitoria de Pesquisa da Universidade de Sao Paulo/USP/Projeto 1. For reading the manuscript with a critical eye. we thank Mirna Casagrande. Christophe Eaynel, Andre Freitas and Olaf Mielke. NR 38 TC 6 Z9 9 U1 0 U2 7 PU SENCKENBERG NATURHISTORISCHE SAMMLUNGEN DRESDEN, MUSEUM TIERKUNDE PI DRESDEN PA KOENIGSBRUECKER LANDSTRASSE 159, DRESDEN, 00000, GERMANY SN 1863-7221 EI 1864-8312 J9 ARTHROPOD SYST PHYLO JI Arthropod. Syst. Phylogeny PD FEB 26 PY 2010 VL 68 IS 1 BP 35 EP 52 PG 18 WC Entomology SC Entomology GA 580OJ UT WOS:000276458500002 ER PT J AU de Santana, CD Vari, RP AF de Santana, Carlos David Vari, Richard P. TI New Rheophilic Species of Electric Knifefish from the Rapids and Waterfalls of the Lower Rio Xingu, Brazil (Gymnotiformes: Apteronotidae) SO COPEIA LA English DT Article ID STERNARCHORHYNCHUS-CASTELNAU; AMAZON BASIN; FISH AB Sternarchogiton zuanoni, a new species of electric knifefish, is described from the rapids and waterfalls of Cachoeira de Kaituka along the Rio Xingu at Altamira, Pari, Brazil. The new species Is diagnosable from congeners by a unique combination of morphometric and meristic features, details of pigmentation, the pattern of dentition on the dentary, the possession of an edentulous premaxilla, and an unelaborated lower lip. The description of S. zuanoni brings the number of species in the genus to five. The presence of S. labiatus in the Rio Orinoco basin Is documented and a key to the species of the genus Is provided. C1 [Vari, Richard P.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Div Fishes, Washington, DC 20013 USA. RP Vari, RP (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Div Fishes, MRC-159,POB 37012, Washington, DC 20013 USA. EM apteronotidae@ig.com.br; varir@si.edu FU National Museum of Natural History, Smithsonian Institution; Herbert R. and Evelyn Axelrod Chair in Systematic Ichthyology in the Division of Fishes, National Museum of Natural History of the Smithsonian Institution FX Support for this project was provided by a Predoctoral Fellowship at the National Museum of Natural History, Smithsonian Institution, and 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. J. Alves-Gomes, J. Armbruster, L. Chao, B. Chernoff, J. Friel, K. Hartel, Z. Lucena, J. Lundberg, D. Nelson, F. Provenzano, L. Rapp Py-Daniel, R. Reis, M. Retzer, R. Robins, M. Rogers, and D. Taphorn provided access to specimens used in this study. F. Provenzano and D. Taphorn assisted with useful discussions on the gymnotiforms of the Rio Orinoco basin. Figure 1 was prepared by T. Griswold and Figure 2 by S. Raredon. NR 15 TC 4 Z9 6 U1 0 U2 6 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 FEB 26 PY 2010 IS 1 BP 160 EP 164 DI 10.1643/CI-09-068 PG 5 WC Zoology SC Zoology GA 564BI UT WOS:000275185500018 ER PT J AU de Santana, CD Crampton, WGR AF de Santana, Carlos David Crampton, William G. R. TI A Review of the South American Electric Fish Genus Porotergus (Gymnotiformes: Apteronotidae) with the Description of a New Species SO COPEIA LA English DT Review AB The species currently assigned to the South American electric fish genus Porotergus are reviewed. Porotergus duende, a new species, is described from the lowland western Amazon basin in Brazil and Peru. Porotergus gimbeli from the lowland Amazon basin in Brazil and Peru, and A gymnotus from the Essequibo drainage of Guyana are redescribed. Porotergus duende and P. gimbeli are restricted to deep channel habitats. Porotergus gymnotus occurs In shallow rivers. Notes on the ecology and electric organ discharge of A duende and P. gimbeli are presented. A key to the members of the genus is provided. C1 [de Santana, Carlos David; Crampton, William G. R.] Univ Cent Florida, Dept Biol, Orlando, FL 32816 USA. [de Santana, Carlos David] Smithsonian Inst, Dept Vertebrate Zool, Natl Museum Nat Hist, Div Fishes, Washington, DC 20013 USA. RP de Santana, CD (reprint author), Inst Nacl de Pesquisas da Amazonia, Av Andre Araujo, BR-2936 Manaus, Amazonas, Brazil. EM apteronotidae@ig.com.br FU National Science Foundation [DEB 9300151, DEB-0614334, DEB-0102593]; Instituto Nacional de Pesquisas da Amazonia; University of Central Florida; Conselho Nacional de Pesquisas e Desenvolvimento Tecnologico (CNPq) [38062/96-2, 381597/97-0 plus] FX J. Alves-Gomes, D. Catania, F. Lima, J. Lima Figueiredo, J. Lundberg, L. Page, L. Rapp Py-Daniel, M. Retzer, R. Robins, M. Rogers, M. Sabaj, R. Vari, P. Willink, and R. Winterbottom provided access to specimens. We acknowledge the Calhamazon Project (National Science Foundation DEB 9300151), J. Lundberg, PI, for making available a substantial portion of the specimens examined here. The authors are grateful to M. Hoang for the photograph of P. gymnotus. CDS is indebted to the Instituto Nacional de Pesquisas da Amazonia, a Smithsonian Predoctoral Fellowship in the Division of Fishes, National Museum of Natural History, and a Postdoctoral fellowship from the University of Central Florida. WGRC was funded by the Conselho Nacional de Pesquisas e Desenvolvimento Tecnologico (CNPq) (grants 38062/96-2 and 381597/97-0 plus extensions) and National Science Foundation (grants DEB-0614334 and DEB-0102593). Collecting was authorized by Instituto Mamiraua and IBAMA permit 0492/99-12 (and extensions) to WGRC. Animal care protocols follow CNPq guidelines. This paper benefited from comments by R. P. Vari and S. H. Weitzman. NR 24 TC 2 Z9 3 U1 1 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 FEB 26 PY 2010 IS 1 BP 165 EP 175 DI 10.1643/CI-05-136 PG 11 WC Zoology SC Zoology GA 564BI UT WOS:000275185500019 ER PT J AU Norrbom, AL Condon, M AF Norrbom, Allen L. Condon, Marty TI Revision of the femoralis group of Blepharoneura Loew (Diptera: Tephritidae) SO ZOOTAXA LA English DT Article DE Diptera; Tephritidae; taxonomy; phylogeny; host plant; Cucurbitaceae ID GURANIA-SPINULOSA; FRUIT-FLIES; CUCURBITACEAE; DIVERSITY AB The femoralis species group of the genus Blepharoneura is revised. The following 42 species, including 32 new species, are recognized: amplihyalina, n. sp. (northwestern Argentina), apaapa, n. sp. (Bolivia), aspiculosa, n. sp. (Mexico), bidigitata, n. sp. (southern Brazil), bipunctata, n. sp. (Ecuador), biseriata Wulp (Mexico), bivittata, n. sp. (Nicaragua, Costa Rica), brevivittata, n. sp. (Costa Rica to Peru), chaconi, n. sp. (Costa Rica), cornelli, n. sp. (Costa Rica), cyclantherae, n. sp. (Mexico), femoralis Wulp (Mexico to Brazil), fernandezi, n. sp. (Venezuela, northern Brazil), furcifer Hendel (Venezuela to Bolivia and Brazil), hirsuta Bates (Venezuela, Guyana, Brazil), hyalinella, n. sp. (Bolivia), io Giglio-Tos (Mexico), isolata, n. sp. (Guatemala), lutea, n. sp. (Costa Rica), macwilliamsae, n. sp. (Costa Rica), marshalli, n. sp. (northwestern Argentina), mexicana, n. sp. (Guatemala, Mexico), mikenoltei, n. sp. (Costa Rica), multipunctata, n. sp. (Ecuador), nigriapex, n. sp. (Bolivia), nigrifemur, n. sp. (Bolivia), osmundsonae, n. sp. (Mexico), punctistigma, n. sp. (Mexico to Costa Rica), quadristriata Wulp (Mexico to Costa Rica; possibly Colombia), quetzali, n. sp. (Guatemala), regina Giglio-Tos (Mexico), rupta (Wulp) (Mexico to Costa Rica), ruptafascia, n. sp. (Ecuador), septemdigitata, n. sp. (Peru, Bolivia), sinepuncta, n. sp. (Costa Rica), splendida Giglio-Tos (Mexico to Ecuador), tau, n. sp. (Costa Rica), thetis Hendel (southern Brazil), unifasciata, n. sp. (Ecuador), variabilis, n. sp. (Mexico), wasbaueri, n. sp. (Ecuador), and zumbadoi, n. sp. (Costa Rica). Blepharoneura amazonensis Lima & Leite, 1952 is considered a new synonym of B. hirsuta Bates, 1933, and a lectotype is designated for Blepharoneura furcifer Hendel, 1914. A key to species and phylogenetic analysis are provided, as well as descriptions, illustrations, distributions, and host plant data (as available) for each species. C1 [Norrbom, Allen L.] ARS, Systemat Entomol Lab, USDA, Smithsonian Inst, Washington, DC 20013 USA. [Condon, Marty] Cornell Coll, Dept Biol, Mt Vernon, IA 52314 USA. RP Norrbom, AL (reprint author), ARS, Systemat Entomol Lab, USDA, Smithsonian Inst, POB 37012,MRC 168, Washington, DC 20013 USA. EM allen.norrbom@ars.usda.gov; MCondon@cornellcollege.edu FU Scientific Cooperation and Research Program; ICD; FAS; USDA; Smithsonian Institution; National Science Foundation [NSF HRD91-03322, NSF DEB 0330845]; Cornell College FX We sincerely thank the many scientists, curators and institutions who kindly loaned or provided specimens for study, particularly Paul Hanson (UCRSJ), Amnon Freidberg (TAUI), Wilford Hanson (USU), and Manuel Zumbado (INBio). J. M. Maes and S. A. Marshall kindly permitted us to deposit the holotypes of B. bivittata and B. marshalli in the USNM. We thank Steve Smith (Smithsonian Institution) for identification of host plants, and Matt Nolte for assistance scoring wing pattern characters. Lucrecia Rodriguez "inked" the terminalia images and enhanced the wing images for publication and prepared the plates. Linda Lawrence produced most of the thorax (dorsal) and abdomen images, J. Marie Metz drew the habitus, head, thorax (lateral), and leg images, and Erica Osmundson drew many of the male terminalia. Gary Steck kindly shared images of the host and larva of B. mexicana. Barbara and Lillian Christie-Pope, Holly Griswold, Mary Harris, Kerry Lewis, Trinity McWilliams, Jon Shik, and Adrienne Valesano assisted in the successful search for infested host material in Costa Rica. We are also grateful to Bob Kula, Wayne Mathis, Norm Woodley, Valery Korneyev and Gary Steck for their thorough reviews of the manuscript. We gratefully acknowledge the following sources of funding, without which this work would not have been possible: Scientific Cooperation and Research Program, ICD, FAS, USDA (ALN project with INBio, Costa Rica), the Smithsonian Institution (postdoctoral fellowship to MC), the National Science Foundation (NSF HRD91-03322, NSF DEB 0330845 to MC), and Cornell College (MC). NR 28 TC 1 Z9 3 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 FEB 26 PY 2010 IS 2374 BP 1 EP 139 PG 139 WC Zoology SC Zoology GA 561SP UT WOS:000274999500001 ER PT J AU Pogue, MG AF Pogue, Michael G. TI The Hadeninae (Lepidoptera: Noctuidae) of Great Smoky Mountains National Park, USA SO ZOOTAXA LA English DT Article DE faunistics; All Taxa Biodiversity Inventory; North Carolina; Tennessee; moths AB Fifty-two species of Hadeninae are recorded from Great Smoky Mountains National Park, Tennessee and North Carolina, USA. Of the six hadenine tribes, five are present in the Park. They include 13 species of Orthosiini, one species of Tholerini, ten species of Hadenini, nine species of Leucaniini, and 19 species of Eriopygini. A total of 160 localities were collected across the Park. The three most diverse localities in the Park were Purchase Knob with 44 species, Big Cove Road with 32 species, and Foothills Parkway with 24 species. The most widespread species in the Park was Pseudorthodes vecors from 59 localities. The most abundant species was Polia detracta with 210 specimens. Images of adults, description/diagnosis, flight period, collected localities, abundance, elevational range, general distribution, and larval hosts are presented for each species. C1 ARS, Systemat Entomol Lab, PSI, USDA,Smithsonian Inst, Washington, DC 20013 USA. RP Pogue, MG (reprint author), ARS, Systemat Entomol Lab, PSI, USDA,Smithsonian Inst, POB 37012,MRC 168, Washington, DC 20013 USA. EM mpogue@sel.barc.usda.gov NR 27 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 FEB 26 PY 2010 IS 2380 BP 1 EP 70 PG 70 WC Zoology SC Zoology GA 561SV UT WOS:000275000100001 ER PT J AU Hultgren, KM Macdonald, KS Duffy, JE AF Hultgren, Kristin M. Macdonald, Kenneth S., III Duffy, J. Emmett TI Sponge-dwelling snapping shrimps of Curacao, with descriptions of three new species SO ZOOTAXA LA English DT Article DE Synalpheus; Zuzalpheus; gambarelloides group; Alpheidae; sponge; symbiotic; coral reef; eusociality ID BELIZE BARRIER-REEF; HOST-SPECIFICITY; CORAL REEFS; SYNALPHEUS; ALPHEIDAE; DECAPODA; EUSOCIALITY; DIVERSITY; COMMUNITY; CRUSTACEA AB Sixteen species of sponge-dwelling snapping shrimp in the genus Synalpheus (gambarelloides group) were collected from sites spanning the south coast of Curacao, including three new to science. Synalpheus hoetjesi sp. nov. belongs to a species complex that includes Synalpheus pandionis, S. dardeaui, S. yano, S. goodei, S. longicarpus, and S. ul. Synalpheus kuadramanus sp. nov. is a distinctive shrimp characterized by a short, square moveable finger on the major first pereopod and by brilliant turquoise embryos in females. Synalpheus orapilosus sp. nov. is a shrimp most morphologically similar to Synalpheus barahonensis-both species share the distinctive character of a tuft of setae on the distal end of the third maxilliped, instead of a distal circlet of spines-but can be distinguished from the latter by the number of carpal segments on the second pereopod. Although eusocial Synalpheus species (defined here as species that live in large colonies with strong reproductive skew) are often the most numerically abundant Synalpheus collected from sponges at other sites, only pair-bonding Synalpheus species were recorded from our collections in Curacao. C1 [Hultgren, Kristin M.] Smithsonian Inst, Natl Museum Nat Hist, MRC 163, Washington, DC 20013 USA. [Macdonald, Kenneth S., III] New Mexico State Univ, Dept Fish Wildlife & Conservat Ecol, Las Cruces, NM 88003 USA. [Duffy, J. Emmett] Coll William & Mary, Sch Marine Sci, Williamsburg, VA 23187 USA. [Duffy, J. Emmett] Coll William & Mary, Virginia Inst Marine Sci, Williamsburg, VA 23187 USA. RP Hultgren, KM (reprint author), Smithsonian Inst, Natl Museum Nat Hist, MRC 163, POB 37012, Washington, DC 20013 USA. EM hultgrenk@si.edu; tripp@nmsu.edu; jeduffy@vims.edu RI Macdonald, Kenneth/F-9822-2011 FU National Geographic Society [8312-07]; Smithsonian Marine Science Network FX This study was made possible by generous funding from the National Geographic Society (Research and Exploration Grant # 8312-07) and from a Smithsonian Marine Science Network postdoctoral funding to KMH. In Curacao, Dr. Paul Hoetjes provided invaluable assistance diving, locating field sites, and in some cases sponge identification. Mark Vermeij and the CARMABI research station provided additional assistance collecting and maintaining sponges. S. Wood provided etymological assistance. This is VIMS publication # 3041. NR 44 TC 10 Z9 12 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 FEB 26 PY 2010 IS 2372 SI SI BP 221 EP 262 PG 42 WC Zoology SC Zoology GA 561SN UT WOS:000274999300020 ER PT J AU Kirchman, JJ Witt, CC McGuire, JA Graves, GR AF Kirchman, Jeremy J. Witt, Christopher C. McGuire, Jimmy A. Graves, Gary R. TI DNA from a 100-year-old holotype confirms the validity of a potentially extinct hummingbird species SO BIOLOGY LETTERS LA English DT Article DE ancient DNA; Andes Mountains; hummingbird; hybrid; extinction ID MAXIMUM-LIKELIHOOD; TROCHILIDAE; REDISCOVERY; SYSTEMATICS; LOST; PERU AB We used mtDNA sequence data to confirm that the controversial 100-year-old holotype of the Bogota sunangel (Heliangelus zusii) represents a valid species. We demonstrate that H. zusii is genetically well differentiated from taxa previously hypothesized to have given rise to the specimen via hybridization. Phylogenetic analyses place H. zusii as sister to a clade of mid-to high-elevation Andean species currently placed in the genera Taphrolesbia and Aglaiocercus. Heliangelus zusii, presumed extinct, has never been observed in nature by biologists. We infer that the species occupied a restricted distribution between the upper tropical and temperate zones of the northern Andes and that it was most probably driven to extinction by deforestation that accompanied human population growth during the nineteenth and early twentieth centuries. We demonstrate the feasibility of obtaining DNA from nearly microscopic tissue samples from old hummingbird specimens and suggest that these methods could be used to resolve the taxonomy of dozens of avian taxa known only from type specimens. C1 [Kirchman, Jeremy J.] New York State Museum & Sci Serv, Albany, NY 12230 USA. [Witt, Christopher C.] Univ New Mexico, Dept Biol, Albuquerque, NM 87131 USA. [Witt, Christopher C.] Univ New Mexico, Museum SW Biol, Albuquerque, NM 87131 USA. [McGuire, Jimmy A.] Univ Calif Berkeley, Museum Vertebrate Zool, Berkeley, CA 94720 USA. [Graves, Gary R.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Kirchman, JJ (reprint author), New York State Museum & Sci Serv, Albany, NY 12230 USA. EM jkirchma@mail.nysed.gov RI Witt, Christopher/D-8587-2012 OI Witt, Christopher/0000-0003-2781-1543 FU NSF [DEB-0543556, DEB-0330750] FX We are grateful to Nate Rice (ANSP) for permission to examine and sample the specimen and to Kelly B. Miller for help with parsimony analyses. We thank the following museums for providing vouchered samples that provided the basis for the original DNA sequences reported in this paper: Academy of Natural Sciences of Philadelphia, Zoological Museum of Copenhagen, Field Museum of Natural History, Louisiana State University Museum of Natural Science and University of New Mexico Museum of Southwestern Biology. Funding for aDNA laboratory work was provided by the New York State Museum. Funding for sequencing of non-ancient hummingbird samples was provided by NSF (DEB-0543556 and DEB-0330750). NR 26 TC 11 Z9 12 U1 0 U2 8 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 1744-9561 J9 BIOL LETTERS JI Biol. Lett. PD FEB 23 PY 2010 VL 6 IS 1 BP 112 EP 115 DI 10.1098/rsbl.2009.0545 PG 4 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 542NR UT WOS:000273501700031 PM 19776061 ER PT J AU McMahon, SM Parker, GG Miller, DR AF McMahon, Sean M. Parker, Geoffrey G. Miller, Dawn R. TI Evidence for a recent increase in forest growth SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE biomass change; carbon cycle; carbon fertilization; climate change; forest stand dynamics ID ABOVEGROUND BIOMASS ACCUMULATION; LONG-TERM; CARBON-CYCLE; TROPICAL FORESTS; CLIMATE-CHANGE; ATMOSPHERIC CO2; PLOT DATA; SEQUESTRATION; ECOSYSTEMS; DYNAMICS AB Forests and their soils contain the majority of the earth's terrestrial carbon stocks. Changes in patterns of tree growth can have a huge impact on atmospheric cycles, biogeochemical cycles, climate change, and biodiversity. Recent studies have shown increases in biomass across many forest types. This increase has been attributed to climate change. However, without knowing the disturbance history of a forest, growth could also be caused by normal recovery from unknown disturbances. Using a unique dataset of tree biomass collected over the past 22 years from 55 temperate forest plots with known land-use histories and stand ages ranging from 5 to 250 years, we found that recent biomass accumulation greatly exceeded the expected growth caused by natural recovery. We have also collected over 100 years of local weather measurements and 17 years of on-site atmospheric CO2 measurements that show consistent increases in line with globally observed climate-change patterns. Combined, these observations show that changes in temperature and CO2 that have been observed worldwide can fundamentally alter the rate of critical natural processes, which is predicted by biogeochemical models. Identifying this rate change is important to research on the current state of carbon stocks and the fluxes that influence how carbon moves between storage and the atmosphere. These results signal a pressing need to better understand the changes in growth rates in forest systems, which influence current and future states of the atmosphere and biosphere. C1 [McMahon, Sean M.; Parker, Geoffrey G.; Miller, Dawn R.] Smithsonian Environm Res Ctr, Forest Ecol Grp, Edgewater, MD 21307 USA. [McMahon, Sean M.] Smithsonian Trop Res Inst, Ctr Trop Forest Sci, APO, AA 34002 USA. RP McMahon, SM (reprint author), Smithsonian Environm Res Ctr, Forest Ecol Grp, Edgewater, MD 21307 USA. EM mcmahons@si.edu OI Parker, Geoffrey/0000-0001-7055-6491 FU HSBC Bank; Smithsonian Tropical Research Institute's Center for Tropical Forest Science FX The authors would like to thank Stuart Davies, Jessica Metcalf, John Parker, Patrick Baker, Nancy Khan, and two anonymous reviewers for helpful comments on the manuscript. We thank Bert Drake for providing the SERC CO2 data. George Rasberry, Donna Tibbs, Michelle Berger, and many volunteers helped to establish and maintain the SERC chronosequence. Funding sources included the HSBC Bank's Climate Partnership and the Smithsonian Tropical Research Institute's Center for Tropical Forest Science. NR 50 TC 131 Z9 134 U1 8 U2 84 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 FEB 23 PY 2010 VL 107 IS 8 BP 3611 EP 3615 DI 10.1073/pnas.0912376107 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 563KN UT WOS:000275130900061 PM 20133710 ER PT J AU Hou, C Kaspari, M Zanden, HBV Gillooly, JF AF Hou, Chen Kaspari, Michael Zanden, Hannah B. Vander Gillooly, James F. TI Energetic basis of colonial living in social insects SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE allometry; colony; scaling; metabolism; metabolic theory of ecology ID ANT HARPEGNATHOS-SALTATOR; METABOLIC-RATE; GENERAL-MODEL; LIFE-SPAN; EVOLUTION; SIZE; TEMPERATURE; RESPIRATION; NETWORKS; GROWTH AB Understanding the ecology and evolution of insect societies requires greater knowledge of how sociality affects the performance of whole colonies. Metabolic scaling theory, based largely on the body mass scaling of metabolic rate, has successfully predicted many aspects of the physiology and life history of individual (or unitary) organisms. Here we show, using a diverse set of social insect species, that this same theory predicts the size dependence of basic features of the physiology (i.e., metabolic rate, reproductive allocation) and life history (i.e., survival, growth, and reproduction) of whole colonies. The similarity in the size dependence of these features in unitary organisms and whole colonies points to commonalities in functional organization. Thus, it raises an important question of how such evolutionary convergence could arise through the process of natural selection. C1 [Hou, Chen; Zanden, Hannah B. Vander; Gillooly, James F.] Univ Florida, Dept Biol, Gainesville, FL 32611 USA. [Hou, Chen] Albert Einstein Coll Med, Dept Syst & Computat Biol, Bronx, NY 10461 USA. [Kaspari, Michael] Univ Oklahoma, Grad Program Ecol & Evolutionary Biol, Norman, OK 73019 USA. [Kaspari, Michael] Univ Oklahoma, Dept Zool, Norman, OK 73019 USA. [Kaspari, Michael] Smithsonian Trop Res Inst, Balboa 084303092, Panama. RP Gillooly, JF (reprint author), Univ Florida, Dept Biol, Gainesville, FL 32611 USA. EM gillooly@ufl.edu OI Hou, Chen/0000-0002-3665-225X; Vander Zanden, Hannah/0000-0003-3366-5116; Kaspari, Michael/0000-0002-9717-5768 NR 43 TC 43 Z9 43 U1 5 U2 36 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 FEB 23 PY 2010 VL 107 IS 8 BP 3634 EP 3638 DI 10.1073/pnas.0908071107 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 563KN UT WOS:000275130900065 PM 20133582 ER PT J AU Sale, SE Drew, JE Knigge, C Zijlstra, AA Irwin, MJ Morris, RAH Phillipps, S Drake, JJ Greimel, R Unruh, YC Groot, PJ Mampaso, A Walton, NA AF Sale, S. E. Drew, J. E. Knigge, C. Zijlstra, A. A. Irwin, M. J. Morris, R. A. H. Phillipps, S. Drake, J. J. Greimel, R. Unruh, Y. C. Groot, P. J. Mampaso, A. Walton, N. A. TI The structure of the outer Galactic disc as revealed by IPHAS early A stars SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE surveys; Galaxy: abundances; Galaxy: disc; Galaxy: stellar content; Galaxy: structure ID OLD OPEN CLUSTERS; ON SPIRAL GALAXIES; H-ALPHA SURVEY; MILKY-WAY; CHEMICAL EVOLUTION; METALLICITY GRADIENT; ABUNDANCE GRADIENT; SOLAR NEIGHBORHOOD; SURFACE-BRIGHTNESS; YOUNG STARS AB This study is an investigation of the stellar density profile of the Galactic disc in the anticentre direction. We select over 40 000 early A stars from INT/WFC Photometric Ha Survey of the Northern Galactic Plane (IPHAS) photometry in the Galactic longitude range 160 degrees < l < 200 degrees close to the equatorial plane (-1 degrees < b < +1 degrees). We then compare their observed reddening-corrected apparent magnitude distribution with simulated photometry obtained from parametrized models in order to set constraints on the anticentre stellar density profile. By selecting A stars, we are appraising the properties of a population only similar to 100 Myr old. We find that the stellar density profile of young stars is well fit to an exponential with length-scale of (3020 +/- 120(statistical) +/- 180(systematic)) pc, which is comparable to that obtained in earlier studies, out to a Galactocentric radius of R(T) = (13.0 +/- 0.5(statistical) +/- 0.6(systematic)) kpc. At larger radii, the rate of decline appears to increase with the scalelength dropping to (1200 +/- 300(statistical) +/- 70(systematic)) pc. This result amounts to a refinement of the conclusions reached in previous studies that the stellar density profile is abruptly truncated. The IPHAS A star data are not compatible with models that propose a sudden change in metallicity at R(G) = 10 kpc. C1 [Sale, S. E.; Unruh, Y. C.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England. [Drew, J. E.] Univ Hertfordshire, STRI, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Knigge, C.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Zijlstra, A. A.] Univ Manchester, Jodrell Bank, Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Irwin, M. J.; Walton, N. A.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Morris, R. A. H.; Phillipps, S.] Univ Bristol, Dept Phys, Astrophys Grp, Bristol BS8 1TL, Avon, England. [Drake, J. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Greimel, R.] Karl Franzens Univ Graz, Inst Phys, A-8010 Graz, Austria. [Groot, P. J.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands. [Mampaso, A.] Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Santa Cruz Tene, Spain. RP Sale, SE (reprint author), Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, Prince Consort Rd, London SW7 2AZ, England. EM s.sale06@imperial.ac.uk RI Sale, Stuart/E-1815-2010; Groot, Paul/K-4391-2016; OI Drew, Janet/0000-0003-1192-7082; Groot, Paul/0000-0002-4488-726X; Unruh, Yvonne/0000-0001-8217-6998; Sale, Stuart/0000-0003-2155-0995; Morris, Rhys/0000-0002-9210-1567; Phillipps, Steven/0000-0001-5991-3486 FU Science & Technology Facilities Council of the United Kingdom FX This paper makes use of data obtained as part of the INT Photometric Ha Survey of the Northern Galactic Plane (IPHAS) carried out on the INT. The INT is operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. All IPHAS data are processed by the Cambridge Astronomical Survey Unit, at the Institute of Astronomy in Cambridge. SES is in recipient of a studentship funded by the Science & Technology Facilities Council of the United Kingdom. NR 91 TC 18 Z9 18 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 FEB 21 PY 2010 VL 402 IS 2 BP 713 EP 723 DI 10.1111/j.1365-2966.2009.15746.x PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 551WH UT WOS:000274242900002 ER PT J AU Hopkins, PF Hernquist, L AF Hopkins, Philip F. Hernquist, Lars TI A new empirical method to infer the starburst history of the Universe from local galaxy properties SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Review DE stars: formation; stars: general; galaxies: active; galaxies: evolution; galaxies: formation; cosmology: theory ID HUBBLE-SPACE-TELESCOPE; ULTRALUMINOUS INFRARED GALAXIES; STAR-FORMING GALAXIES; ACTIVE GALACTIC NUCLEI; HIGH-REDSHIFT GALAXIES; BRIGHTEST CLUSTER GALAXIES; SUPERMASSIVE BLACK-HOLES; CCD SURFACE PHOTOMETRY; DUST-OBSCURED GALAXIES; SPITZER MIDINFRARED SPECTROSCOPY AB The centres of ellipticals and bulges are formed dissipationally, via gas inflows over short time-scales-the 'starburst' mode of star formation. Recent work has shown that the surface brightness profiles, kinematics and stellar populations of spheroids can be used to separate the dissipational component from the dissipationless 'envelope' made up of stars formed over more extended histories in separate objects, and violently assembled in mergers. Given high-resolution, detailed observations of these 'burst relic' components of ellipticals (specifically their stellar mass surface density profiles), together with the simple assumptions that some form of the Kennicutt-Schmidt law holds and that the burst was indeed a dissipational, gas-rich event, we show that it is possible to invert the observed profiles and obtain the time- and space-dependent star formation history of each burst. We perform this exercise using a large sample of well-studied spheroids, which have also been used to calibrate estimates of the 'burst relic' populations. We show that the implied bursts scale in magnitude, mass and peak star formation rate (SFR) with galaxy mass in a simple manner, and provide fits for these correlations. The typical burst mass M(burst) is similar to 10 per cent of the total spheroid mass, the characteristic starburst time-scale implied is a nearly galaxy-mass-independent t(burst) similar to 10(8) yr, the peak SFR of the burst is similar to M(burst)/t(burst) and bursts decay subsequently in power-law fashion as (M) over dot(*) alpha t(-2.4). As a function of time, we obtain the spatial size of the starburst; burst sizes at peak activity scale with burst mass in a manner similar to the observed spheroid size-mass relation, but are smaller than the full galaxy size by a factor of similar to 10; the size grows in time as the central, most dense regions are more quickly depleted by star formation as R(burst) alpha t(0.5). Combined with observational measurements of the nuclear stellar population ages of these systems-i.e. the distribution of times when these bursts occurred-it is possible to re-construct the dissipational burst contribution to the distribution of SFRs and infrared (IR) luminosity functions (LFs) and luminosity density of the Universe. We do so and show that these burst LFs agree well with the observed IR LFs at the brightest luminosities, at redshifts z similar to 0-2. At low luminosities, however, bursts are always unimportant; the transition luminosity between these regimes increases with redshift from the ultraluminous infrared galaxy threshold at z similar to 0 to hyper-luminous infrared galaxy thresholds at z similar to 2. At the highest redshifts z greater than or similar to 2, we can set strict upper limits on starburst magnitudes, based on the maximum stellar mass remaining at high densities at z = 0, and find tension between these and estimated number counts of sub-millimetre galaxies, implying that some change in bolometric corrections, the number counts themselves or the stellar initial mass function may be necessary. At all redshifts, bursts are a small fraction of the total SFR or luminosity density, similar to 5-10 per cent, in good agreement with estimates of the contribution of merger-induced star formation. C1 [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. [Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Hopkins, PF (reprint author), Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. EM phopkins@astro.berkeley.edu FU Miller Institute for Basic Research in Science, University of California Berkeley FX We thank Chris Hayward and Josh Younger for helpful discussions throughout the development of this paper. Support for PFH was provided by the Miller Institute for Basic Research in Science, University of California Berkeley. NR 192 TC 29 Z9 29 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 FEB 21 PY 2010 VL 402 IS 2 BP 985 EP 1004 DI 10.1111/j.1365-2966.2009.15933.x PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 551WH UT WOS:000274242900022 ER PT J AU Park, S Hughes, JP Slane, PO Mori, K Burrows, DN AF Park, Sangwook Hughes, John P. Slane, Patrick O. Mori, Koji Burrows, David N. TI A DEEP CHANDRA OBSERVATION OF THE OXYGEN-RICH SUPERNOVA REMNANT 0540-69.3 IN THE LARGE MAGELLANIC CLOUD SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: abundances; ISM: individual objects (SNR 0540-69.3); ISM: supernova remnants; X-rays: ISM ID CCD IMAGING SPECTROMETER; PSR B0540-69; X-RAYS; SNR B0540-69.3; H I; PULSAR; SHELL; YOUNG; EMISSION; NEBULA AB Using our deep similar to 120 ks Chandra observation, we report on the results from our spatially resolved X-ray spectral analysis of the "oxygen-rich" supernova remnant (SNR) 0540-69.3 in the Large Magellanic Cloud. We conclusively establish the nonthermal nature of the "arcs" in the east and west boundaries of the SNR, which confirms the cosmic-ray electron acceleration in the supernova shock (B similar to 20-140 mu G). We report tentative evidence for Fe overabundance in the southern region close to the outer boundary of the SNR. While such a detection would be intriguing, the existence of Fe ejecta is not conclusive with the current data because of poor photon statistics and limited plasma models. If it is verified using deeper X-ray observations and improved plasma models, the presence of Fe ejecta, which was produced in the core of the supernova, near the SNR's outer boundary would provide an intriguing opportunity to study the explosive nucleosynthesis and the ejecta mixing in this young core-collapse SNR. There is no evidence of X-ray counterparts for the optical O-rich ejecta in the central regions of the SNR. C1 [Park, Sangwook; Burrows, David N.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Hughes, John P.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Slane, Patrick O.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Mori, Koji] Miyazaki Univ, Dept Appl Phys, Miyazaki 8892192, Japan. RP Park, S (reprint author), Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. EM park@astro.psu.edu FU Smithsonian Astrophysical Observatory [GO5-6063X] FX The authors thank the referee for the careful review that helped improve this work. We also thank K. Borkowski for providing us the updated atomic database and for the extensive discussion on the Fe L line fits in the low-ionization plasma. S. P. also thanks S. Zhekov for the helpful discussion on the Fe L lines. S. P. and K. M. thank F. Bocchino for a useful discussion. This work was supported in part by the Smithsonian Astrophysical Observatory under Chandra grant GO5-6063X. NR 39 TC 16 Z9 16 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 FEB 20 PY 2010 VL 710 IS 2 BP 948 EP 957 DI 10.1088/0004-637X/710/2/948 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 551TN UT WOS:000274233300006 ER PT J AU Piconcelli, E Vignali, C Bianchi, S Nicastro, F Miniutti, G Fiore, F AF Piconcelli, Enrico Vignali, Cristian Bianchi, Stefano Nicastro, Fabrizio Miniutti, Giovanni Fiore, Fabrizio TI INVESTIGATING THE COMPLEX X-RAY SPECTRUM OF A BROAD-LINE 2MASS RED QUASAR: XMM-NEWTON OBSERVATION OF FTM 0830+3759 SO ASTROPHYSICAL JOURNAL LA English DT Review DE galaxies: active; galaxies: nuclei; infrared: galaxies; X-rays: individual (FTM 0830+3759) ID ACTIVE GALACTIC NUCLEI; ALL-SKY SURVEY; DUST-REDDENED QUASARS; SEYFERT-1 GALAXY MRK-335; RADIO-QUIET QUASARS; K-ALPHA-LINES; HOST GALAXIES; STELLAR OBJECTS; ABSORPTION-LINE; SPACE-TELESCOPE AB We report results from a 50 ks XMM-Newton observation of the dust-reddened broad-line quasar FTM 0830+3759 (z = 0.413) selected from the Faint Images of the Radio Sky at Twenty cm/Two Micron All Sky Survey red quasar survey. For this active galactic nucleus (AGN), a very short 9 ks Chandra exposure had suggested a feature-rich X-ray spectrum and Hubble Space Telescope images revealed a very disturbed host galaxy morphology. Contrary to classical, optically selected quasars, the X-ray properties of red (i.e., with J - K-s > 1.7 and R - K-s > 4.0) broad-line quasars are still quite unexplored, although there is a growing consensus that, due to moderate obscuration, these objects can offer a unique view of spectral components typically swamped by the AGN light in normal, blue quasars. The XMM-Newton observation discussed here has definitely confirmed the complexity of the X-ray spectrum revealing the presence of a cold (or mildly ionized) absorber with N-H approximate to 10(22) cm(-2) along the line of sight to the nucleus and a Compton reflection component accompanied by an intense Fe K alpha emission line in this quasar with a L2-10keV approximate to 5 x 10(44) erg s(-1). A soft-excess component is also required by the data. The match between the column density derived by our spectral analysis and that expected on the basis of reddening due to the dust suggests the possibility that both absorptions occur in the same medium. FTM 0830+3759 is characterized by an extinction/absorption-corrected X-ray-to-optical flux ratio alpha(ox) = -2.3, which is steeper than expected on the basis of its UV luminosity. These findings indicate that the X-ray properties of FTM 0830+3759 differ from those typically observed for optically selected broad-line quasars with comparable hard X-ray luminosity. C1 [Piconcelli, Enrico; Nicastro, Fabrizio; Fiore, Fabrizio] Osservatorio Astron Roma INAF, I-00040 Monte Porzio Catone, Italy. [Vignali, Cristian] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. [Bianchi, Stefano] Univ Roma Tre, Dipartimento Fis, I-00146 Rome, Italy. [Nicastro, Fabrizio] Fdn Res & Technol, IESL, Iraklion 71110, Crete, Greece. [Nicastro, Fabrizio] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02155 USA. [Fiore, Fabrizio] Ctr Astrobiol CSIC INTA LAEFF, LAEX, E-28691 Madrid, Spain. RP Piconcelli, E (reprint author), Osservatorio Astron Roma INAF, Via Frascati 33, I-00040 Monte Porzio Catone, Italy. EM piconcelli@oa-roma.inaf.it RI Bianchi, Stefano/B-4804-2010; Vignali, Cristian/J-4974-2012; Miniutti, Giovanni/L-2721-2014; OI Bianchi, Stefano/0000-0002-4622-4240; Vignali, Cristian/0000-0002-8853-9611; Miniutti, Giovanni/0000-0003-0707-4531; Fiore, Fabrizio/0000-0002-4031-4157; piconcelli, enrico/0000-0001-9095-2782; Nicastro, Fabrizio/0000-0002-6896-1364 FU ASI/INAF [I/088/06/0]; XMM-Newton [NNX08AY05G]; Ministerio de Ciencia e Innovacion; CSIC; National Aeronautics and Space Administration FX We thank the anonymous referee for valuable feedback. E. P. is grateful to R. Maiolino, M. Giustini, L. Ballo, and M. Mignoli for helpful discussions and suggestions. E. P., C. V., and S. B. acknowledge support under ASI/INAF contract I/088/06/0. F. N. acknowledges the XMM-Newton grant NNX08AY05G. G. M. thanks the Ministerio de Ciencia e Innovacion and CSIC for support through a Ramon y Cajal contract. This research has made use of the SIMBAD database, operated at CDS (Strasbourg, France), and the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. Based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. NR 118 TC 4 Z9 4 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2010 VL 710 IS 2 BP 992 EP 1002 DI 10.1088/0004-637X/710/2/992 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 551TN UT WOS:000274233300010 ER PT J AU Cantrell, AG Bailyn, CD Orosz, JA McClintock, JE Remillard, RA Froning, CS Neilsen, J Gelino, DM Gou, LJ AF Cantrell, Andrew G. Bailyn, Charles D. Orosz, Jerome A. McClintock, Jeffrey E. Remillard, Ronald A. Froning, Cynthia S. Neilsen, Joseph Gelino, Dawn M. Gou, Lijun TI THE INCLINATION OF THE SOFT X-RAY TRANSIENT A0620-00 AND THE MASS OF ITS BLACK HOLE SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; stars: individual (A0620-00); X-rays: binaries ID BINARY A0620-00; MODEL ATMOSPHERES; SECONDARY STAR; ACCRETION DISC; LIGHT-CURVE; CONSTRAINTS AB We analyze photometry of the soft X-ray transient A0620-00 spanning nearly 30 years, including previously published and previously unpublished data. Previous attempts to determine the inclination of A0620 using subsets of these data have yielded a wide range of measured values of i. Differences in the measured value of i have been due to changes in the shape of the light curve and uncertainty regarding the contamination from the disk. We give a new technique for estimating the disk fraction and find that disk light is significant in all light curves, even in the infrared. We also find that all changes in the shape and normalization of the light curve originate in a variable disk component. After accounting for this disk component, we find that all the data, including light curves of significantly different shapes, point to a consistent value of i. Combining results from many separate data sets, we find i = 51 degrees.0 +/- 0 degrees.9, implying M = 6.6 +/- 0.25 M(circle dot). Using our dynamical model and zero-disk stellar VIH magnitudes, we find d = 1.06 +/- 0.12 kpc. Understanding the disk origin of nonellipsoidal variability may assist with making reliable determinations of i in other systems, and the fluctuations in disk light may provide a new observational tool for understanding the three-dimensional structure of the accretion disk. C1 [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. [McClintock, Jeffrey E.; Gou, Lijun] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Remillard, Ronald A.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Froning, Cynthia S.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Neilsen, Joseph] Harvard Univ, Dept Astron, Cambridge, MA 02138 USA. [Gelino, Dawn M.] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA. RP Cantrell, AG (reprint author), Yale Univ, Dept Astron, POB 208101, New Haven, CT 06520 USA. EM andrew.cantrell@yale.edu; charles.bailyn@yale.edu; orosz@sciences.sdsu.edu; jmcclintock@cfa.harvard.edu; rr@space.mit.edu; Cynthia.Froning@Colorado.EDU; jneilsen@cfa.harvard.edu; dawn@ipac.caltech.edu; lgou@cfa.harvard.edu OI Neilsen, Joseph/0000-0002-8247-786X NR 33 TC 62 Z9 62 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 FEB 20 PY 2010 VL 710 IS 2 BP 1127 EP 1141 DI 10.1088/0004-637X/710/2/1127 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 551TN UT WOS:000274233300018 ER PT J AU Liu, Y Elvis, M McHardy, IM Grupe, D Wilkes, BJ Reeves, J Brickhouse, N Krongold, Y Mathur, S Minezaki, T Nicastro, F Yoshii, Y Zhang, SN AF Liu, Yuan Elvis, Martin McHardy, Ian M. Grupe, Dirk Wilkes, Belinda J. Reeves, James Brickhouse, Nancy Krongold, Yair Mathur, Smita Minezaki, Takeo Nicastro, Fabrizio Yoshii, Yuzuru Zhang, Shuang Nan TI SUZAKU MONITORING OF THE IRON K EMISSION LINE IN THE TYPE 1 ACTIVE GALACTIC NUCLEUS NGC 5548 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: individual (NGC 5548); galaxies: Seyfert; quasars: emission lines; X-rays: galaxies ID SEYFERT-1 GALAXY NGC-5548; RAY SPECTRAL VARIABILITY; ALPHA-EMISSION; XMM-NEWTON; COLUMN DENSITIES; BOARD SUZAKU; FEK-ALPHA; REGION; SPECTROSCOPY; QUASARS AB We present seven sequential weekly observations of NGC 5548 conducted in 2007 with the Suzaku X-ray Imaging Spectrometer (XIS) in the 0.2-12 keV band and Hard X-ray Detector (HXD) in the 10-600 keV band. The iron K alpha line is well detected in all seven observations and K beta line is also detected in four observations. In this paper, we investigate the origin of the Fe K lines using both the width of the line and the reverberation mapping method. With the co-added XIS and HXD spectra, we identify Fe K alpha and K beta line at 6.396(-0.007)(+0.009) keV and 7.08(-0.05)(+0.05) keV, respectively. The width of line obtained from the co-added spectra is 38(-18)(+16) eV (FWHM = 4200(-2000)(+1800) km s(-1)) which corresponds to a radius of 20(-10)(+50) light days, for the virial production of 1.220 x 10(7) M(circle dot) in NGC 5548. To quantitatively investigate the origin of the narrow Fe line by the reverberation mapping method, we compare the observed light curves of Fe K alpha line with the predicted ones, which are obtained by convolving the continuum light curve with the transfer functions in a thin shell and an inclined disk. The best-fit result is given by the disk case with i = 30 degrees which is better than a fit to a constant flux of the Fe K line at the 92.7% level (F-test). However, the results with other geometries are also acceptable (P > 50%). We find that the emitting radius obtained from the light curve is 25-37 light days, which is consistent with the radius derived from the Fe K line width. Combining the results of the line width and variation, the most likely site for the origin of the narrow iron lines is 20-40 light days away from the central engine, though other possibilities are not completely ruled out. This radius is larger than the H beta emitting parts of the broad-line region at 6-10 light days (obtained by the simultaneous optical observation), and smaller than the inner radius of the hot dust in NGC 5548 (at about 50 light days). C1 [Liu, Yuan; Elvis, Martin; Wilkes, Belinda J.; Brickhouse, Nancy; Nicastro, Fabrizio] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Liu, Yuan; Zhang, Shuang Nan] Tsinghua Univ, Dept Phys, Beijing 100084, Peoples R China. [Liu, Yuan; Zhang, Shuang Nan] Tsinghua Univ, Ctr Astrophys, Beijing 100084, Peoples R China. [McHardy, Ian M.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Grupe, Dirk] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Reeves, James] Univ Keele, Sch Phys & Geog Sci, Astrophys Grp, Keele ST5 5BG, Staffs, England. [Krongold, Yair] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. [Mathur, Smita] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Minezaki, Takeo; Yoshii, Yuzuru] Univ Tokyo, Sch Sci, Inst Astron, Tokyo 1810015, Japan. [Zhang, Shuang Nan] Chinese Acad Sci, Inst High Energy Phys, Key Lab Particle Astrophys, Beijing 100049, Peoples R China. [Zhang, Shuang Nan] Univ Alabama, Dept Phys, Huntsville, AL 35899 USA. RP Liu, Y (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM yliu@cfa.harvard.edu; elvis@cfa.harvard.edu RI XRAY, SUZAKU/A-1808-2009; OI Brickhouse, Nancy/0000-0002-8704-4473; Nicastro, Fabrizio/0000-0002-6896-1364; Wilkes, Belinda/0000-0003-1809-2364 FU Ministry of Education at Tsinghua University; Chinese Academy of Sciences [KJCX2-YW-T03]; National Natural Science Foundation of China [10821061, 10733010, 10725313]; 973 Program of China [2009CB824800]; CXC [GO7-8136A]; Suzaku [NNX08AB81G] FX Y. L. thanks Junfeng Wang and Joanna Kuraszkiewicz for the helpful discussions. S. N. Z. acknowledges partial funding support by the Yangtze Endowment from the Ministry of Education at Tsinghua University, Directional Research Project of the Chinese Academy of Sciences under project No. KJCX2-YW-T03 and by the National Natural Science Foundation of China under grant Nos. 10821061, 10733010, 10725313, and by 973 Program of China under grant 2009CB824800. This work has been funded by CXC grant GO7-8136A and Suzaku Grant NNX08AB81G. NR 54 TC 18 Z9 18 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 FEB 20 PY 2010 VL 710 IS 2 BP 1228 EP 1238 DI 10.1088/0004-637X/710/2/1228 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 551TN UT WOS:000274233300024 ER PT J AU Sadavoy, SI Di Francesco, J Bontemps, S Megeath, ST Rebull, LM Allgaier, E Carey, S Gutermuth, R Hora, J Huard, T McCabe, CE Muzerolle, J Noriega-Crespo, A Padgett, D Terebey, S AF Sadavoy, Sarah I. Di Francesco, James Bontemps, Sylvain Megeath, S. Thomas Rebull, Luisa M. Allgaier, Erin Carey, Sean Gutermuth, Robert Hora, Joe Huard, Tracy McCabe, Caer-Eve Muzerolle, James Noriega-Crespo, Alberto Padgett, Deborah Terebey, Susan TI THE MASS DISTRIBUTION OF STARLESS AND PROTOSTELLAR CORES IN GOULD BELT CLOUDS SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; ISM: clouds; stars: formation; stars: luminosity function, mass function; stars: protostars ID SPITZER C2D SURVEY; YOUNG STELLAR OBJECTS; PERSEUS MOLECULAR CLOUD; ARRAY CAMERA IRAC; INTERSTELLAR CLOUDS; DENSE CORES; UNBIASED SUBMILLIMETER; MIDINFRARED SURVEYS; INITIAL CONDITIONS; SPACE-TELESCOPE AB Using data from the SCUBA Legacy Catalogue (850 mu m) and Spitzer Space Telescope (3.6-70 mu m), we explore dense cores in the Ophiuchus, Taurus, Perseus, Serpens, and Orion molecular clouds. We develop a new method to discriminate submillimeter cores found by Submillimeter Common-User Bolometer Array (SCUBA) as starless or protostellar, using point source photometry from Spitzer wide field surveys. First, we identify infrared sources with red colors associated with embedded young stellar objects (YSOs). Second, we compare the positions of these YSO candidates to our submillimeter cores. With these identifications, we construct new, self-consistent starless and protostellar core mass functions (CMFs) for the five clouds. We find best-fit slopes to the high-mass end of the CMFs of -1.26 +/- 0.20, -1.22 +/- 0.06, -0.95 +/- 0.20, and -1.67 +/- 0.72 for Ophiuchus, Taurus, Perseus, and Orion, respectively. Broadly, these slopes are each consistent with the -1.35 power-law slope of the Salpeter initial mass function at higher masses, but suggest some differences. We examine a variety of trends between these CMF shapes and their parent cloud properties, potentially finding a correlation between the high-mass slope and core temperature. We also find a trend between core mass and effective size, but we are very limited by sensitivity. We make similar comparisons between core mass and size with visual extinction (for A(V) >= 3) and find no obvious trends. We also predict the numbers and mass distributions of cores that future surveys with SCUBA-2 may detect in each of these clouds. C1 [Sadavoy, Sarah I.; Di Francesco, James] Univ Victoria, Dept Phys & Astron, STN CSC, Victoria, BC V8W 3P6, Canada. [Sadavoy, Sarah I.; Di Francesco, James] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Bontemps, Sylvain] Observ Bordeaux, F-33270 Floirac, France. [Megeath, S. Thomas; Allgaier, Erin] Univ Toledo, Ritter Observ, Toledo, OH 43606 USA. [Rebull, Luisa M.; Carey, Sean; McCabe, Caer-Eve; Noriega-Crespo, Alberto; Padgett, Deborah] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Gutermuth, Robert] Univ Massachusetts, Smith Coll, Northampton, MA 01063 USA. [Hora, Joe] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Huard, Tracy] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Muzerolle, James] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Terebey, Susan] Calif State Univ Los Angeles, Dept Phys & Astron, Los Angeles, CA 90032 USA. RP Sadavoy, SI (reprint author), Univ Victoria, Dept Phys & Astron, STN CSC, POB 355, Victoria, BC V8W 3P6, Canada. EM ssadavoy@uvic.ca OI Rebull, Luisa/0000-0001-6381-515X; Hora, Joseph/0000-0002-5599-4650 NR 71 TC 62 Z9 63 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 FEB 20 PY 2010 VL 710 IS 2 BP 1247 EP 1270 DI 10.1088/0004-637X/710/2/1247 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 551TN UT WOS:000274233300026 ER PT J AU Kratter, KM Murray-Clay, RA Youdin, AN AF Kratter, Kaitlin M. Murray-Clay, Ruth A. Youdin, Andrew N. TI THE RUNTS OF THE LITTER: WHY PLANETS FORMED THROUGH GRAVITATIONAL INSTABILITY CAN ONLY BE FAILED BINARY STARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: general; brown dwarfs; planet-disk interactions; planets and satellites: formation; protoplanetary disks ID PASSIVE CIRCUMSTELLAR DISKS; BROWN DWARF DESERT; T-TAURI STARS; PROTOPLANETARY DISK; ACCRETION DISKS; PROTOSTELLAR DISCS; GIANT PLANETS; HR 8799; MAGNETOROTATIONAL INSTABILITY; ORBITAL MIGRATION AB Recent direct imaging discoveries suggest a new class of massive, distant planets around A stars. These widely separated giants have been interpreted as signs of planet formation driven by gravitational instability, but the viability of this mechanism is not clear-cut. In this paper, we first discuss the local requirements for fragmentation and the initial fragment mass scales. We then consider whether the fragment's subsequent growth can be terminated within the planetary mass regime. Finally, we place disks in the larger context of star formation and disk evolution models. We find that in order for gravitational instability to produce planets, disksmust be atypically cold in order to reduce the initial fragment mass. In addition, fragmentation must occur during a narrow window of disk evolution, after infall has mostly ceased, but while the disk is still sufficiently massive to undergo gravitational instability. Under more typical conditions, disk-born objects will likely grow well above the deuterium burning planetary mass limit. We conclude that if planets are formed by gravitational instability, they must be the low-mass tail of the distribution of disk-born companions. To validate this theory, ongoing direct imaging surveys must find a greater abundance of brown dwarf and M-star companions to A stars. Their absence would suggest planet formation by a different mechanism such as core accretion, which is consistent with the debris disks detected in these systems. C1 [Kratter, Kaitlin M.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Murray-Clay, Ruth A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Youdin, Andrew N.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. RP Kratter, KM (reprint author), Univ Toronto, Dept Astron & Astrophys, 50 St George St, Toronto, ON M5S 3H4, Canada. RI Youdin, Andrew/C-1596-2013 OI Youdin, Andrew/0000-0002-3644-8726 NR 85 TC 133 Z9 133 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 FEB 20 PY 2010 VL 710 IS 2 BP 1375 EP 1386 DI 10.1088/0004-637X/710/2/1375 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 551TN UT WOS:000274233300035 ER PT J AU Fabrycky, DC Murray-Clay, RA AF Fabrycky, Daniel C. Murray-Clay, Ruth A. TI STABILITY OF THE DIRECTLY IMAGED MULTIPLANET SYSTEM HR 8799: RESONANCE AND MASSES SO ASTROPHYSICAL JOURNAL LA English DT Article DE celestial mechanics; methods: numerical; planetary systems ID MULTI-PLANET SYSTEMS; EXTRA-SOLAR PLANETS; DEBRIS DISK; 3-BODY PROBLEM; GIANT PLANETS; DYNAMICS; EVOLUTION; GJ-876; MOTION; STARS AB A new era of directly imaged extrasolar planets has produced a three-planet system, where the masses of the planets have been estimated by untested cooling models. We point out that the nominal circular, face-on orbits of the planets lead to a dynamical instability in similar to 10(5) yr, a factor of at least 100 shorter than the estimated age of the star. Reduced planetary masses produce stability only for unreasonably small planets (less than or similar to 2 M(Jup)). Relaxing the face-on assumption, but still requiring circular orbits while fitting the observed positions, makes the instability time even shorter. A promising solution is that the inner two planets have a 2: 1 commensurability between their periods, and they avoid close encounters with each other through this resonance. The fact that the inner resonance has lasted until now, in spite of the perturbations of the outer planet, leads to a limit less than or similar to 10 M(Jup) on the masses unless the outer two planets are also engaged in a 2: 1 mean-motion resonance. In a double resonance, which is consistent with the current data, the system could survive until now even if the planets have masses of similar to 20 M(Jup). Apsidal alignment can further enhance the stability of a mean-motion resonant system. A completely different dynamical configuration, with large eccentricities and large mutual inclinations among the planets, is possible but finely tuned. C1 [Fabrycky, Daniel C.; Murray-Clay, Ruth A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Fabrycky, DC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 51, Cambridge, MA 02138 USA. EM daniel.fabrycky@gmail.com OI Fabrycky, Daniel/0000-0003-3750-0183 FU Michelson Fellowship; National Aeronautics and Space Administration; Michelson Science Center; Institute for Theory and Computation Fellowship at Harvard University FX We thank Matthew Holman, Eric Ford, Jack Lissauer, Guillermo Torres, Sean Andrews, YanqinWu, AndrewShannon, and members of CITA and University of Toronto Astrophysics department for helpful discussions. We thank Scott Tremaine, Eugene Chiang, and the anonymous referee for suggesting that we expand the investigation to mutually inclined solutions. D. F. is grateful for funding through a Michelson Fellowship, which is supported by the National Aeronautics and Space Administration and administered by the Michelson Science Center. R. M. is grateful for an Institute for Theory and Computation Fellowship at Harvard University. NR 52 TC 76 Z9 76 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 FEB 20 PY 2010 VL 710 IS 2 BP 1408 EP 1421 DI 10.1088/0004-637X/710/2/1408 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 551TN UT WOS:000274233300038 ER PT J AU O'Donovan, FT Charbonneau, D Harrington, J Madhusudhan, N Seager, S Deming, D Knutson, HA AF O'Donovan, Francis T. Charbonneau, David Harrington, Joseph Madhusudhan, N. Seager, Sara Deming, Drake Knutson, Heather A. TI DETECTION OF PLANETARY EMISSION FROM THE EXOPLANET TrES-2 USING SPITZER/IRAC SO ASTROPHYSICAL JOURNAL LA English DT Article DE eclipses; infrared: stars; planetary systems; stars: individual (GSC 03549-02811); techniques: photometric ID EXTRASOLAR GIANT PLANETS; INFRARED ARRAY CAMERA; HD 189733B; HOT JUPITERS; THERMAL EMISSION; SPACE-TELESCOPE; LIGHT CURVES; TEMPERATURE INVERSION; TRANSITING PLANETS; DAYSIDE SPECTRUM AB We present here the results of our observations of TrES-2 using the Infrared Array Camera on Spitzer. We monitored this transiting system during two secondary eclipses, when the planetary emission is blocked by the star. The resulting decrease in flux is 0.127% +/- 0.021%, 0.230% +/- 0.024%, 0.199% +/- 0.054%, and 0.359% +/- 0.060% at 3.6 mu m, 4.5 mu m, 5.8 mu m, and 8.0 mu m, respectively. We show that three of these flux contrasts are well fit by a blackbody spectrum with T(eff) = 1500 K, as well as by a more detailed model spectrum of a planetary atmosphere. The observed planet-to-star flux ratios in all four IRAC channels can be explained by models with and without a thermal inversion in the atmosphere of TrES-2, although with different atmospheric chemistry. Based on the assumption of thermochemical equilibrium, the chemical composition of the inversion model seems more plausible, making it a more favorable scenario. TrES-2 also falls in the category of highly irradiated planets which have been theoretically predicted to exhibit thermal inversions. However, more observations at infrared and visible wavelengths would be needed to confirm a thermal inversion in this system. Furthermore, we find that the times of the secondary eclipses are consistent with previously published times of transit and the expectation from a circular orbit. This implies that TrES-2 most likely has a circular orbit, and thus does not obtain additional thermal energy from tidal dissipation of a non-zero orbital eccentricity, a proposed explanation for the large radius of this planet. C1 [O'Donovan, Francis T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [O'Donovan, Francis T.] CALTECH, Pasadena, CA 91125 USA. [Charbonneau, David; Knutson, Heather A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Harrington, Joseph] Univ Cent Florida, Dept Phys, Orlando, FL 32816 USA. [Madhusudhan, N.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Seager, Sara] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. [Deming, Drake] NASA, Goddard Space Flight Ctr, Planetary Syst Lab, Greenbelt, MD 20771 USA. RP O'Donovan, FT (reprint author), NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM ftod@caltech.edu RI Harrington, Joseph/E-6250-2011; O'Donovan, Francis/I-2423-2014; OI O'Donovan, Francis/0000-0002-4858-6106; Charbonneau, David/0000-0002-9003-484X; Harrington, Joseph/0000-0002-8955-8531 FU Jet Propulsion Laboratory, California Institute of Technology; NASANASA Postdoctoral Program at the Goddard Space Flight Center [NNG05GJ29G] 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 the National Aeronautics and Space Administration (NASA). This research was supported in part by NASA under grant NNG05GJ29G (issued through the Origins of Solar Systems Program) and also by an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center (administered by Oak Ridge Associated Universities through a contract with NASA). NR 55 TC 37 Z9 37 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 FEB 20 PY 2010 VL 710 IS 2 BP 1551 EP 1556 DI 10.1088/0004-637X/710/2/1551 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 551TN UT WOS:000274233300049 ER PT J AU Green, PJ Myers, AD Barkhouse, WA Mulchaey, JS Bennert, VN Cox, TJ Aldcroft, TL AF Green, Paul J. Myers, Adam D. Barkhouse, Wayne A. Mulchaey, John S. Bennert, Vardha N. Cox, Thomas J. Aldcroft, Thomas L. TI SDSS J1254+0846: A BINARY QUASAR CAUGHT IN THE ACT OF MERGING SO ASTROPHYSICAL JOURNAL LA English DT Review DE black hole physics; galaxies: active; galaxies: interactions; galaxies: nuclei; quasars: emission lines ID SUPERMASSIVE BLACK-HOLES; DIGITAL-SKY-SURVEY; SPACE-TELESCOPE IMAGES; ULTRALUMINOUS INFRARED GALAXIES; ABSORPTION-LINE QUASARS; DOUBLE-PEAKED EMITTER; RADIO-QUIET QUASARS; BAND IMAGING SURVEY; GALACTIC NUCLEI; HOST GALAXIES AB We present the first luminous, spatially resolved binary quasar that clearly inhabits an ongoing galaxy merger. SDSS J125455.09+084653.9 and SDSS J125454.87+084652.1 (SDSS J1254+0846 hereafter) are two luminous z = 0.44 radio-quiet quasars, with a radial velocity difference of just 215 km s(-1), separated on the sky by 21 kpc in a disturbed host galaxy merger showing obvious tidal tails. The pair was targeted as part of a complete sample of binary quasar candidates with small transverse separations drawn from SDSS DR6 photometry. We present follow-up optical imaging which shows broad, symmetrical tidal arm features spanning some 75 kpc at the quasars' redshift. Previously, the triggering of two quasars during a merger had only been hypothesized but our observations provide strong evidence of such an event. SDSS J1254+0846, as a face-on, pre-coalescence merger hosting two luminous quasars separated by a few dozen kpc, provides a unique opportunity to probe quasar activity in an ongoing gas-rich merger. Numerical modeling suggests that the system consists of two massive disk galaxies prograde to their mutual orbit, caught during the first passage of an active merger. This demonstrates rapid black hole growth during the early stages of a merger between galaxies with pre-existing bulges. Neither of the two luminous nuclei show significant intrinsic absorption by gas or dust in our optical or X-ray observations, illustrating that not all merging quasars will be in an obscured, ultraluminous phase. We find that the Eddington ratio for the fainter component B is rather normal, while for the A component L/L-Edd is quite (> 3 sigma) high compared to quasars of similar luminosity and redshift, possibly evidence for strong merger-triggered accretion. More such mergers should be identifiable at higher redshifts using binary quasars as tracers. C1 [Green, Paul J.; Cox, Thomas J.; Aldcroft, Thomas L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Myers, Adam D.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Barkhouse, Wayne A.] Univ N Dakota, Dept Phys & Astrophys, Grand Forks, ND 58202 USA. [Mulchaey, John S.; Cox, Thomas J.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA. [Bennert, Vardha N.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. RP Green, PJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM pgreen@cfa.harvard.edu FU National Aeronautics and Space Administration [GO9-0114A, NAS8-03060]; National Science Foundation; Alfred P. Sloan Foundation; NSF; US Department of Energy; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England FX Support for this work was provided by the National Aeronautics and Space Administration through Chandra Award Number GO9-0114A issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060. This paper includes data gathered with the 6.5mMagellan Telescopes located at Las Campanas Observatory, Chile. Discovery optical images were obtained at Kitt Peak National Observatory, National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under cooperative agreement with the National Science Foundation. 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 paper has used data from the SDSS archive. Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the NSF, the US Department of Energy, the National Aeronautics and Space Administration (NASA), the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSSWeb site is at http://www.sdss.org/. Thanks to Emilio Falco for valuable discussions. NR 117 TC 47 Z9 47 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 FEB 20 PY 2010 VL 710 IS 2 BP 1578 EP 1588 DI 10.1088/0004-637X/710/2/1578 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 551TN UT WOS:000274233300051 ER PT J AU Mieske, S Jordan, A Cote, P Peng, EW Ferrarese, L Blakeslee, JP Mei, S Baumgardt, H Tonry, JL Infante, L West, MJ AF Mieske, Steffen Jordan, Andres Cote, Patrick Peng, Eric W. Ferrarese, Laura Blakeslee, John P. Mei, Simona Baumgardt, Holger Tonry, John L. Infante, Leopoldo West, Michael J. TI THE ACS FORNAX CLUSTER SURVEY. IX. THE COLOR-MAGNITUDE RELATION OF GLOBULAR CLUSTER SYSTEMS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: individual (Fornax, Virgo); galaxies: fundamental parameters; globular clusters: general ID EARLY-TYPE GALAXIES; MASS-METALLICITY RELATION; DATA REDUCTION PROCEDURES; X-RAY BINARIES; VIRGO-CLUSTER; SELF-ENRICHMENT; OMEGA-CENTAURI; STAR-FORMATION; ELLIPTIC GALAXIES; WIDE-FIELD AB We investigate the color-magnitude relation for globular clusters (GCs)-the so-called blue tilt-detected in the Advanced Camera for Surveys (ACS) Fornax Cluster Survey and using the combined sample of GCs from the ACS Fornax and Virgo Cluster Surveys. We find a tilt of gamma(z) equivalent to d(g - z)/dz = -0.0257 +/- 0.0050 for the full GC sample of the Fornax Cluster Survey (approximate to 5800 GCs). This is slightly shallower than the value gamma(z) = -0.0459 +/- 0.0048 found for the Virgo Cluster Survey GC sample (approximate to 11,100 GCs). The slope for the merged Fornax and Virgo data sets (approximate to 16,900 GCs) is gamma(z) = -0.0293 +/- 0.0085, corresponding to a mass-metallicity relation of Z alpha M(0.43+0.12). We find that the blue tilt sets in at masses in excess of M similar to 2 x 10(5)M(circle dot). The tilt is stronger for GCs belonging to high-mass galaxies (M(*) greater than or similar to 5 x 10(10) M(circle dot)) than for those in low-mass galaxies (M(*) less than or similar to 5 x 10(10) M(circle dot)). It is also more pronounced for GCs with smaller galactocentric distances. Our findings suggest a range of mass-metallicity relations Z(GC) alpha M(GC)(0.3-0.7) which vary as a function of host galaxy mass/luminosity, a scaling similar to that observed for dwarf spheroidal galaxies. We compare our observations to a recent model of star cluster self-enrichment with generally favorable results. We suggest that, within the context of this model, the protocluster clouds out of which the GCs formed may have had density profiles slightly steeper than isothermal and/or star formation efficiencies somewhat below 0.3. We caution, however, that the significantly different appearance of the color-magnitude diagrams (CMDs) defined by the GC systems associated with galaxies of similar mass and morphological type poses a challenge to any single mechanism, including self-enrichment, that seeks to explain generically the observed GC color-magnitude relations. We therefore suggest that the detailed (and stochastic) merger/accretion histories of individual galaxies have likely played a non-negligible role determining the distribution of GCs in the CMDs of individual GC systems. C1 [Mieske, Steffen; West, Michael J.] European So Observ, Santiago, Chile. [Jordan, Andres; Infante, Leopoldo] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile. [Jordan, Andres] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Cote, Patrick; Ferrarese, Laura; Blakeslee, John P.] Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Peng, Eric W.] Peking Univ, Dept Astron, Beijing 100871, Peoples R China. [Mei, Simona] Univ Paris Denis Diderot, F-75205 Paris 13, France. [Mei, Simona] Observ Paris, GEPI, F-92195 Meudon, France. [Baumgardt, Holger] Argelander Inst Astron, D-53121 Bonn, Germany. [Tonry, John L.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. RP Mieske, S (reprint author), European So Observ, Alonso Cordova 3107, Santiago, Chile. RI Baumgardt, Holger/A-5444-2012; OI Jordan, Andres/0000-0002-5389-3944; Blakeslee, John/0000-0002-5213-3548 FU STScI [GO-9401, GO-10217]; NASA [NAS5-26555]; Chilean Center for Astrophysics FONDAP [15010003]; NSF [AST 02-05960]; National Aeronautics and Space Administration FX Support for programs GO-9401 and GO-10217 was provided through grants from STScI, which is operated by AURA, Inc., under NASA contract NAS5-26555. A.J. and L. I. acknowledge support from the Chilean Center of Excellence in Astrophysics and Associated Technologies and from the Chilean Center for Astrophysics FONDAP 15010003. M.J.W. acknowledges support through NSF grant AST 02-05960. 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 77 TC 41 Z9 41 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 FEB 20 PY 2010 VL 710 IS 2 BP 1672 EP 1682 DI 10.1088/0004-637X/710/2/1672 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 551TN UT WOS:000274233300060 ER PT J AU Bakos, GA Torres, G Pal, A Hartman, J Kovacs, G Noyes, RW Latham, DW Sasselov, DD Sipocz, B Esquerdo, GA Fischer, DA Johnson, JA Marcy, GW Butler, RP Isaacson, H Howard, A Vogt, S Kovacs, G Fernandez, J Moor, A Stefanik, RP Lazar, J Papp, I Sari, P AF Bakos, G. A. Torres, G. Pal, A. Hartman, J. Kovacs, Geza Noyes, R. W. Latham, D. W. Sasselov, D. D. Sipocz, B. Esquerdo, G. A. Fischer, D. A. Johnson, J. A. Marcy, G. W. Butler, R. P. Isaacson, H. Howard, A. Vogt, S. Kovacs, Gabor Fernandez, J. Moor, A. Stefanik, R. P. Lazar, J. Papp, I. Sari, P. TI HAT-P-11b: A SUPER-NEPTUNE PLANET TRANSITING A BRIGHT K STAR IN THE KEPLER FIELD SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars: individual (HAT-P-11, GSC 03561-02092); techniques: photometric; techniques: spectroscopic ID EXTRA-SOLAR PLANETS; LOWER MAIN-SEQUENCE; M-CIRCLE-PLUS; EARTH ORBITING GJ-436; HARPS SEARCH; LIGHT-CURVES; OSCILLATION FREQUENCIES; EVOLUTIONARY MODELS; ECCENTRIC ORBIT; Y-2 ISOCHRONES AB We report on the discovery of HAT-P-11b, the smallest radius transiting extrasolar planet (TEP) discovered from the ground, and the first hot Neptune discovered to date by transit searches. HAT-P-11b orbits the bright (V = 9.587) and metal rich ([Fe/H] = +0.31 +/- 0.05) K4 dwarf star GSC 03561-02092 with P = 4.8878162 +/- 0.0000071 days and produces a transit signal with depth of 4.2 mmag, the shallowest found by transit searches that is due to a confirmed planet. We present a global analysis of the available photometric and radial velocity (RV) data that result in stellar and planetary parameters, with simultaneous treatment of systematic variations. The planet, like its near-twin GJ 436b, is somewhat larger than Neptune (17 M-circle plus, 3.8 R-circle plus) both in mass M-p = 0.081 +/- 0.009 M-J (25.8 +/- 2.9 M-circle plus) and radius R-p = 0.422 +/- 0.014 R-J (4.73 +/- 0.16 R-circle plus). HAT-P-11b orbits in an eccentric orbit with e = 0.198 +/- 0.046 and omega = 355.degrees 2 +/- 17.degrees 3, causing a reflex motion of its parent star with amplitude 11.6 +/- 1.2 ms(-1), a challenging detection due to the high level of chromospheric activity of the parent star. Our ephemeris for the transit events is T-c = 2454605.89132 +/- 0.00032 (BJD), with duration 0.0957 +/- 0.0012 days, and secondary eclipse epoch of 2454608.96 +/- 0.15 days (BJD). The basic stellar parameters of the host star are M-star = 0.809(-0.027)(+0.020) M-circle dot, R-star = 0.752 +/- 0.021 R-circle dot, and T-eff star = 4780 +/- 50 K. Importantly, HAT-P-11 will lie on one of the detectors of the forthcoming Kepler mission; this should make possible fruitful investigations of the detailed physical characteristic of both the planet and its parent star at unprecedented precision. We discuss an interesting constraint on the eccentricity of the system by the transit light curve and stellar parameters. This will be particularly useful for eccentric TEPs with low-amplitude RV variations in Kepler's field. We also present a blend analysis, that for the first time treats the case of a blended transiting hot Jupiter mimicking a transiting hot Neptune, and proves that HAT-P-11b is not such a blend. C1 [Bakos, G. A.; Torres, G.; Pal, A.; Hartman, J.; Noyes, R. W.; Latham, D. W.; Sasselov, D. D.; Sipocz, B.; Esquerdo, G. A.; Kovacs, Gabor; Fernandez, J.; Stefanik, R. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Pal, A.; Sipocz, B.] Eotvos Lorand Univ, Dept Astron, Budapest, Hungary. [Kovacs, Geza; Moor, A.] Konkoly Observ Budapest, Budapest, Hungary. [Fischer, D. A.; Isaacson, H.] San Francisco State Univ, Dept Phys & Astron, San Francisco, CA 94132 USA. [Johnson, J. A.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Marcy, G. W.; Howard, A.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Butler, R. P.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20005 USA. [Vogt, S.] Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA. [Lazar, J.; Papp, I.; Sari, P.] Hungarian Astron Assoc, Budapest, Hungary. RP Bakos, GA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM gbakos@cfa.harvard.edu RI Butler, Robert/B-1125-2009; Howard, Andrew/D-4148-2015; OI Howard, Andrew/0000-0001-8638-0320; Hartman, Joel/0000-0001-8732-6166; Fischer, Debra/0000-0003-2221-0861 NR 99 TC 164 Z9 165 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 FEB 20 PY 2010 VL 710 IS 2 BP 1724 EP 1745 DI 10.1088/0004-637X/710/2/1724 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 551TN UT WOS:000274233300065 ER PT J AU Johnson, RE Markevitch, M Wegner, GA Jones, C Forman, WR AF Johnson, Ryan E. Markevitch, Maxim Wegner, Gary A. Jones, Christine Forman, William R. TI CORE GAS SLOSHING IN ABELL 1644 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: general; galaxies: clusters: individual (Abell 1644); galaxies: interactions; X-rays: galaxies: clusters ID RELAXED GALAXY CLUSTERS; COLD FRONTS; HYDRA-A; CHANDRA; SAMPLE; EINSTEIN; A1644; ROSAT; MASS; BAND AB We present an analysis of a 72 ks Chandra observation of the double cluster Abell 1644 (z = 0.047). The X-ray temperatures indicate that the masses are M(500) = (2.6 +/- 0.4) x 10(14) h(-1) M(circle dot) for the northern sub-cluster and M(500) = (3.1 +/- 0.4) x 10(14) h(-1) M(circle dot) for the southern, main cluster. We identify a sharp edge in the radial X-ray surface brightness of the main cluster, which we find to be a cold front, with a jump in temperature of a factor of similar to 3. This edge possesses a spiral morphology characteristic of core gas sloshing around the cluster potential minimum. We present observational evidence, supported by hydrodynamic simulations, that the northern sub-cluster is the object that initiated the core gas sloshing in the main cluster at least 700 Myr ago. We discuss reheating of the main cluster's core gas via two mechanisms brought about by the sloshing gas: first, the release of gravitational potential energy gained by the core's displacement from the potential minimum, and second, a dredging inward of the outer, higher entropy cluster gas along finger-shaped streams. We find that the available gravitational potential energy is small compared to the energy released by the cooling gas in the core. C1 [Johnson, Ryan E.; Wegner, Gary A.] Dartmouth Coll, Dept Phys & Astron, Wilder Lab, Hanover, NH 03755 USA. [Johnson, Ryan E.; Markevitch, Maxim; Jones, Christine; Forman, William R.] Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Johnson, RE (reprint author), Dartmouth Coll, Dept Phys & Astron, Wilder Lab, Hanover, NH 03755 USA. EM ryan.e.johnson@dartmouth.edu; mmarkevitch@cfa.harvard.edu; gary.a.wegner@bellz.dartmouth.edu; cjf@cfa.harvard.edu; wrf@cfa.harvard.edu OI Forman, William/0000-0002-9478-1682 FU NASA [NNX08AD89G, CXO GO6-7094X, GO6-7095X]; CXC [NAS8-03060] FX R.E.J. thanks Alexey Vikhlinin, John Zuhone, Scott Randall, Bill Joye, Liz Galle, and Nina Bonaventura for useful discussions and help in the Chandra data processing. R.E.J. acknowledges support for this work from a Dartmouth Graduate Fellowship along with a Smithsonian Astrophysical Observatory Predoctoral Fellowship provided by NASA through Chandra Award numbers NNX08AD89G, CXO GO6-7094X, and GO6-7095X issued by CXC, which is operated by the Smithsonian Astrophysical Observatory under contract NAS8-03060. This research has made extensive use of SAOImage DS9, in addition to software provided by CXC in the application packages CIAO, ChIPS, and Sherpa. NR 32 TC 24 Z9 24 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 FEB 20 PY 2010 VL 710 IS 2 BP 1776 EP 1785 DI 10.1088/0004-637X/710/2/1776 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 551TN UT WOS:000274233300069 ER PT J AU Brickhouse, NS Cranmer, SR Dupree, AK Luna, GJM Wolk, S AF Brickhouse, N. S. Cranmer, S. R. Dupree, A. K. Luna, G. J. M. Wolk, S. TI A DEEP CHANDRA X-RAY SPECTRUM OF THE ACCRETING YOUNG STAR TW HYDRAE SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; stars: coronae; stars: formation; stars: individual (TW Hydrae); techniques: spectroscopic; X-rays: stars ID EMISSION-LINE DIAGNOSTICS; LARGE ARRAY OBSERVATIONS; HELIUM-LIKE IONS; TAURI-STARS; DISK ACCRETION; MAGNETOSPHERIC ACCRETION; H-2 FLUORESCENCE; STELLAR CORONAE; DG-TAURI; FE-XVII AB We present X-ray spectral analysis of the accreting young star TW Hydrae from a 489 ks observation using the Chandra High Energy Transmission Grating. The spectrum provides a rich set of diagnostics for electron temperature T(e), electron density N(e), hydrogen column density N(H), relative elemental abundances, and velocities, and reveals its source in three distinct regions of the stellar atmosphere: the stellar corona, the accretion shock, and a very large extended volume of warm postshock plasma. The presence of Mg XII, Si XIII, and Si XIV emission lines in the spectrum requires coronal structures at similar to 10 MK. Lower temperature lines (e. g., from O VIII, Ne IX, and Mg XI) formed at 2.5 MK appear more consistent with emission from an accretion shock. He-like Ne IX line ratio diagnostics indicate that T(e) = 2.50 +/- 0.25 MK and N(e) = 3.0 +/- 0.2 x 10(12) cm(-3) in the shock. These values agree well with standard magnetic accretion models. However, the Chandra observations significantly diverge from current model predictions for the postshock plasma. This gas is expected to cool radiatively, producing O VII as it flows into an increasingly dense stellar atmosphere. Surprisingly, O VII indicates N(e) = 5.7(-1.2)(+4.4) x 10(11) cm(-3), 5 times lower than N(e) in the accretion shock itself and similar to 7 times lower than the model prediction. We estimate that the postshock region producing O VII has roughly 300 times larger volume and 30 times more emitting mass than the shock itself. Apparently, the shocked plasma heats the surrounding stellar atmosphere to soft X-ray emitting temperatures and supplies this material to nearby large magnetic structures-which may be closed magnetic loops or open magnetic field leading to mass outflow. Our model explains the soft X-ray excess found in many accreting systems as well as the failure to observe high N(e) signatures in some stars. Such accretion-fed coronae may be ubiquitous in the atmospheres of accreting young stars. C1 [Brickhouse, N. S.; Cranmer, S. R.; Dupree, A. K.; Luna, G. J. M.; Wolk, S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Brickhouse, NS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Brickhouse, Nancy/0000-0002-8704-4473; Wolk, Scott/0000-0002-0826-9261 FU NASA [GO7-8018X, NAS8-03060, NNG04GE77G] FX We acknowledge support from NASA to the Smithsonian Astrophysical Observatory (SAO) under Chandra GO7-8018X for G.J.M.L. N.S.B. and S.J.W. were supported by NASA contract NAS8-03060 to SAO for the Chandra X-ray Center. S. R. C.'s contribution to this work was supported by the Sprague Fund of the Smithonian Institution Research Endowment and by NASA grant NNG04GE77G to SAO. We thank Randall Smith for supporting the customized APEC code runs. We thank the Chandra Mission Planning team for their efforts to accommodate the ground-based observing campaign. NR 64 TC 68 Z9 68 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 FEB 20 PY 2010 VL 710 IS 2 BP 1835 EP 1847 DI 10.1088/0004-637X/710/2/1835 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 551TN UT WOS:000274233300074 ER PT J AU Karovska, M Gaetz, TJ Carilli, CL Hack, W Raymond, JC Lee, NP AF Karovska, Margarita Gaetz, Terrance J. Carilli, Christopher L. Hack, Warren Raymond, John C. Lee, Nicholas P. TI A PRECESSING JET IN THE CH Cyg SYMBIOTIC SYSTEM SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE accretion, accretion disks; binaries: close; stars: individual (CH Cyg); stars: winds, outflows; X-rays: general ID STARS; OUTBURST AB Jets have been detected in only a few symbiotic binaries to date, and CH Cyg is one of them. In 2001, a non-relativistic jet was detected in CH Cyg for the first time in X-rays. We carried out coordinated Chandra, Hubble Space Telescope (HST), and VLA observations in 2008 to study the propagation of this jet and its interaction with the circumbinary medium. We detected the jet with Chandra and HST and determined that the apex has expanded to the south from similar to 300 AU to similar to 1400 AU, with the shock front propagating with velocity <100 km s(-1). The shock front has significantly slowed down since 2001. Unexpectedly, we also discovered a powerful jet in the NE-SW direction, in the X-ray, optical and radio. This jet has a multi-component structure, including an inner jet and a counterjet at similar to 170 AU, and a SW component ending in several clumps extending out to similar to 750 AU. The structure of the jet and the curvature of the outer portion of the SW jet suggest an episodically powered precessing jet or a continuous precessing jet with occasional mass ejections or pulses. We carried out detailed spatial mapping of the X-ray emission and correlation with the optical and radio emission. X-ray spectra were extracted from the central source, inner NE counterjet, and the brightest clump at a distance of similar to 500 AU from the central source. We discuss the initial results of our analyses, including the multi-component spectral fitting of the jet components and of the central source. C1 [Karovska, Margarita; Gaetz, Terrance J.; Raymond, John C.; Lee, Nicholas P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Carilli, Christopher L.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Hack, Warren] Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Karovska, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mkarovska@cfa.harvard.edu NR 31 TC 5 Z9 5 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD FEB 20 PY 2010 VL 710 IS 2 BP L132 EP L136 DI 10.1088/2041-8205/710/2/L132 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 567BR UT WOS:000275417800007 ER PT J AU Marscher, AP Jorstad, SG Larionov, VM Aller, MF Aller, HD Lahteenmaki, A Agudo, I Smith, PS Gurwell, M Hagen-Thorn, VA Konstantinova, TS Larionova, EG Larionova, LV Melnichuk, DA Blinov, DA Kopatskaya, EN Troitsky, IS Tornikoski, M Hovatta, T Schmidt, GD D'Arcangelo, FD Bhattarai, D Taylor, B Olmstead, AR Manne-Nicholas, E Roca-Sogorb, M Gomez, JL McHardy, IM Kurtanidze, O Nikolashvili, MG Kimeridze, GN Sigua, LA AF Marscher, Alan P. Jorstad, Svetlana G. Larionov, Valeri M. Aller, Margo F. Aller, Hugh D. Lahteenmaki, Anne Agudo, Ivan Smith, Paul S. Gurwell, Mark Hagen-Thorn, Vladimir A. Konstantinova, Tatiana S. Larionova, Elena G. Larionova, Liudmila V. Melnichuk, Daria A. Blinov, Dmitry A. Kopatskaya, Evgenia N. Troitsky, Ivan S. Tornikoski, Merja Hovatta, Talvikki Schmidt, Gary D. D'Arcangelo, Francesca D. Bhattarai, Dipesh Taylor, Brian Olmstead, Alice R. Manne-Nicholas, Emily Roca-Sogorb, Mar Gomez, Jose L. McHardy, Ian M. Kurtanidze, Omar Nikolashvili, Maria G. Kimeridze, Givi N. Sigua, Lorand A. TI PROBING THE INNER JET OF THE QUASAR PKS 1510-089 WITH MULTI-WAVEBAND MONITORING DURING STRONG GAMMA-RAY ACTIVITY SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE gamma rays: general; polarization; quasars: individual (PKS 1510-089); radio continuum: galaxies; X-rays: galaxies ID BL-LACERTAE OBJECTS; BASE-LINE ARRAY; GALACTIC NUCLEI; POLARIMETRIC OBSERVATIONS; RELATIVISTIC JETS; HIGH-FREQUENCIES; AREA TELESCOPE; RADIO-SOURCES; 3C 279; POLARIZATION AB We present results from monitoring the multi-waveband flux, linear polarization, and parsec-scale structure of the quasar PKS 1510-089, concentrating on eight major gamma-ray flares that occurred during the interval 2009.0-2009.5. The gamma-ray peaks were essentially simultaneous with maxima at optical wavelengths, although the flux ratio of the two wave bands varied by an order of magnitude. The optical polarization vector rotated by 720 degrees during a five-day period encompassing six of these flares. This culminated in a very bright, similar to 1 day, optical and gamma-ray flare as a bright knot of emission passed through the highest-intensity, stationary feature (the "core") seen in 43 GHz Very Long Baseline Array images. The knot continued to propagate down the jet at an apparent speed of 22c and emit strongly at gamma-ray energies as a months-long X-ray/radio outburst intensified. We interpret these events as the result of the knot following a spiral path through a mainly toroidal magnetic field pattern in the acceleration and collimation zone of the jet, after which it passes through a standing shock in the 43 GHz core and then continues downstream. In this picture, the rapid gamma-ray flares result from scattering of infrared seed photons from a relatively slow sheath of the jet as well as from optical synchrotron radiation in the faster spine. The 2006-2009.7 radio and X-ray flux variations are correlated at very high significance; we conclude that the X-rays are mainly from inverse Compton scattering of infrared seed photons by 20-40 MeV electrons. C1 [Marscher, Alan P.; Jorstad, Svetlana G.; D'Arcangelo, Francesca D.; Bhattarai, Dipesh; Taylor, Brian; Olmstead, Alice R.; Manne-Nicholas, Emily] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA. [Jorstad, Svetlana G.; Larionov, Valeri M.; Hagen-Thorn, Vladimir A.; Konstantinova, Tatiana S.; Larionova, Elena G.; Larionova, Liudmila V.; Melnichuk, Daria A.; Blinov, Dmitry A.; Kopatskaya, Evgenia N.; Troitsky, Ivan S.] St Petersburg State Univ, Astron Inst, St Petersburg 198504, Russia. [Larionov, Valeri M.; Hagen-Thorn, Vladimir A.] Isaac Newton Inst Chile, St Petersburg Branch, St Petersburg, Russia. [Aller, Margo F.; Aller, Hugh D.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Lahteenmaki, Anne; Tornikoski, Merja; Hovatta, Talvikki] Helsinki Univ Technol TKK, Metsahovi Radio Observ, FIN-02540 Kylmala, Finland. [Agudo, Ivan; Roca-Sogorb, Mar; Gomez, Jose L.] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. [Smith, Paul S.; Schmidt, Gary D.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Gurwell, Mark] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Taylor, Brian] Lowell Observ, Flagstaff, AZ 86001 USA. [McHardy, Ian M.] Univ Southampton, Dept Phys & Astron, Southampton SO17 1BJ, Hants, England. [Kurtanidze, Omar; Nikolashvili, Maria G.; Kimeridze, Givi N.; Sigua, Lorand A.] Abastumani Astrophys Observ, Mt Kanobili, Abastumani, Rep of Georgia. RP Marscher, AP (reprint author), Boston Univ, Inst Astrophys Res, 725 Commonwealth Ave, Boston, MA 02215 USA. EM marscher@bu.edu RI Larionov, Valeri/H-1349-2013; Larionova, Elena/H-7287-2013; Blinov, Dmitry/G-9925-2013; Lahteenmaki, Anne/L-5987-2013; Kurtanidze, Omar/J-6237-2014; Agudo, Ivan/G-1701-2015; Morozova, Daria/H-1298-2013; Troitskiy, Ivan/K-7979-2013; Jorstad, Svetlana/H-6913-2013; Grishina, Tatiana/H-6873-2013; Hagen-Thorn, Vladimir/H-3983-2013; Kopatskaya, Evgenia/H-4720-2013 OI Larionova, Liudmila/0000-0002-0274-1481; Larionov, Valeri/0000-0002-4640-4356; Larionova, Elena/0000-0002-2471-6500; Blinov, Dmitry/0000-0003-0611-5784; Agudo, Ivan/0000-0002-3777-6182; Morozova, Daria/0000-0002-9407-7804; Troitskiy, Ivan/0000-0002-4218-0148; Jorstad, Svetlana/0000-0001-9522-5453; Grishina, Tatiana/0000-0002-3953-6676; Hagen-Thorn, Vladimir/0000-0002-6431-8590; Kopatskaya, Evgenia/0000-0001-9518-337X FU NASA [NNX08AJ64G, NNX08AV65G]; NSF [AST-0907893, AST-0607523]; Russian RFBR [09-02-0092]; Spanish "Ministerio de Ciencia e Innovacion" [AYA2007-67626-C03-03]; Academy of Finland; University of Michigan; Georgian National Science Foundation [GNSF/ST08/4-404]; Smithsonian Institution; Academia Sinica; UK Science and Technology Facilities Council FX Funding of this research included NASA grants NNX08AJ64G, NNX08AV65G, and NNX08AV65G, NSF grants AST-0907893 and AST-0607523 (U. Michigan), Russian RFBR grant 09-02-0092, Spanish "Ministerio de Ciencia e Innovacion" grant AYA2007-67626-C03-03, the Academy of Finland, the University of Michigan, and Georgian National Science Foundation grant GNSF/ST08/4-404. The VLBA is an instrument of the National Radio Astronomy Observatory, a facility of the NSF, operated under cooperative agreement by Associated Universities, Inc. The Calar Alto Observatory is jointly operated by the Max-Planck-Institut fur Astronomie and the Instituto de Astrofisica de Andalucia-CSIC. The SMA is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics, funded by the Smithsonian Institution and the Academia Sinica. The Liverpool Telescope, operated on the island of La Palma by Liverpool John Moores University in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias, is funded by the UK Science and Technology Facilities Council. NR 35 TC 191 Z9 193 U1 4 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 FEB 20 PY 2010 VL 710 IS 2 BP L126 EP L131 DI 10.1088/2041-8205/710/2/L126 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 567BR UT WOS:000275417800006 ER PT J AU Appelquist, T Avakian, A Babich, R Brower, RC Cheng, M Clark, MA Cohen, SD Fleming, GT Kiskis, J Neil, ET Osborn, JC Rebbi, C Schaich, D Vranas, P AF Appelquist, T. Avakian, A. Babich, R. Brower, R. C. Cheng, M. Clark, M. A. Cohen, S. D. Fleming, G. T. Kiskis, J. Neil, E. T. Osborn, J. C. Rebbi, C. Schaich, D. Vranas, P. TI Toward TeV Conformality SO PHYSICAL REVIEW LETTERS LA English DT Article ID GAUGE-THEORIES; SCALE; HYPERCOLOR AB We study the chiral properties of an SU(3) gauge theory with N(f) massless Dirac fermions in the fundamental representation when N(f) is increased from 2 to 6. For N(f) = 2, our lattice simulations lead to a value of <(psi) over bar psi >/F(3), where F is the Nambu-Goldstone-boson decay constant and <(psi) over bar psi > is the chiral condensate, which agrees with the measured QCD value. For N(f) = 6, this ratio shows significant enhancement, presaging an even larger enhancement anticipated as N(f) increases further, toward the critical value for transition from confinement to infrared conformality. C1 [Appelquist, T.; Fleming, G. T.; Neil, E. T.] Yale Univ, Dept Phys, Sloane Lab, New Haven, CT 06520 USA. [Avakian, A.; Babich, R.; Brower, R. C.; Cohen, S. D.; Rebbi, C.; Schaich, D.] Boston Univ, Dept Phys, Boston, MA 02215 USA. [Cheng, M.; Vranas, P.] Lawrence Livermore Natl Lab, Phys Sci Directorate, Livermore, CA 94550 USA. [Clark, M. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Clark, M. A.] Harvard Univ, Initiat Innovat Comp, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. [Kiskis, J.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Osborn, J. C.] Argonne Leadership Comp Facil, Argonne, IL 60439 USA. RP Appelquist, T (reprint author), Yale Univ, Dept Phys, Sloane Lab, New Haven, CT 06520 USA. RI Schaich, David/J-6644-2013; Fleming, George/L-6614-2013; OI Schaich, David/0000-0002-9826-2951; Fleming, George/0000-0002-4987-7167; Cohen, Saul/0000-0001-6804-3320 FU National Nuclear Security Agency and Office of Science; U.S. Department of Energy; U.S. National Science Foundation FX We thank LLNL and the Multiprogrammatic and Institutional Computing program for time on the BlueGene/L supercomputer, and the Aspen Center for Physics. This work was supported by the National Nuclear Security Agency and Office of Science (High Energy Physics), U.S. Department of Energy; and by the U.S. National Science Foundation. NR 20 TC 47 Z9 47 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 FEB 19 PY 2010 VL 104 IS 7 AR 071601 DI 10.1103/PhysRevLett.104.071601 PG 4 WC Physics, Multidisciplinary SC Physics GA 557JD UT WOS:000274664500010 PM 20366870 ER PT J AU Borucki, WJ Koch, D Basri, G Batalha, N Brown, T Caldwell, D Caldwell, J Christensen-Dalsgaard, J Cochran, WD DeVore, E Dunham, EW Dupree, AK Gautier, TN Geary, JC Gilliland, R Gould, A Howell, SB Jenkins, JM Kondo, Y Latham, DW Marcy, GW Meibom, S Kjeldsen, H Lissauer, JJ Monet, DG Morrison, D Sasselov, D Tarter, J Boss, A Brownlee, D Owen, T Buzasi, D Charbonneau, D Doyle, L Fortney, J Ford, EB Holman, MJ Seager, S Steffen, JH Welsh, WF Rowe, J Anderson, H Buchhave, L Ciardi, D Walkowicz, L Sherry, W Horch, E Isaacson, H Everett, ME Fischer, D Torres, G Johnson, JA Endl, M MacQueen, P Bryson, ST Dotson, J Haas, M Kolodziejczak, J Van Cleve, J Chandrasekaran, H Twicken, JD Quintana, EV Clarke, BD Allen, C Li, J Wu, H Tenenbaum, P Verner, E Bruhweiler, F Barnes, J Prsa, A AF Borucki, William J. Koch, David Basri, Gibor Batalha, Natalie Brown, Timothy Caldwell, Douglas Caldwell, John Christensen-Dalsgaard, Jorgen Cochran, William D. DeVore, Edna Dunham, Edward W. Dupree, Andrea K. Gautier, Thomas N., III Geary, John C. Gilliland, Ronald Gould, Alan Howell, Steve B. Jenkins, Jon M. Kondo, Yoji Latham, David W. Marcy, Geoffrey W. Meibom, Soren Kjeldsen, Hans Lissauer, Jack J. Monet, David G. Morrison, David Sasselov, Dimitar Tarter, Jill Boss, Alan Brownlee, Don Owen, Toby Buzasi, Derek Charbonneau, David Doyle, Laurance Fortney, Jonathan Ford, Eric B. Holman, Matthew J. Seager, Sara Steffen, Jason H. Welsh, William F. Rowe, Jason Anderson, Howard Buchhave, Lars Ciardi, David Walkowicz, Lucianne Sherry, William Horch, Elliott Isaacson, Howard Everett, Mark E. Fischer, Debra Torres, Guillermo Johnson, John Asher Endl, Michael MacQueen, Phillip Bryson, Stephen T. Dotson, Jessie Haas, Michael Kolodziejczak, Jeffrey Van Cleve, Jeffrey Chandrasekaran, Hema Twicken, Joseph D. Quintana, Elisa V. Clarke, Bruce D. Allen, Christopher Li, Jie Wu, Haley Tenenbaum, Peter Verner, Ekaterina Bruhweiler, Frederick Barnes, Jason Prsa, Andrej TI Kepler Planet-Detection Mission: Introduction and First Results SO SCIENCE LA English DT Article ID EXOPLANETS; HAT-P-7B; EARTH; FIELD; STAR AB The Kepler mission was designed to determine the frequency of Earth-sized planets in and near the habitable zone of Sun-like stars. The habitable zone is the region where planetary temperatures are suitable for water to exist on a planet's surface. During the first 6 weeks of observations, Kepler monitored 156,000 stars, and five new exoplanets with sizes between 0.37 and 1.6 Jupiter radii and orbital periods from 3.2 to 4.9 days were discovered. The density of the Neptune-sized Kepler-4b is similar to that of Neptune and GJ 436b, even though the irradiation level is 800,000 times higher. Kepler-7b is one of the lowest-density planets (similar to 0.17 gram per cubic centimeter) yet detected. Kepler-5b, -6b, and -8b confirm the existence of planets with densities lower than those predicted for gas giant planets. C1 [Borucki, William J.; Koch, David; Lissauer, Jack J.; Morrison, David; Rowe, Jason; Bryson, Stephen T.; Dotson, Jessie; Haas, Michael] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Basri, Gibor; Marcy, Geoffrey W.; Anderson, Howard; Walkowicz, Lucianne; Isaacson, Howard] Univ Calif Berkeley, Berkeley, CA 94720 USA. [Batalha, Natalie] San Jose State Univ, San Jose, CA 95192 USA. [Brown, Timothy] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA. [Caldwell, Douglas; DeVore, Edna; Jenkins, Jon M.; Tarter, Jill; Doyle, Laurance; Van Cleve, Jeffrey; Chandrasekaran, Hema; Twicken, Joseph D.; Quintana, Elisa V.; Clarke, Bruce D.; Li, Jie; Wu, Haley; Tenenbaum, Peter] SETI Inst, Mountain View, CA 94043 USA. [Christensen-Dalsgaard, Jorgen; Kjeldsen, Hans] Aarhus Univ, Aarhus, Denmark. [Cochran, William D.; Endl, Michael; MacQueen, Phillip] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA. [Dunham, Edward W.] Lowell Observ, Flagstaff, AZ 86001 USA. [Gautier, Thomas N., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Dupree, Andrea K.; Geary, John C.; Latham, David W.; Meibom, Soren; Sasselov, Dimitar; Charbonneau, David; Holman, Matthew J.; Buchhave, Lars; Torres, Guillermo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gilliland, Ronald] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Monet, David G.] US Naval Observ, Flagstaff, AZ 86001 USA. [Ford, Eric B.] Univ Florida, Gainesville, FL 32611 USA. [Everett, Mark E.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Howell, Steve B.; Sherry, William] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Fischer, Debra] Yale Univ, New Haven, CT 06520 USA. [Caldwell, John] York Univ, N York, ON M3J 1P3, Canada. [Gould, Alan] Lawrence Hall Sci, Berkeley, CA 94720 USA. [Boss, Alan] Carnegie Inst Washington, Washington, DC 20015 USA. [Owen, Toby] Univ Hawaii, Hilo, HI 96720 USA. [Brownlee, Don] Univ Washington, Seattle, WA 98195 USA. [Buzasi, Derek] Eureka Sci, Oakland, CA 94602 USA. [Horch, Elliott] So Connecticut State Univ, New Haven, CT 06515 USA. [Fortney, Jonathan] Univ Calif Santa Cruz, Santa Cruz, CA 95064 USA. [Seager, Sara] MIT, Cambridge, MA 02139 USA. [Steffen, Jason H.] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA. [Welsh, William F.] San Diego State Univ, San Diego, CA 92182 USA. [Ciardi, David; Johnson, John Asher] CALTECH, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Kondo, Yoji] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20025 USA. [Kolodziejczak, Jeffrey] George C Marshall Space Flight Ctr, Huntsville, AL 35805 USA. [Allen, Christopher] Orbital Sci, Mountain View, CA 94043 USA. [Verner, Ekaterina; Bruhweiler, Frederick] Catholic Univ Amer, Washington, DC 20064 USA. [Barnes, Jason] Univ Idaho, Moscow, ID 83844 USA. [Prsa, Andrej] Villanova Univ, Villanova, PA 19085 USA. RP Borucki, WJ (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM William.J.Borucki@nasa.gov RI Barnes, Jason/B-1284-2009; Steffen, Jason/A-4320-2013; rowe, james/C-3661-2013; Caldwell, Douglas/L-7911-2014; OI Barnes, Jason/0000-0002-7755-3530; rowe, james/0000-0001-7216-8679; Caldwell, Douglas/0000-0003-1963-9616; Fortney, Jonathan/0000-0002-9843-4354; Buchhave, Lars A./0000-0003-1605-5666; Ciardi, David/0000-0002-5741-3047 FU NASA FX Kepler was competitively selected as the 10th Discovery mission. Funding for this mission is provided by NASA's Science Mission Directorate. NR 33 TC 946 Z9 947 U1 51 U2 197 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 FEB 19 PY 2010 VL 327 IS 5968 BP 977 EP 980 DI 10.1126/science.1185402 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 556XE UT WOS:000274625800034 PM 20056856 ER PT J AU Abdo, AA Ackermann, M Ajello, M Axelsson, M Baldini, L Ballet, J Barbiellini, G Bastieri, D Baughman, BM Bechtol, K Bellazzini, R Berenji, B Blandford, RD Bloom, ED Bock, DCJ Bogart, JR Bonamente, E Borgland, AW Bouvier, A Bregeon, J Brez, A Brigida, M Bruel, P Burnett, TH Buson, S Caliandro, GA Cameron, RA Caraveo, PA Casandjian, JM Cavazzuti, E Cecchi, C Celik, O Chekhtman, A Cheung, CC Chiang, J Ciprini, S Claus, R Cohen-Tanugi, J Collmar, W Cominsky, LR Conrad, J Corbel, S Corbet, R Costamante, L Cutini, S Dermer, CD de Angelis, A de Palma, F Digel, SW Silva, EDE Drell, PS Dubois, R Dumora, D Farnier, C Favuzzi, C Fegan, SJ Ferrara, EC Focke, WB Fortin, P Frailis, M Fuhrmann, L Fukazawa, Y Funk, S Fusco, P Gargano, F Gasparrini, D Gehrels, N Germani, S Giebels, B Giglietto, N Giommi, P Giordano, F Giroletti, M Glanzman, T Godfrey, G Grenier, IA Grove, JE Guillemot, L Guiriec, S Hanabata, Y Harding, AK Hayashida, M Hays, E Horan, D Hughes, RE Iafrate, G Itoh, R Jackson, MS Johannesson, G Johnson, AS Johnson, WN Kadler, M Kamae, T Katagiri, H Kataoka, J Kawai, N Kerr, M Knodlseder, J Kocian, ML Kuss, M Lande, J Larsson, S Latronico, L Lemoine-Goumard, M Longo, F Loparco, F Lott, B Lovellette, MN Lubrano, P Macquart, J Madejski, GM Makeev, A Max-Moerbeck, W Mazziotta, MN McConville, W McEnery, JE McGlynn, S Meurer, C Michelson, F Mitthumsiri, W Mizuno, T Moiseev, AA Monte, C Monzani, ME Morselli, A Moskalenko, IV Murgia, S Nestoras, I Nolan, PL Norris, JP Nuss, E Ohsugi, T Okumura, A Omodei, N Orlando, E Ormes, JF Paneque, D Panetta, JH Parent, D Pavlidou, V Pearson, TJ Pelassa, V Pepe, M Pesce-Rollins, M Piron, F Porter, TA Raino, S Rando, R Razzano, M Readhead, A Reimer, A Reimer, O Reposeur, T Reyes, LC Richards, JL Rochester, LS Rodriguez, AY Roth, M Ryde, F Sadrozinski, HFW Sanchez, D Sander, A Parkinson, PMS Scargle, JD Sgro, C Shaw, MS Shrader, C Siskind, EJ Smith, DA Smith, PD Spandre, G Spinelli, P Stawarz, L Stevenson, M Strickman, MS Suson, DJ Tajima, H Takahashi, H Takahashi, T Tanaka, T Taylor, GB Thayer, JB Thayer, JG Thompson, DJ Tibaldo, L Torres, DF Tosti, G Tramacere, A Uchiyama, Y Usher, TL Vasileiou, V Vilchez, N Vitale, V Waite, AP Wang, P Wehrle, AE Winer, BL Wood, KS Ylinen, T Zensus, JA Ziegler, M Uemura, M Ikejiri, Y Kawabata, KS Kino, M Sakimoto, K Sasada, M Sato, S Yamanaka, M Villata, M Raiteri, CM Agudo, I Aller, HD Aller, MF Angelakis, E Arkharov, AA Bach, U Benitez, E Berdyugin, A Blinov, DA Boettcher, M Buemi, CS Chen, WP Dolci, M Dultzin, D Efimova, NV Gurwell, MA Gusbar, C Gomez, JL Heidt, J Hiriart, D Hovatta, T Jorstad, SG Konstantinova, TS Kopatskaya, EN Koptelova, E Kurtanidze, OM Lahteenmaki, A Larionov, VM Larionova, EG Leto, P Lin, HC Lindfors, E Marscher, AP McHardy, IM Melnichuk, DA Mommert, M Nilsson, K Di Paola, A Reinthal, R Richter, GM Roca-Sogorb, M Roustazadeh, P Sigua, LA Takalo, LO Tornikoski, M Trigilio, C Troitsky, IS Umana, G Villforth, C Grainge, K Moderski, R Nalewajko, K Sikora, M AF Abdo, A. A. Ackermann, M. Ajello, M. Axelsson, M. Baldini, L. Ballet, J. Barbiellini, G. Bastieri, D. Baughman, B. M. Bechtol, K. Bellazzini, R. Berenji, B. Blandford, R. D. Bloom, E. D. Bock, D. C. -J. Bogart, J. R. Bonamente, E. Borgland, A. W. Bouvier, A. Bregeon, J. Brez, A. Brigida, M. Bruel, P. Burnett, T. H. Buson, S. Caliandro, G. A. Cameron, R. A. Caraveo, P. A. Casandjian, J. M. Cavazzuti, E. Cecchi, C. Celik, Oe Chekhtman, A. Cheung, C. C. Chiang, J. Ciprini, S. Claus, R. Cohen-Tanugi, J. Collmar, W. Cominsky, L. R. Conrad, J. Corbel, S. Corbet, R. Costamante, L. Cutini, S. Dermer, C. D. de Angelis, A. de Palma, F. Digel, S. W. 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. Fortin, P. Frailis, M. Fuhrmann, L. Fukazawa, Y. Funk, S. Fusco, P. Gargano, F. Gasparrini, D. Gehrels, N. Germani, S. Giebels, B. Giglietto, N. Giommi, P. Giordano, F. Giroletti, M. Glanzman, T. Godfrey, G. Grenier, I. A. Grove, J. E. Guillemot, L. Guiriec, S. Hanabata, Y. Harding, A. K. Hayashida, M. Hays, E. Horan, D. Hughes, R. E. Iafrate, G. Itoh, R. Jackson, M. S. Johannesson, G. Johnson, A. S. Johnson, W. N. Kadler, M. Kamae, T. Katagiri, H. Kataoka, J. Kawai, N. Kerr, M. Knoedlseder, J. Kocian, M. L. Kuss, M. Lande, J. Larsson, S. Latronico, L. Lemoine-Goumard, M. Longo, F. Loparco, F. Lott, B. Lovellette, M. N. Lubrano, P. Macquart, J. Madejski, G. M. Makeev, A. Max-Moerbeck, W. Mazziotta, M. N. McConville, W. McEnery, J. E. McGlynn, S. Meurer, C. Michelson, F. Mitthumsiri, W. Mizuno, T. Moiseev, A. A. Monte, C. Monzani, M. E. Morselli, A. Moskalenko, I. V. Murgia, S. Nestoras, I. Nolan, P. L. Norris, J. P. Nuss, E. Ohsugi, T. Okumura, A. Omodei, N. Orlando, E. Ormes, J. F. Paneque, D. Panetta, J. H. Parent, D. Pavlidou, V. Pearson, T. J. Pelassa, V. Pepe, M. Pesce-Rollins, M. Piron, F. Porter, T. A. Raino, S. Rando, R. Razzano, M. Readhead, A. Reimer, A. Reimer, O. Reposeur, T. Reyes, L. C. Richards, J. L. Rochester, L. S. Rodriguez, A. Y. Roth, M. Ryde, F. Sadrozinski, H. F. -W. Sanchez, D. Sander, A. Parkinson, P. M. Saz Scargle, J. D. Sgro, C. Shaw, M. S. Shrader, C. Siskind, E. J. Smith, D. A. Smith, P. D. Spandre, G. Spinelli, P. Stawarz, L. Stevenson, M. Strickman, M. S. Suson, D. J. Tajima, H. Takahashi, H. Takahashi, T. Tanaka, T. Taylor, G. B. Thayer, J. B. Thayer, J. G. Thompson, D. J. Tibaldo, L. Torres, D. F. Tosti, G. Tramacere, A. Uchiyama, Y. Usher, T. L. Vasileiou, V. Vilchez, N. Vitale, V. Waite, A. P. Wang, P. Wehrle, A. E. Winer, B. L. Wood, K. S. Ylinen, T. Zensus, J. A. Ziegler, M. Uemura, M. Ikejiri, Y. Kawabata, K. S. Kino, M. Sakimoto, K. Sasada, M. Sato, S. Yamanaka, M. Villata, M. Raiteri, C. M. Agudo, I. Aller, H. D. Aller, M. F. Angelakis, E. Arkharov, A. A. Bach, U. Benitez, E. Berdyugin, A. Blinov, D. A. Boettcher, M. Buemi, C. S. Chen, W. P. Dolci, M. Dultzin, D. Efimova, N. V. Gurwell, M. A. Gusbar, C. Gomez, J. L. Heidt, J. Hiriart, D. Hovatta, T. Jorstad, S. G. Konstantinova, T. S. Kopatskaya, E. N. Koptelova, E. Kurtanidze, O. M. Lahteenmaki, A. Larionov, V. M. Larionova, E. G. Leto, P. Lin, H. C. Lindfors, E. Marscher, A. P. McHardy, I. M. Melnichuk, D. A. Mommert, M. Nilsson, K. Di Paola, A. Reinthal, R. Richter, G. M. Roca-Sogorb, M. Roustazadeh, P. Sigua, L. A. Takalo, L. O. Tornikoski, M. Trigilio, C. Troitsky, I. S. Umana, G. Villforth, C. Grainge, K. Moderski, R. Nalewajko, K. Sikora, M. CA Fermi LAT Collaboration 3C 279 Multiband Campaign TI A change in the optical polarization associated with a gamma-ray flare in the blazar 3C 279 SO NATURE LA English DT Article ID ACTIVE GALACTIC NUCLEUS; RELATIVISTIC JET; RADIO-SOURCES; VARIABILITY; EMISSION; TELESCOPE; RADIATION; QUASAR; ULTRAVIOLET; 3C-279 AB It is widely accepted that strong and variable radiation detected over all accessible energy bands in a number of active galaxies arises from a relativistic, Doppler-boosted jet pointing close to our line of sight(1). The size of the emitting zone and the location of this region relative to the central supermassive black hole are, however, poorly known, with estimates ranging from light-hours to a light-year or more. Here we report the coincidence of a gamma (gamma)-ray flare with a dramatic change of optical polarization angle. This provides evidence for co-spatiality of optical and gamma-ray emission regions and indicates a highly ordered jet magnetic field. The results also require a non-axisymmetric structure of the emission zone, implying a curved trajectory for the emitting material within the jet, with the dissipation region located at a considerable distance from the black hole, at about 10(5) gravitational radii. C1 [Ackermann, M.; Ajello, M.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bogart, J. R.; Borgland, A. W.; Bouvier, A.; Cameron, R. A.; Chiang, J.; Claus, R.; Costamante, L.; Digel, S. W.; 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.; Kocian, M. L.; Lande, J.; Madejski, G. M.; Michelson, F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Paneque, D.; Panetta, J. H.; Reimer, A.; Reimer, O.; Rochester, L. S.; Shaw, M. S.; Stawarz, L.; Tajima, H.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Waite, A. P.; Wang, P.] Stanford Univ, Dept Phys, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [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, Natl Res Council Res Associate, Washington, DC 20001 USA. [Ackermann, M.; Ajello, M.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bogart, J. 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V.] Pulkovo Observ, St Petersburg 196140, Russia. [Benitez, E.; Dultzin, D.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. [Berdyugin, A.; Blinov, D. A.; Lindfors, E.; Nilsson, K.; Reinthal, R.; Takalo, L. O.; Villforth, C.] Univ Turku, Tuorla Observ, FI-21500 Piikkio, Finland. [Blinov, D. A.; Efimova, N. V.; Konstantinova, T. S.; Kopatskaya, E. N.; Larionov, V. M.; Larionova, E. G.; Melnichuk, D. A.; Troitsky, I. S.] St Petersburg State Univ, Astron Inst, St Petersburg, Russia. [Boettcher, M.; Gusbar, C.; Roustazadeh, P.] Ohio Univ, Dept Phys & Astron, Athens, OH 45701 USA. [Buemi, C. S.; Leto, P.; Trigilio, C.; Umana, G.] Osserv Astrofis Catania, I-95123 Catania, Italy. [Chen, W. P.; Koptelova, E.; Lin, H. C.] Natl Cent Univ, Grad Inst Astron, Jhongli 32054, Taiwan. [Dolci, M.] Osservatorio Astron Collurania, INAF, I-64100 Teramo, Italy. [Gurwell, M. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Heidt, J.; Mommert, M.] Heidelberg Univ, D-69117 Heidelberg, Germany. [Hiriart, D.] Univ Nacl Autonoma Mexico, Inst Astron, Ensenada 22860, Baja California, Mexico. [Hovatta, T.; Lahteenmaki, A.; Tornikoski, M.] Aalto Univ, Metsahovi Radio Observ, FIN-02540 Kylmala, Finland. [Jorstad, S. G.; Marscher, A. P.] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA. [Kurtanidze, O. M.; Sigua, L. A.] Abastumani Observ, GE-0301 Mt Kanobili, Abastumani, Rep of Georgia. [McHardy, I. M.] Univ Southampton, Sch Phys & Astron, Southampton SO17 BJ, Hants, England. [Di Paola, A.] Osserv Astron Roma, I-00040 Monte Porzio Catone, Italy. [Richter, G. M.] Astrophys Inst Potsdam, D-14482 Potsdam, Germany. [Grainge, K.] Univ Cambridge, Cavendish Lab, Cambridge CB3 0HE, England. [Moderski, R.; Nalewajko, K.; Sikora, M.] Nicolaus Copernicus Astron Ctr, PL-00716 Warsaw, Poland. RP Hayashida, M (reprint author), Stanford Univ, Dept Phys, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. EM hayasida@stanford.edu; madejski@slac.stanford.edu RI Larionov, Valeri/H-1349-2013; Kopatskaya, Evgenia/H-4720-2013; Thompson, David/D-2939-2012; Harding, Alice/D-3160-2012; 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; Nolan, Patrick/A-5582-2009; Kuss, Michael/H-8959-2012; giglietto, nicola/I-8951-2012; Macquart, Jean-Pierre/B-5306-2013; Tosti, Gino/E-9976-2013; Larionova, Elena/H-7287-2013; Efimova, Natalia/I-2196-2013; Saz Parkinson, Pablo Miguel/I-7980-2013; Blinov, Dmitry/G-9925-2013; Rando, Riccardo/M-7179-2013; Lahteenmaki, Anne/L-5987-2013; Hays, Elizabeth/D-3257-2012; Johnson, Neil/G-3309-2014; Reimer, Olaf/A-3117-2013; Kurtanidze, Omar/J-6237-2014; Funk, Stefan/B-7629-2015; Pavlidou, Vasiliki/C-2944-2011; Agudo, Ivan/G-1701-2015; Pearson, Timothy/N-2376-2015; Morozova, Daria/H-1298-2013; Troitskiy, Ivan/K-7979-2013; Jorstad, Svetlana/H-6913-2013; Grishina, Tatiana/H-6873-2013; Loparco, Francesco/O-8847-2015; Johannesson, Gudlaugur/O-8741-2015; Gargano, Fabio/O-8934-2015; Moskalenko, Igor/A-1301-2007; Mazziotta, Mario /O-8867-2015; Sgro, Carmelo/K-3395-2016; Torres, Diego/O-9422-2016; OI Larionov, Valeri/0000-0002-4640-4356; Kopatskaya, Evgenia/0000-0001-9518-337X; Thompson, David/0000-0001-5217-9135; lubrano, pasquale/0000-0003-0221-4806; Morselli, Aldo/0000-0002-7704-9553; giglietto, nicola/0000-0002-9021-2888; Larionova, Elena/0000-0002-2471-6500; Efimova, Natalia/0000-0002-8071-4753; Blinov, Dmitry/0000-0003-0611-5784; Reimer, Olaf/0000-0001-6953-1385; Funk, Stefan/0000-0002-2012-0080; Pavlidou, Vasiliki/0000-0002-0870-1368; Agudo, Ivan/0000-0002-3777-6182; Pearson, Timothy/0000-0001-5213-6231; Morozova, Daria/0000-0002-9407-7804; Troitskiy, Ivan/0000-0002-4218-0148; Jorstad, Svetlana/0000-0001-9522-5453; Grishina, Tatiana/0000-0002-3953-6676; Loparco, Francesco/0000-0002-1173-5673; Johannesson, Gudlaugur/0000-0003-1458-7036; Gargano, Fabio/0000-0002-5055-6395; Moskalenko, Igor/0000-0001-6141-458X; Mazziotta, Mario /0000-0001-9325-4672; Torres, Diego/0000-0002-1522-9065; Dolci, Mauro/0000-0001-8000-5642; Buemi, Carla Simona/0000-0002-7288-4613; giommi, paolo/0000-0002-2265-5003; Di Paola, Andrea/0000-0002-2189-8644; De Angelis, Alessandro/0000-0002-3288-2517; Iafrate, Giulia/0000-0002-6185-8292; Frailis, Marco/0000-0002-7400-2135; Villata, Massimo/0000-0003-1743-6946; Caraveo, Patrizia/0000-0003-2478-8018; Leto, Paolo/0000-0003-4864-2806; Sgro', Carmelo/0000-0001-5676-6214 FU Georgian National Science Foundation; Spanish "Ministerio de Ciencia e Innovacion''; NSF; NASA; Smithsonian Institution in the United States; UK Science and Technology Facilities Council; Academia Sinica in Taiwan; Russian RFBR; Academy of Finland; JSPS; K. A. Wallenberg Foundation FX 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 for science analysis during the operations phase is also gratefully acknowledged. The GASP-WEBT observatories participating in this work are Abastumani, Calar Alto, Campo Imperatore, Crimean, Kitt Peak (MDM), L'Ampolla, Lowell (Perkins-PRISM), Lulin, Roque de los Muchachos (KVA and Liverpool), San Pedro Martir, St Petersburg for the optical-NIR bands, and Mauna Kea (SMA), Medicina, Metsahovi, Noto and UMRAO for the millimetre radio band, and are supported in part by the Georgian National Science Foundation, the Spanish "Ministerio de Ciencia e Innovacion'', the NSF and NASA and the Smithsonian Institution in the United States, the UK Science and Technology Facilities Council, the Academia Sinica in Taiwan, the Russian RFBR and the Academy of Finland. M. H. is supported by the JSPS for the Postdoctoral Fellowship for Research Abroad. J. Conrad is a Royal Swedish Academy of Sciences Research Fellow, funded by a grant from the K. A. Wallenberg Foundation. L. T. is partially supported by the International Doctorate on Astroparticle Physics (IDAPP) programme. NR 25 TC 164 Z9 165 U1 1 U2 22 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 EI 1476-4687 J9 NATURE JI Nature PD FEB 18 PY 2010 VL 463 IS 7283 BP 919 EP 923 DI 10.1038/nature08841 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 556HZ UT WOS:000274582700039 ER PT J AU Rueda, LM Brown, TL Kim, HC Chong, ST Klein, TA Foley, DH Anyamba, A Smith, M Pak, EP Wilkerson, RC AF Rueda, Leopoldo M. Brown, Tracy L. Kim, Heung Chul Chong, Sung-Tae Klein, Terry A. Foley, Desmond H. Anyamba, Assaf Smith, Matthew Pak, Edwin P. Wilkerson, Richard C. TI Species composition, larval habitats, seasonal occurrence and distribution of potential malaria vectors and associated species of Anopheles (Diptera: Culicidae) from the Republic of Korea SO MALARIA JOURNAL LA English DT Article ID ECOLOGICAL CONDITIONS; SATELLITE DATA; IMAGERY; KENYA AB Background: Larval mosquito habitats of potential malaria vectors and related species of Anopheles from three provinces (Gyeonggi, Gyeongsangbuk, Chungcheongbuk Provinces) of the Republic of Korea were surveyed in 2007. This study aimed to determine the species composition, seasonal occurrence and distributions of Anopheles mosquitoes. Satellite derived normalized difference vegetation index data (NDVI) was also used to study the seasonal abundance patterns of Anopheles mosquitoes. Methods: Mosquito larvae from various habitats were collected using a standard larval dipper or a white plastic larval tray, placed in plastic bags, and were preserved in 100% ethyl alcohol for species identification by PCR and DNA sequencing. The habitats in the monthly larval surveys included artificial containers, ground depressions, irrigation ditches, drainage ditches, ground pools, ponds, rice paddies, stream margins, inlets and pools, swamps, and uncultivated fields. All field-collected specimens were identified to species, and relationships among habitats and locations based on species composition were determined using cluster statistical analysis. Results: In about 10,000 specimens collected, eight species of Anopheles belonging to three groups were identified: Hyrcanus Group - Anopheles sinensis, Anopheles kleini, Anopheles belenrae, Anopheles pullus, Anopheles lesteri, Anopheles sineroides; Barbirostris Group - Anopheles koreicus; and Lindesayi Group - Anopheles lindesayi japonicus. Only An. sinensis was collected from all habitats groups, while An. kleini, An. pullus and An. sineroides were sampled from all, except artificial containers. The highest number of Anopheles larvae was found in the rice paddies (34.8%), followed by irrigation ditches (23.4%), ponds (17.0%), and stream margins, inlets and pools (12.0%). Anopheles sinensis was the dominant species, followed by An. kleini, An. pullus and An. sineroides. The monthly abundance data of the Anopheles species from three locations (Munsan, Jinbo and Hayang) were compared against NDVI and NDVI anomalies. Conclusion: The species composition of Anopheles larvae varied in different habitats at various locations. Anopheles populations fluctuated with the seasonal dynamics of vegetation for 2007. Multi-year data of mosquito collections are required to provide a better characterization of the abundance of these insects from year to year, which can potentially provide predictive capability of their population density based on remotely sensed ecological measurements. C1 [Rueda, Leopoldo M.; Brown, Tracy L.; Foley, Desmond H.; Wilkerson, Richard C.] Walter Reed Army Inst Res, Div Entomol, Silver Spring, MD 20910 USA. [Rueda, Leopoldo M.; Brown, Tracy L.; Foley, Desmond H.; Wilkerson, Richard C.] Smithsonian Inst, Museum Support Ctr, WRAIR, Walter Reed Biosystemat Unit, Suitland, MD 20746 USA. [Kim, Heung Chul; Chong, Sung-Tae] Unit 15247, APO, AP 96205 USA. [Klein, Terry A.] Unit 15281, USAMEDDAC Korea, APO, AP 96205 USA. [Anyamba, Assaf; Smith, Matthew; Pak, Edwin P.] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA. RP Rueda, LM (reprint author), Walter Reed Army Inst Res, Div Entomol, Silver Spring, MD 20910 USA. EM ruedapol@si.edu RI Valle, Ruben/A-7512-2013; OI Foley, Desmond/0000-0001-7525-4601 FU Center for Health Promotion and Preventive Medicine; Global Emerging Infections Surveillance and Response Systems, Silver Spring, MD; Walter Reed Army Institute of Research; Smithsonian Institution FX Thanks go to A. Driskell and G. Harrison (Laboratory of Analytical Biology, Smithsonian Institution) for conducting PCR/sequencing of some mosquito samples; personnel of the 5th Medical Detachment, and staff of 65th Medical Brigade, U. S. Army, ROK, for field collections of mosquito specimens; and J. Pecor and WRBU staff for curatorial help. Special thanks go to D. J. Brambilla (Research Triangle Institute, Research Triangle Park, NC) for statistical analysis; and G. Bieler (RTP, NC), C. Lim (WRAIR) and V. Sherwood (WRAIR) for statistical and related support. We are grateful to F. Ruiz, C. R. Summers and B. P. Rueda for helpful reviews of the manuscript. Funding for this work was provided by the Center for Health Promotion and Preventive Medicine, Global Emerging Infections Surveillance and Response Systems, Silver Spring, MD. 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 opinions and assertions contained herein are those of the authors and are not to be construed as official or reflecting the views of the Department of the Army or the Department of Defense. NR 27 TC 14 Z9 14 U1 0 U2 8 PU BIOMED CENTRAL LTD PI LONDON PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND SN 1475-2875 J9 MALARIA J JI Malar. J. PD FEB 17 PY 2010 VL 9 AR 55 DI 10.1186/1475-2875-9-55 PG 11 WC Infectious Diseases; Parasitology; Tropical Medicine SC Infectious Diseases; Parasitology; Tropical Medicine GA 567RI UT WOS:000275463900002 PM 20163728 ER PT J AU Abrahamovich, AH Lucia, M Alvarez, LJ Smith, DR AF Abrahamovich, Alberto H. Lucia, Mariano Alvarez, Leopoldo J. Smith, David R. TI Type specimens of sawflies (Insecta: Hymenoptera: Symphyta) housed in the Museo de La Plata, Argentina SO ZOOTAXA LA English DT Article DE sawflies; catalogue; type material; Museo de La Plata Collection ID UNITED-STATES; AMERICA SOUTH; TENTHREDINIDAE; SYNOPSIS AB The primary and secondary type specimens of 27 species of sawflies housed at the Museo de La Plata (Division Entomolog a), Argentina are listed. Information on kinds of types, collection data, and current status are provided. The types belong to species described by P. Jorgensen, C. Schrottky, and D. R. Smith. Two new synonymies are recognized: Aphilodyctium nigripenne Schrottky, 1913 syn. nov. of Waldheimia nigripennis Jorgensen 1913 and Siobla argentina Schrottky, 1913 syn. nov. of Stromboceros argentinus Jorgensen 1913. C1 [Abrahamovich, Alberto H.; Lucia, Mariano; Alvarez, Leopoldo J.] Univ Nacl La Plata, Museo La Plata, Div Entomol, La Plata, Buenos Aires, Argentina. [Abrahamovich, Alberto H.; Lucia, Mariano; Alvarez, Leopoldo J.] CONICET CIC, Buenos Aires, DF, Argentina. [Smith, David R.] ARS, Systemat Entomol Lab, PSI, USDA,Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA. RP Abrahamovich, AH (reprint author), Univ Nacl La Plata, Museo La Plata, Div Entomol, Paseo Bosque S-N,B1900DNG, La Plata, Buenos Aires, Argentina. EM albertoa@fcnym.unlp.edu.ar; smith@ars.usda.gov NR 17 TC 1 Z9 1 U1 0 U2 0 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD FEB 16 PY 2010 IS 2360 BP 63 EP 68 PG 6 WC Zoology SC Zoology GA 557AR UT WOS:000274640400004 ER PT J AU Guz, SS AF Guz, Savannah Schroll TI Fibromyalgia 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 FEB 15 PY 2010 VL 135 IS 3 BP 118 EP 118 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 556QM UT WOS:000274606200220 ER PT J AU Guz, SS AF Guz, Savannah Schroll TI Cancer 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 FEB 15 PY 2010 VL 135 IS 3 BP 118 EP 118 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 556QM UT WOS:000274606200223 ER PT J AU Guz, SS AF Guz, Savannah Schroll TI Poisons and Antidotes 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 FEB 15 PY 2010 VL 135 IS 3 BP 118 EP 118 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 556QM UT WOS:000274606200225 ER PT J AU Guz, SS AF Guz, Savannah Schroll TI The Child Abuse Sourcebook, 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 FEB 15 PY 2010 VL 135 IS 3 BP 118 EP 118 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 556QM UT WOS:000274606200219 ER PT J AU Guz, SS AF Guz, Savannah Schroll TI The Handbook of Adolescent Psychology, 3rd 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 5 PU REED BUSINESS INFORMATION PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD FEB 15 PY 2010 VL 135 IS 3 BP 118 EP 118 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 556QM UT WOS:000274606200221 ER PT J AU Guz, SS AF Guz, Savannah Schroll TI Men's Health Concerns Sourcebook 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 FEB 15 PY 2010 VL 135 IS 3 BP 118 EP 118 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 556QM UT WOS:000274606200222 ER PT J AU Guz, SS AF Guz, Savannah Schroll TI Polio 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 FEB 15 PY 2010 VL 135 IS 3 BP 118 EP 118 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 556QM UT WOS:000274606200226 ER PT J AU Guz, SS AF Guz, Savannah Schroll TI Praeger Handbook of Asian American Health: Notice and Take Action 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 FEB 15 PY 2010 VL 135 IS 3 BP 118 EP 118 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 556QM UT WOS:000274606200224 ER PT J AU Westmoquette, MS Slavin, JD Smith, LJ Gallagher, JS AF Westmoquette, M. S. Slavin, J. D. Smith, L. J. Gallagher, J. S., III TI VLT/FLAMES-ARGUS observations of stellar wind-ISM cloud interactions in NGC 6357 star SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE H ii regions; ISM: individual: NGC 6357; ISM: kinematics and dynamics ID TURBULENT MIXING LAYERS; H-II-REGION; STAR-FORMATION; INTERSTELLAR-MEDIUM; GALACTIC OUTFLOW; ELEPHANT TRUNKS; LINE-PROFILES; ORION NEBULA; HII-REGIONS; YOUNG STARS AB We present optical/near-IR integral field unit observations of a gas pillar in the Galactic H ii region NGC 6357 containing the young open star cluster Pismis 24. These observations have allowed us to examine in detail the gas conditions of the strong wind-clump interactions taking place on its surface. By accurately decomposing the H alpha line profile, we identify the presence of a narrow (similar to 20 km s-1) and broad (50-150 km s-1) component, both of which we can associate with the pillar and its surroundings. Furthermore, the broadest broad component widths are found in a region that follows the shape of the eastern pillar edge. These connections have allowed us to firmly associate the broad component with emission from ionized gas within turbulent mixing layers on the pillar's surface set up by the shear flows of the winds from the O stars in the cluster. We discuss the implications of our findings in terms of the broad emission-line component that is increasingly found in extragalactic starburst environments. Although the broad linewidths found here are narrower, we conclude that the mechanisms producing both must be the same. The difference in linewidths may result from the lower total mechanical wind energy produced by the O stars in Pismis 24 compared to that from a typical young massive star cluster found in a starburst galaxy. The pillar's edge is also clearly defined by dense (less than or similar to 5000 cm-3), hot (greater than or similar to 20 000 K) and excited (via the [N ii]/H alpha and [S ii]/H alpha ratios) gas conditions, implying the presence of a D-type ionization front propagating into the pillar surface. Although there must be both photoevaporation outflows produced by the ionization front and mass loss through mechanical ablation, we see no evidence for any significant bulk gas motions on or around the pillar. We postulate that the evaporated/ablated gas must be rapidly heated before being entrained. C1 [Westmoquette, M. S.; Smith, L. J.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Slavin, J. D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Smith, L. J.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Smith, L. J.] European Space Agcy, Res & Sci Support Dept, Baltimore, MD 21218 USA. [Gallagher, J. S., III] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. RP Westmoquette, MS (reprint author), UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England. EM msw@star.ucl.ac.uk FU National Science Foundation [AST-0708967] FX We thank Mark Gieles for his help in preparing and executing the observations. MSW would also like to thank Matt Redman and Mike Barlow for their careful reading of earlier versions of the manuscript and useful discussions regarding the nature of the observed wind-clump interactions. JSG's research was partially funded by the National Science Foundation through grant AST-0708967 to the University of Wisconsin-Madison. NR 48 TC 6 Z9 6 U1 0 U2 2 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 FEB 11 PY 2010 VL 402 IS 1 BP 152 EP 160 DI 10.1111/j.1365-2966.2009.15912.x PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 554SA UT WOS:000274453500013 ER PT J AU Maurer, JI Mazzali, PA Deng, J Filippenko, AV Hamuy, M Kirshner, RP Matheson, T Modjaz, M Pian, E Stritzinger, M Taubenberger, S Valenti, S AF Maurer, J. I. Mazzali, P. A. Deng, J. Filippenko, A. V. Hamuy, M. Kirshner, R. P. Matheson, T. Modjaz, M. Pian, E. Stritzinger, M. Taubenberger, S. Valenti, S. TI Characteristic velocities of stripped-envelope core-collapse supernova cores star SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE line: profiles; radiative transfer; supernovae: general ID GAMMA-RAY BURST; SN 1998BW; NEBULAR SPECTRA; IC SUPERNOVAE; NEUTRON-STAR; X-RAY; OPTICAL SPECTROSCOPY; IB/C SUPERNOVAE; IA SUPERNOVAE; LIGHT-CURVE AB The velocity of the inner ejecta of stripped-envelope core-collapse supernovae (CC-SNe) is studied by means of an analysis of their nebular spectra. Stripped-envelope CC-SNe are the result of the explosion of bare cores of massive stars (>= 8 M(circle dot)), and their late-time spectra are typically dominated by a strong [O i] lambda lambda 6300, 6363 emission line produced by the innermost, slow-moving ejecta which are not visible at earlier times as they are located below the photosphere. A characteristic velocity of the inner ejecta is obtained for a sample of 56 stripped-envelope CC-SNe of different spectral types (IIb, Ib, Ic) using direct measurements of the linewidth as well as spectral fitting. For most SNe, this value shows a small scatter around 4500 km s-1. Observations (< 100 d) of stripped-envelope CC-SNe have revealed a subclass of very energetic SNe, termed broad-lined SNe (BL-SNe) or hypernovae, which are characterized by broad absorption lines in the early-time spectra, indicative of outer ejecta moving at very high velocity (v >= 0.1c). SNe identified as BL in the early phase show large variations of core velocities at late phases, with some having much higher and some having similar velocities with respect to regular CC-SNe. This might indicate asphericity of the inner ejecta of BL-SNe, a possibility we investigate using synthetic three-dimensional nebular spectra. C1 [Maurer, J. I.; Mazzali, P. A.; Taubenberger, S.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Mazzali, P. A.] Scuola Normale Super Pisa, I-56126 Pisa, Italy. [Mazzali, P. A.] Natl Inst Astrophys OAPd, I-35122 Padua, Italy. [Deng, J.] CAS, Natl Astron Observ, Beijing 1000012, Peoples R China. [Filippenko, A. V.; Modjaz, M.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Hamuy, M.] Univ Chile, Dept Astron, Santiago, Chile. [Kirshner, R. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Matheson, T.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Pian, E.] Trieste Astron Observ, INAF, I-34143 Trieste, Italy. [Pian, E.; Valenti, S.] European So Observ, D-85748 Garching, Germany. [Stritzinger, M.] Carnegie Observ, Las Campanas Observ, La Serena, Chile. [Stritzinger, M.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen O, Denmark. RP Maurer, JI (reprint author), Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85741 Garching, Germany. EM maurer@mpa-garching.mpg.de RI Hamuy, Mario/G-7541-2016; OI Pian, Elena/0000-0001-8646-4858 FU European Southern Observatory telescopes [081.D-0173(A), 082.D-0292(A)]; Gemini Observatory; Association of Universities for Research in Astronomy, Inc.; National Science Foundation; Science and Technology Facilities Council (United Kingdom); National Research Council (Canada); CONICYT; Australian Research Council (Australia); Ministerio da Ciencia e Tecnologia (Brazil); Ministerio de Ciencia, Tecnologia e Innovacion Productiva (Argentina); NSF [AST-0607485, AST-0908886]; TABASGO Foundation; Fondecyt [1060808]; Millennium Center for Supernova Science [P06-045-F]; Centro de Astrofisica FONDAP [15010003]; Center of Excellence in Astrophysics and Associated Technologies [PFB 06]; NSFC [10673014]; National Basic Research Program of China [2009CB824800] FX This paper presents new observations made with the following facilities: the European Southern Observatory telescopes (Chile) obtained from the ESO/ST-ECF Science Archive Facility (Prog ID. 081.D-0173(A), 082.D-0292(A)) and the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the National Science Foundation on behalf of the Gemini partnership: the NSF (United States), the Science and Technology Facilities Council (United Kingdom), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministerio da Ciencia e Tecnologia (Brazil) and Ministerio de Ciencia, Tecnologia e Innovacion Productiva (Argentina). AVF's supernova research has been funded by NSF grants AST-0607485 and AST-0908886, as well as by the TABASGO Foundation. MH acknowledges funding from Fondecyt grant 1060808, the Millennium Center for Supernova Science through grant P06-045-F, Centro de Astrofisica FONDAP 15010003, and from Center of Excellence in Astrophysics and Associated Technologies (PFB 06). JD's supernova research has been funded by the NSFC (Grant No. 10673014) and by the National Basic Research Program of China (Grant No. 2009CB824800). NR 95 TC 24 Z9 24 U1 0 U2 3 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 FEB 11 PY 2010 VL 402 IS 1 BP 161 EP 172 DI 10.1111/j.1365-2966.2009.15905.x PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 554SA UT WOS:000274453500014 ER PT J AU Sanders, JS Fabian, AC Smith, RK Peterson, JR AF Sanders, J. S. Fabian, A. C. Smith, R. K. Peterson, J. R. TI A direct limit on the turbulent velocity of the intracluster medium in the core of Abell 1835 from XMM-Newton SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: clusters: individual: Abell 1835; cooling flows; intergalactic medium; X-rays: galaxies ID BRIGHTEST CLUSTER SAMPLE; COOLING FLOW CLUSTERS; X-RAY; GALAXY CLUSTERS; PERSEUS CLUSTER; GAS MOTIONS; MOLECULAR GAS; SPECTROSCOPY; CONSTRAINTS; PROFILES AB We examine deep XMM-Newton Reflection Grating Spectrometer observations of the X-ray luminous galaxy cluster A1835. For the first time in a galaxy cluster, we place direct limits on turbulent broadening of the emission lines. This is possible because the coolest X-ray emitting gas in the cluster, which is responsible for the lines, occupies a small region within the core. The most conservative determination of the 90 per cent upper limit on line-of-sight, non-thermal, velocity broadening is 274 km s(-1), measured from the emission lines originating within 30 kpc radius. The ratio of turbulent to thermal energy density in the core is therefore less than 13 per cent. There are no emission lines in the spectrum showing evidence for gas below similar to 3.5 keV. We examine the quantity of gas as a function of temperature and place a limit of 140M(circle dot) yr(-1) (90 per cent) for gas cooling radiatively below 3.85 keV. C1 [Sanders, J. S.; Fabian, A. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Smith, R. K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Peterson, J. R.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. RP Sanders, JS (reprint author), Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. EM jss@ast.cam.ac.uk OI Sanders, Jeremy/0000-0003-2189-4501 FU Royal Society; NASA [NNX08AX45G] FX ACF thanks the Royal Society for support. JRP is supported by NASA grant # NNX08AX45G. We thank Helen Russell for providing the Chandra spectra of this cluster and an anonymous referee for helpful comments. NR 35 TC 50 Z9 50 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 FEB 11 PY 2010 VL 402 IS 1 BP L11 EP L15 DI 10.1111/j.1745-3933.2009.00789.x PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 554SA UT WOS:000274453500061 ER PT J AU Christiansen, JL Ballard, S Charbonneau, D Madhusudhan, N Seager, S Holman, MJ Wellnitz, DD Deming, D A'Hearn, MF AF Christiansen, Jessie L. Ballard, Sarah Charbonneau, David Madhusudhan, Nikku Seager, Sara Holman, Matthew J. Wellnitz, Dennis D. Deming, Drake A'Hearn, Michael F. CA EPOXI Team TI STUDYING THE ATMOSPHERE OF THE EXOPLANET HAT-P-7b VIA SECONDARY ECLIPSE MEASUREMENTS WITH EPOXI, SPITZER, AND KEPLER SO ASTROPHYSICAL JOURNAL LA English DT Article DE eclipses; planetary systems; stars: individual (HAT-P-7) ID COLLISION-INDUCED ABSORPTION; INFRARED-EMISSION SPECTRUM; LIGHT-CURVE PROJECT; THERMAL EMISSION; TEMPERATURE INVERSION; EXTRASOLAR PLANET; SPACE-TELESCOPE; GIANT PLANETS; HOT JUPITERS; ARRAY CAMERA AB The highly irradiated transiting exoplanet, HAT-P-7b, currently provides one of the best opportunities for studying planetary emission in the optical and infrared wavelengths. We observe six near-consecutive secondary eclipses of HAT-P-7b at optical wavelengths with the EPOXI spacecraft. We place an upper limit on the relative eclipse depth of 0.055% (95% confidence). We also analyze Spitzer observations of the same target in the infrared, obtaining secondary eclipse depths of 0.098 +/- 0.017%, 0.159%+/- 0.022%, 0.245%+/- 0.031%, and 0.225%+/- 0.052% in the 3.6, 4.5, 5.8, and 8.0 mu m IRAC bands, respectively. We combine these measurements with the recently published Kepler secondary eclipse measurement and generate atmospheric models for the dayside of the planet that are consistent with both the optical and infrared measurements. The data are best fit by models with a temperature inversion, as expected from the high incident flux. The models predict a low optical albedo of less than or similar to 0.13, with subsolar abundances of Na, K, TiO, and VO. We also find that the best-fitting models predict that 10% of the absorbed stellar flux is redistributed to the nightside of the planet, which is qualitatively consistent with the inefficient day-night redistribution apparent in the Kepler phase curve. Models without thermal inversions fit the data only at the 1.25s level, and also require an overabundance of methane, which is not expected in the very hot atmosphere of HAT-P-7b. We also analyze the eight transits of HAT-P-7b present in the EPOXI data set and improve the constraints on the system parameters, finding a period of P = 2.2047308 +/- 0.0000025 days, a stellar radius of R(star) = 1.824 +/- 0.089 R(circle dot), a planetary radius of R(p) = 1.342 +/- 0.068 R(Jup), and an inclination of i = 85.7(-2.2)(+3.5) deg. C1 [Christiansen, Jessie L.; Ballard, Sarah; Charbonneau, David; Holman, Matthew J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Madhusudhan, Nikku; Seager, Sara] MIT, Cambridge, MA 02159 USA. [Wellnitz, Dennis D.; Deming, Drake; A'Hearn, Michael F.] Univ Maryland, College Pk, MD 20742 USA. RP Christiansen, JL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jchristi@cfa.harvard.edu RI Wellnitz, Dennis/B-4080-2012; OI Charbonneau, David/0000-0002-9003-484X FU National Aeronautics and Space Administration's Discovery Program [NNX08AB64A, NNX08AD05A]; NASA FX Support for this work was provided by the EPOXI Project of the National Aeronautics and Space Administration's Discovery Program via funding to the Goddard Space Flight Center, and to Harvard University via Cooperative Agreement NNX08AB64A, and to the Smithsonian Astrophysical Observatory via Cooperative Agreement NNX08AD05A. This work is also based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract to NASA. The authors acknowledge and are grateful for the use of publicly available transit modeling routines by Eric Agol and Kaisey Mandel, and also the Levenberg-Marquardt least-squares minimization routine MPFITFUN by Craig Markwardt. The authors also thank H. Knutson and F. Fressin for several useful discussions about Spitzer data analysis. NR 39 TC 54 Z9 55 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 FEB 10 PY 2010 VL 710 IS 1 BP 97 EP 104 DI 10.1088/0004-637X/710/1/97 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 546YH UT WOS:000273850800010 ER PT J AU Migliari, S Tomsick, JA Miller-Jones, JCA Heinz, S Hynes, RI Fender, RP Gallo, E Jonker, PG Maccarone, TJ AF Migliari, S. Tomsick, J. A. Miller-Jones, J. C. A. Heinz, S. Hynes, R. I. Fender, R. P. Gallo, E. Jonker, P. G. Maccarone, T. J. TI THE COMPLETE SPECTRUM OF THE NEUTRON STAR X-RAY BINARY 4U 0614+091 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; infrared: general; ISM: jets and outflows; X-rays: binaries ID MILLISECOND PULSAR SAX-J1808.4-3658; ACCRETING BLACK-HOLES; SYNCHROTRON EMISSION; DOMINATED ACCRETION; RXTE OBSERVATIONS; EVENT HORIZONS; GRS 1915+105; COMPACT JET; CYGNUS X-1; OUTBURST AB We observed the neutron star (NS) ultra-compact X-ray binary 4U 0614+091 quasi-simultaneously in the radio band (Very Large Array), mid-infrared (IR)/IR (Spitzer/Multiband Imaging Photometer for Spitzer and Infrared Array Camera), near-IR/optical (Small and Moderate Aperture Research Telescope System), optical-UV (Swift/UV-Optical Telescope), soft and hard X-rays (Swift/X-ray Telescope and Rossi-X-ray Timing Explorer). The source was steadily in its "hard state." We detected the source in the whole range, for the first time in the radio band at 4.86 and 8.46 GHz and in the mid-IR at 24 mu m, up to 100 keV. The optically thick synchrotron spectrum of the jet is consistent with being flat from the radio to the mid-IR band. The flat jet spectrum breaks in the range similar to(1-4) x 10(13) Hz to an optically thin power-law synchrotron spectrum with spectral index similar to -0.5. These observations allow us to estimate a lower limit on the jet radiative power of similar to 3 x 10(32) erg s(-1) and a total jet power L(J) similar to 10(34)mu(-1)(0.05) E(c)(0.53) erg s(-1) (where E(c) is the high-energy cutoff of the synchrotron spectrum in eV and mu(0.05) is the radiative efficiency in units of 0.05). The contemporaneous detection of the optically thin part of the compact jet and the X-ray tail above 30 keV allows us to assess the contribution of the jet to the hard X-ray tail by synchrotron self-Compton (SSC) processes. We conclude that, for realistic jet size, boosting, viewing angle, and energy partition, the SSC emission alone, from the post-shock, accelerated, non-thermal population in the jet, is not a viable mechanism to explain the observed hard X-ray tail of the NS 4U 0614+091. C1 [Migliari, S.] European Space Astron Ctr, E-28691 Madrid, Spain. [Migliari, S.] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. [Tomsick, J. A.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Miller-Jones, J. C. A.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Heinz, S.] Univ Wisconsin, Dept Astron, Madison, WI 53593 USA. [Hynes, R. I.] Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA 70803 USA. [Fender, R. P.; Maccarone, T. J.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Jonker, P. G.] Netherlands Inst Space Res, SRON, NL-3584 CA Utrecht, Netherlands. [Gallo, E.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Jonker, P. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Migliari, S (reprint author), European Space Astron Ctr, Apartado POB 78, E-28691 Madrid, Spain. RI Miller-Jones, James/B-2411-2013; OI Miller-Jones, James/0000-0003-3124-2814; Heinz, Sebastian/0000-0002-8433-8652 FU Space Telescope Science Institute [HST-HF-01218.01-A]; NASA [NAS5-26555]; Associated Universities, Inc; Spitzer [1289781, 1321162] FX M. thanks Sera Markoff for uncountable discussions and Erik Kuulkers also for sharing the results of his work before publication. S. M. is an ESA Fellow. J. M. J. is a Jansky Fellow. E. G. is a Hubble Fellow, supported through Postdoctoral Fellowship grant no. HST-HF-01218.01-A from the Space Telescope Science Institute, which is operated by AURA Inc., under NASA contract NAS5-26555. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. 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. S. M. was partially supported by Spitzer grant 1289781. J. A. T. was partially supported by Spitzer grant 1321162. NR 72 TC 39 Z9 39 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 FEB 10 PY 2010 VL 710 IS 1 BP 117 EP 124 DI 10.1088/0004-637X/710/1/117 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 546YH UT WOS:000273850800013 ER PT J AU Boroson, B Vrtilek, SD AF Boroson, Bram Vrtilek, Saeqa Dil TI X-RAY VARIATIONS AT THE ORBITAL PERIOD FROM CYGNUS X-1 IN THE HIGH/SOFT STATE SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: individual (Cygnus X-1); X-rays: binaries ID BLACK-HOLE CANDIDATES; TIME-SERIES ANALYSIS; TIMING EXPLORER; STELLAR WINDS; LONG-TERM; 226868=CYGNUS X-1; MASS; VARIABILITY; BINARIES; ULTRAVIOLET AB Orbital variability has been found in the X-ray hardness of the black hole candidate Cygnus X-1 during the soft/high X-ray state using light curves provided by the Rossi X-ray Timing Explorer's All-Sky Monitor. We are able to set broad limits on how the mass-loss rate and X-ray luminosity vary between the hard and soft states. The folded light curve shows diminished flux in the soft X-ray band at phi = 0 ( defined as the time of the superior conjunction of the X-ray source). Models of the orbital variability provide slightly superior fits when the absorbing gas is concentrated in neutral clumps and better explain the strong variability in hardness. In combination with the previously established hard/low state dips, our observations give a lower limit to the mass-loss rate in the soft state ((M) over dot < 2 x 10(-6) M(circle dot) yr(-1)) than the limit in the hard state ((M) over dot < 4 x 10(-6) M(circle dot) yr(-1)). Without a change in the wind structure between X-ray states, the greater mass-loss rate during the low/hard state would be inconsistent with the increased flaring seen during the high-soft state. C1 [Boroson, Bram; Vrtilek, Saeqa Dil] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Boroson, B (reprint author), Smithsonian Astrophys Observ, Mail Stop 83, Cambridge, MA 02138 USA. EM bboroson@cfa.harvard.edu; svrtilek@cfa.harvard.edu NR 49 TC 5 Z9 5 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 FEB 10 PY 2010 VL 710 IS 1 BP 197 EP 206 DI 10.1088/0004-637X/710/1/197 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 546YH UT WOS:000273850800019 ER PT J AU Covington, MD Kassin, SA Dutton, AA Weiner, BJ Cox, TJ Jonsson, P Primack, JR Faber, SM Koo, DC AF Covington, Matthew D. Kassin, Susan A. Dutton, Aaron A. Weiner, Benjamin J. Cox, Thomas J. Jonsson, Patrik Primack, Joel R. Faber, Sandra M. Koo, David C. TI EVOLUTION OF THE STELLAR MASS TULLY-FISHER RELATION IN DISK GALAXY MERGER SIMULATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: formation; galaxies: interactions; galaxies: kinematics and dynamics ID INTEGRAL FIELD SPECTROSCOPY; DIGITAL SKY SURVEY; ELLIPTIC GALAXIES; SCALING RELATIONS; DARK-MATTER; COSMOLOGICAL SIMULATIONS; INTERACTING GALAXIES; FUNDAMENTAL PLANE; MAJOR MERGERS; GAS CLOUDS AB There is a large observational scatter toward low velocities in the stellar mass Tully-Fisher (TF) relation if disturbed and compact objects are included. However, this scatter can be eliminated if one replaces rotation velocity with S(0.5), a quantity that includes a velocity dispersion term added in quadrature with the rotation velocity. In this work, we use a large suite of hydrodynamic N-body galaxy merger simulations to explore a possible mechanism for creating the observed relations. Using mock observations of the simulations, we test for the presence of observational effects and explore the relationship between S(0.5) and intrinsic properties of the galaxies. We find that galaxy mergers can explain the scatter in the TF as well as the tight S(0.5)-stellar mass relation. Furthermore, S(0.5) is correlated with the total central mass of a galaxy, including contributions due to dark matter. C1 [Covington, Matthew D.; Primack, Joel R.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Kassin, Susan A.] Univ Oxford, Subdept Astrophys, Oxford OX1 3RH, England. [Dutton, Aaron A.; Faber, Sandra M.; Koo, David C.] Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA. [Dutton, Aaron A.; Faber, Sandra M.; Koo, David C.] Univ Calif Santa Cruz, Dept Astron, Santa Cruz, CA 95064 USA. [Weiner, Benjamin J.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Cox, Thomas J.] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. [Covington, Matthew D.; Jonsson, Patrik] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. RP Covington, MD (reprint author), Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. EM covin039@umn.edu; s.kassin1@physics.ox.ac.uk RI Covington, Matthew/C-7622-2011; OI Covington, Matthew/0000-0003-4044-7387; Weiner, Benjamin/0000-0001-6065-7483 FU NASA ATP [NNX07AG94G]; UCSC Physics Department; UCSC UARC-ARP; NSF [AST-0507483, AST-0808133, HST GO-10532.02-A, HST AR-10965.02-A, HST GO-11206.02-A] FX M. D. C. acknowledges support from NASA ATP grant NNX07AG94G, the UCSC Physics Department, and a UCSC UARC-ARP grant. J.R.P. was supported by NASA ATP grant NNX07AG94G. Simulations analyzed here were carried out at NERSC, NASA's Columbia supercomputer, and UCSC computer clusters. S. A. K., A. A. D., S. M. F., and D. C. K. were supported by NSF grants AST-0507483 and AST-0808133, and grants HST GO-10532.02-A, HST AR-10965.02-A, and HST GO-11206.02-A. NR 65 TC 19 Z9 19 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 FEB 10 PY 2010 VL 710 IS 1 BP 279 EP 288 DI 10.1088/0004-637X/710/1/279 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 546YH UT WOS:000273850800026 ER PT J AU Temim, T Slane, P Reynolds, SP Raymond, JC Borkowski, KJ AF Temim, Tea Slane, Patrick Reynolds, Stephen P. Raymond, John C. Borkowski, Kazimierz J. TI DEEP CHANDRA OBSERVATIONS OF THE CRAB-LIKE PULSAR WIND NEBULA G54.1+0.3 AND SPITZER SPECTROSCOPY OF THE ASSOCIATED INFRARED SHELL SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; infrared: general; ISM: supernova remnants; pulsars: individual (PSR J1930+1852); X-rays: general ID SUPERNOVA REMNANT G54.1+0.3; RICH PROTOPLANETARY NEBULAE; ACTIVE GALACTIC NUCLEI; 21 MICRON FEATURE; SPACE-TELESCOPE; INTERSTELLAR-MEDIUM; MU-M; DUST; EMISSION; STARS AB G54.1+0.3 is a young pulsar wind nebula (PWN), closely resembling the Crab, for which no thermal shell emission has been detected in X-rays. Recent Spitzer observations revealed an infrared (IR) shell containing a dozen point sources arranged in a ring-like structure, previously proposed to be young stellar objects. An extended knot of emission located in the NW part of the shell appears to be aligned with the pulsar's X-ray jet, suggesting a possible interaction with the shell material. Surprisingly, the IR spectrum of the knot resembles the spectrum of freshly formed dust in Cas A, and is dominated by an unidentified dust emission feature at 21 mu m. The spectra of the shell also contain various emission lines and show that some are significantly broadened, suggesting that they originate in rapidly expanding supernova (SN) ejecta. We present the first evidence that the PWN is driving shocks into expanding SN ejecta and we propose an alternative explanation for the origin of the IR emission in which the shell is composed entirely of SN ejecta. In this scenario, the freshly formed SN dust is being heated by early-type stars belonging to a cluster in which the SN exploded. Simple dust models show that this interpretation can give rise to the observed shell emission and the IR point sources. C1 [Temim, Tea; Slane, Patrick; Raymond, John C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Temim, Tea] Univ Minnesota, Sch Phys & Astron, Dept Astron, Minneapolis, MN 55455 USA. [Reynolds, Stephen P.; Borkowski, Kazimierz J.] N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA. RP Temim, T (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Temim, Tea/0000-0001-7380-3144 FU NASA [NAS8-03060]; CXC [GO8-9064X] FX P.O.S. acknowledges partial support from NASA contract NAS8-03060. T. T. acknowledges partial support from CXC grant GO8-9064X. We thank Alexey Vikhlinin for the ACIS data reduction script, Joe Hora for useful discussion on the 21 mu m feature in PPNe, Achim Tappe for tips on CUBISM line intensity maps, Charles Lada for discussion on young stars, Anne Hofmeister for nano-SiC absorbance data, and Jeonghee Rho for the discussion on the 21 mu m feature in Cas A. 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. 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. SMART was developed by the IRS Team at Cornell University and is available through the Spitzer Science Center at Caltech. NR 46 TC 18 Z9 19 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 FEB 10 PY 2010 VL 710 IS 1 BP 309 EP 324 DI 10.1088/0004-637X/710/1/309 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 546YH UT WOS:000273850800028 ER PT J AU Krongold, Y Elvis, M Andrade-Velazquez, M Nicastro, F Mathur, S Reeves, JN Brickhouse, NS Binette, L Jimenez-Bailon, E Grupe, D Liu, Y McHardy, IM Minezaki, T Yoshii, Y Wilkes, B AF Krongold, Y. Elvis, M. Andrade-Velazquez, M. Nicastro, F. Mathur, S. Reeves, J. N. Brickhouse, N. S. Binette, L. Jimenez-Bailon, E. Grupe, D. Liu, Y. McHardy, I. M. Minezaki, T. Yoshii, Y. Wilkes, B. TI SUZAKU MONITORING OF THE SEYFERT 1 GALAXY NGC 5548: WARM ABSORBER LOCATION AND ITS IMPLICATION FOR COSMIC FEEDBACK SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: individual (NGC 5548); galaxies: Seyfert; quasars: absorption lines ID ACTIVE GALACTIC NUCLEI; REFLECTION GRATING SPECTROMETER; BROAD-LINE REGION; X-RAY/UV CAMPAIGN; XMM-NEWTON VIEW; BLACK-HOLES; IONIZED-GAS; OUTFLOW; NGC-3783; QUASARS AB We present a 2 month Suzaku X-ray monitoring of the Seyfert 1 galaxy NGC 5548. The campaign consists of seven observations (with exposure time of similar to 30 ks each), separated by similar to 1 week. This paper focus on the X-ray Imaging Spectrometer data of NGC 5548. We analyze the response in the opacity of the gas that forms the well-known ionized absorber in this source for ionizing flux variations. Despite variations by a factor of similar to 4 in the impinging continuum, the soft X-ray spectra of the source show little spectral variations, suggesting no response from the ionized absorber. A detailed time modeling of the spectra confirms the lack of opacity variations for an absorbing component with high ionization (U-X approximate to -0.85), and high outflow velocity (v(out) approximate to 1040 km s(-1)), as the ionization parameter was found to be consistent with a constant value during the whole campaign. Instead, the models suggest that the ionization parameter of a low ionization (U-X approximate to -2.8), low velocity (v(out) approximate to 590 km s(-1)) absorbing component might be changing linearly with the ionizing flux, as expected for gas in photoionization equilibrium. However, given the lack of spectral variations among observations, we consider the variations in this component as tentative. Using the lack of variations, we set an upper limit of n(e) < 2.0 x 10(7) cm(-3) for the electron density of the gas forming the high ionization, high velocity component. This implies a large distance from the continuum source (R > 0.033 pc; R > 5000 R-S). If the variations in the low ionization, low velocity component are real, they imply n(e) > 9.8 x 10(4) cm(-3) and R < 3 pc. We discuss our results in terms of two different scenarios: a large-scale outflow originating in the inner parts of the accretion disk, or a thermally driven wind originating much farther out. Given the large distance of the wind, the implied mass outflow rate is also large ((M) over dot(w) > 0.08 (M) over dot(accr); the mass outflow is dominated by the high ionization component). The associated total kinetic energy deployed by the wind in the host galaxy (> 1.2 x 10(56) erg) can be enough to disrupt the interstellar medium, possibly quenching or regulating large-scale star formation. However, the total mass and energy ejected by the wind may still be lower than the one required for cosmic feedback, even when extrapolated to quasar luminosities. Such feedback would require that we are observing the wind before it is fully accelerated. C1 [Krongold, Y.; Andrade-Velazquez, M.; Binette, L.; Jimenez-Bailon, E.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. [Elvis, M.; Nicastro, F.; Brickhouse, N. S.; Liu, Y.; Wilkes, B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Nicastro, F.] Osserv Astron Roma, INAF, Rome, Italy. [Nicastro, F.] Univ Crete, FORTH, Khania, Greece. [Mathur, S.] Ohio State Univ, Columbus, OH 43210 USA. [Reeves, J. N.] Keele Univ, Sch Phys & Geog Sci, Astrophys Grp, Keele ST5 8EH, Staffs, England. [Grupe, D.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [McHardy, I. M.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Minezaki, T.; Yoshii, Y.] Univ Tokyo, Inst Astron, Sch Sci, Tokyo 1810015, Japan. RP Krongold, Y (reprint author), Univ Nacl Autonoma Mexico, Inst Astron, Apartado Postal 70-264, Mexico City 04510, DF, Mexico. RI XRAY, SUZAKU/A-1808-2009; OI Brickhouse, Nancy/0000-0002-8704-4473; Nicastro, Fabrizio/0000-0002-6896-1364; Wilkes, Belinda/0000-0003-1809-2364 FU UNAM PAPIIT [IN118905]; CONACyT [J-49594]; NASA, Chandra X-ray Center [NAS8-03060, NNX08AB81G] FX This work was supported by the UNAM PAPIIT grant IN118905 and the CONACyT grant J-49594. N. S. B. acknowledges support from NASA to the Chandra X-ray Center through NAS8-03060. This work was supported by NASA grant NNX08AB81G. NR 63 TC 15 Z9 15 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2010 VL 710 IS 1 BP 360 EP 371 DI 10.1088/0004-637X/710/1/360 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 546YH UT WOS:000273850800032 ER PT J AU Andrews, SM Czekala, I Wilner, DJ Espaillat, C Dullemond, CP Hughes, AM AF Andrews, Sean M. Czekala, Ian Wilner, D. J. Espaillat, Catherine Dullemond, C. P. Hughes, A. M. TI TRUNCATED DISKS IN TW Hya ASSOCIATION MULTIPLE STAR SYSTEMS SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: spectroscopic; binaries: visual; circumstellar matter; protoplanetary disks; stars: pre-main sequence ID SUBMILLIMETER CONTINUUM FLUX; ECCENTRIC STELLAR BINARIES; CIRCUMSTELLAR DUST DISKS; MAIN-SEQUENCE STARS; SOLAR-TYPE STARS; X-RAY-SPECTRUM; TAURI STARS; HYDRAE ASSOCIATION; HD 98800; YOUNG BINARIES AB We present high angular resolution (down to 0 ''.3 approximate to 13 AU in diameter) Submillimeter Array observations of the 880 mu m (340 GHz) thermal continuum emission from circumstellar dust disks in the nearby HD 98800 and Hen 3-600 multiple star systems. In both cases, the dust emission is resolved and localized around one stellar component-the HD 98800B and Hen 3-600A spectroscopic binaries-with no evidence for circum-system material. Using two-dimensional Monte Carlo radiative transfer calculations, we compare the Submillimeter Array interferometer visibilities and broadband spectral energy distributions with truncated disk models to empirically locate the inner and outer edges of both disks. The HD 98800B disk appears to be aligned with the spectroscopic binary orbit, is internally truncated at a radius of 3.5 AU, and extends to only 10-15 AU from the central stars. The Hen 3-600A disk is slightly larger, with an inner edge at similar to 1 AU and an outer radius of 15-25 AU. These inferred disk structures compare favorably with theoretical predictions of their truncation due to tidal interactions with the stellar companions. C1 [Czekala, Ian; Wilner, D. J.; Hughes, A. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Czekala, Ian] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Dullemond, C. P.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. EM sandrews@cfa.harvard.edu OI Dullemond, Cornelis/0000-0002-7078-5910; Czekala, Ian/0000-0002-1483-8811 FU Smithsonian Institute; Academia Sinica; NASA, Space Telescope Science Institute [HF-01203.01-A, NAS 5-26555, NNG05GI81G]; National Science Foundation (NSF) [0754568, 0901947]; Smithsonian Institution FX We are grateful to David Latham and Guillermo Torres for sharing their orbital expertise on these systems, and especially to Elise Furlan and the Spitzer GTO team lead by Dan Watson for kindly permitting the use of their calibrated IRS spectra. We thank the referee for an insightful review that helped improve the article. 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 Institute and the Academia Sinica. Support for this work was provided by NASA through Hubble Fellowship grant HF-01203.01-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. Partial support for I. C. was provided by the NSF REU and DOD ASSURE programs under NSF grant 0754568 and by the Smithsonian Institution. D. J. W. acknowledges support from NASA Origins grant NNG05GI81G. C. E. was supported by the National Science Foundation under award 0901947. NR 79 TC 30 Z9 30 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 FEB 10 PY 2010 VL 710 IS 1 BP 462 EP 469 DI 10.1088/0004-637X/710/1/462 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 546YH UT WOS:000273850800040 ER PT J AU Cranmer, SR AF Cranmer, Steven R. TI AN EFFICIENT APPROXIMATION OF THE CORONAL HEATING RATE FOR USE IN GLOBAL SUN-HELIOSPHERE SIMULATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE interplanetary medium; magnetohydrodynamics (MHD); solar wind; Sun: corona; turbulence; waves ID FAST SOLAR-WIND; WKB ALFVEN WAVES; DIFFERENTIAL ION FLOW; LOW-FREQUENCY WAVES; MAGNETOHYDRODYNAMIC TURBULENCE; MHD TURBULENCE; STELLAR ATMOSPHERES; MAGNETIC-FIELD; SPACE WEATHER; FLUX TUBES AB The origins of the hot solar corona and the supersonically expanding solar wind are still the subject of debate. A key obstacle in the way of producing realistic simulations of the Sun-heliosphere system is the lack of a physically motivated way of specifying the coronal heating rate. Recent one-dimensional models have been found to reproduce many observed features of the solar wind by assuming the energy comes from Alfven waves that are partially reflected, then dissipated by magnetohydrodynamic turbulence. However, the nonlocal physics of wave reflection has made it difficult to apply these processes to more sophisticated (three-dimensional) models. This paper presents a set of robust approximations to the solutions of the linear Alfven wave reflection equations. A key ingredient of the turbulent heating rate is the ratio of inward-to-outward wave power, and the approximations developed here allow this to be written explicitly in terms of local plasma properties at any given location. The coronal heating also depends on the frequency spectrum of Alfven waves in the open-field corona, which has not yet been measured directly. A model-based assumption is used here for the spectrum, but the results of future measurements can be incorporated easily. The resulting expression for the coronal heating rate is self-contained, computationally efficient, and applicable directly to global models of the corona and heliosphere. This paper tests and validates the approximations by comparing the results to exact solutions of the wave transport equations in several cases relevant to the fast and slow solar wind. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Cranmer, SR (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM scranmer@cfa.harvard.edu FU National Aeronautics and Space Administration ( NASA) [NNG04GE77G, NNX09AB27G] FX I gratefully acknowledge Adriaan van Ballegooijen, William Matthaeus, and Ofer Cohen for many valuable discussions, as well as Steve Tomczyk and Scott McIntosh for making available a tabulated version of their CoMP power spectrum. I also thank the anonymous referee for constructive suggestions that have improved this paper. This work was supported by the National Aeronautics and Space Administration ( NASA) under grants NNG04GE77G and NNX09AB27G to the Smithsonian Astrophysical Observatory. NR 99 TC 34 Z9 34 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2010 VL 710 IS 1 BP 676 EP 688 DI 10.1088/0004-637X/710/1/676 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 546YH UT WOS:000273850800052 ER PT J AU Garcia, MR Hextall, R Baganoff, FK Galache, J Melia, F Murray, SS Primini, FA Sjouwerman, LO Williams, B AF Garcia, Michael R. Hextall, Richard Baganoff, Frederick K. Galache, Jose Melia, Fulvio Murray, Stephen S. Primini, F. A. Sjouwerman, Lorant O. Williams, Ben TI X-RAY AND RADIO VARIABILITY OF M31*, THE ANDROMEDA GALAXY NUCLEAR SUPERMASSIVE BLACK HOLE SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; galaxies: individual (M31); galaxies: nuclei ID HUBBLE-SPACE-TELESCOPE; SAGITTARIUS-A-ASTERISK; ADVECTION-DOMINATED ACCRETION; GALACTIC-CENTER; CENTRAL REGION; POINT SOURCES; XMM-NEWTON; CHANDRA OBSERVATIONS; UNRESOLVED EMISSION; M31 BULGE AB We confirm our earlier tentative detection of M31* in X-rays and measure its light curve and spectrum. Observations in 2004-2005 find M31* rather quiescent in the X-ray and radio. However, X-ray observations in 2006-2007 show M31* to be highly variable at times. A separate variable X-ray source is found near P1, the brighter of the two optical nuclei. The apparent angular Bondi radius of M31* is the largest of any black hole and large enough to be well resolved with Chandra. The diffuse emission within this Bondi radius is found to have an X-ray temperature similar to 0.3 keV and density 0.1 cm(-3), indistinguishable from the hot gas in the surrounding regions of the bulge given the statistics allowed by the current observations. The X-ray source at the location of M31* is consistent with a point source and a power-law spectrum with energy slope 0.9 +/- 0.2. Our identification of this X-ray source with M31* is based solely on positional coincidence. C1 [Garcia, Michael R.; Hextall, Richard; Galache, Jose; Murray, Stephen S.; Primini, F. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hextall, Richard] Univ Southampton, Dept Phys, Southampton SO9 5NH, Hants, England. [Baganoff, Frederick K.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02138 USA. [Melia, Fulvio] Univ Arizona, Dept Phys, Program Appl Math, Tucson, AZ 85721 USA. [Melia, Fulvio] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Sjouwerman, Lorant O.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Williams, Ben] Univ Washington, Dept Astron, Seattle, WA 98195 USA. RP Garcia, MR (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM garcia@head.cfa.harvard.edu OI Primini, Francis/0000-0002-6077-0643 FU Chandra grant [GO-6088A]; Chandra X-ray Center [NAS8-03060] FX This work was supported in part by Chandra grant GO-6088A and Chandra X-ray Center Contract NAS8-03060. NR 61 TC 23 Z9 23 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 FEB 10 PY 2010 VL 710 IS 1 BP 755 EP 763 DI 10.1088/0004-637X/710/1/755 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 546YH UT WOS:000273850800058 ER PT J AU Shi, H Zhao, JH Han, JL AF Shi, Hui Zhao, Jun-Hui Han, J. L. TI NATURE OF W51e2: MASSIVE CORES AT DIFFERENT PHASES OF STAR FORMATION SO ASTROPHYSICAL JOURNAL LA English DT Article DE HII regions; ISM: individual objects (W51e2); stars: formation ID HIGH-RESOLUTION OBSERVATIONS; H 2 REGIONS; RADIO-CONTINUUM; CIRCUMSTELLAR DISK; DYNAMICAL COLLAPSE; MAGNETIC-FIELDS; PROPER MOTIONS; FORMING REGION; DUST EMISSION; EVOLUTION AB We present high-resolution continuum images of the W51e2 complex processed from archival data of the Submillimeter Array (SMA) at 0.85 and 1.3 mm and the Very Large Array at 7 and 13 mm. We also made line images and profiles of W51e2 for three hydrogen radio recombination lines (RRLs; H26 alpha, H53 alpha, and H66 alpha) and absorption of two molecular lines of HCN(4-3) and CO(2-1). At least four distinct continuum components have been detected in the 3 '' region of W51e2 from the SMA continuum images at 0.85 and 1.3 mm with resolutions of 0.'' 3 x 0.'' 2 and 1.'' 4 x 0.'' 7, respectively. The west component, W51e2-W, coincides with the ultracompact HII region reported from previous radio observations. The H26 alpha line observation reveals an unresolved hyper-compact ionized core (< 0.'' 06 or < 310 AU) with a high electron temperature of 1.2x10(4) K, with the corresponding emission measure EM > 7 x 10(10) pc cm(-6) and the electron density N(e) > 7 x 10(6) cm(-3). The inferred Lyman continuum flux implies that the HII region W51e2-W requires a newly formed massive star, an O8 star or a cluster of B-type stars, to maintain the ionization. W51e2-E, the brightest component at 0.85 mm, is located 0.'' 9 east from the hyper-compact ionized core. It has a total mass of similar to 140 M(circle dot) according to our spectral energy distribution analysis and a large infall rate of > 1.3 x 10(-3) M(circle dot) yr(-1) inferred from the absorption of HCN. W51e2-E appears to be the accretion center in W51e2. Given the fact that no free-free emission and no RRLs have been detected, the massive core of W51e2-E appears to host one or more growing massive proto-stars. Located 2 '' northwest from W51e2-E, W51e2-NW is detected in the continuum emission at 0.85 and 1.3 mm. No continuum emission has been detected at lambda >= 7 mm. Along with the maser activities previously observed, our analysis suggests that W51e2-NW is at an earlier phase of star formation. W51e2-N is located 2 '' north of W51e2-E and has only been detected at 1.3 mm with a lower angular resolution (similar to 1 ''), suggesting that it is a primordial, massive gas clump in the W51e2 complex. 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, Jia20 Datun Rd, Beijing 100012, Peoples R China. EM shihui@nao.cas.cn; jzhao@cfa.harvard.edu; hjl@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 the referee for helpful comments, Dr. S.-L. Qin for providing help with the data reduction and analysis, and Professor Y.-F. Wu for helpful discussions. H. Shi and J.-L. Han 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 35 TC 16 Z9 16 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 FEB 10 PY 2010 VL 710 IS 1 BP 843 EP 852 DI 10.1088/0004-637X/710/1/843 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 546YH UT WOS:000273850800066 ER PT J AU Evans, DA Reeves, JN Hardcastle, MJ Kraft, RP Lee, JC Virani, SN AF Evans, D. A. Reeves, J. N. Hardcastle, M. J. Kraft, R. P. Lee, J. C. Virani, S. N. TI THE HARD X-RAY VIEW OF REFLECTION, ABSORPTION, AND THE DISK-JET CONNECTION IN THE RADIO-LOUD AGN 3C 33 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: individual (3C 33); galaxies: jets; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; SEYFERT-GALAXIES; CHANDRA-HETGS; IRON LINES; CYGNUS X-1; UNIFICATION; EMISSION; SAMPLE; SUZAKU; SPECTRUM AB We present results from Suzaku and Swift observations of the nearby radio galaxy 3C 33, and investigate the nature of absorption, reflection, and jet production in this source. We model the 0.5-100 keV nuclear continuum with a power law that is transmitted either through one or more layers of pc-scale neutral material, or through a modestly ionized pc-scale obscurer. The standard signatures of reflection from a neutral accretion disk are absent in 3C 33: there is no evidence of a relativistically blurred Fe K alpha emission line, and no Compton reflection hump above 10 keV. We find the upper limit to the neutral reflection fraction is R < 0.41 for an e-folding energy of 1 GeV. We observe a narrow, neutral Fe K alpha line, which is likely to originate at least 2000 R(s) from the black hole. We show that the weakness of reflection features in 3C 33 is consistent with two interpretations: either the inner accretion flow is highly ionized, or the black-hole spin configuration is retrograde with respect to the accreting material. C1 [Evans, D. A.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Evans, D. A.; Kraft, R. P.; Lee, J. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Reeves, J. N.] Keele Univ, Sch Phys & Geog Sci, Astrophys Grp, Keele ST5 5BG, Staffs, England. [Hardcastle, M. J.] Univ Hertfordshire, Sch Phys Astron & Math, Hatfield AL10 9AB, Herts, England. [Virani, S. N.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. RP Evans, DA (reprint author), MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. RI Hardcastle, Martin/E-2264-2012; XRAY, SUZAKU/A-1808-2009 OI Hardcastle, Martin/0000-0003-4223-1117; FU NASA [NNX08AI59G, NAS8-03060]; Royal Society for a Research Fellowship; ESA Member States FX We wish to thank the anonymous referee for comments which greatly improved this paper. D.A.E. gratefully acknowledges financial support for this work from NASA under grant number NNX08AI59G. M.J.H. thanks the Royal Society for a Research Fellowship. This research has made use of data obtained from the Suzaku satellite, a collaborative mission between the space agencies of Japan (JAXA) and the USA (NASA). This work has also made use of the Chandra X-ray Observatory, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8-03060. This work is additionally based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. Finally, 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 NASA. NR 34 TC 10 Z9 10 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 FEB 10 PY 2010 VL 710 IS 1 BP 859 EP 868 DI 10.1088/0004-637X/710/1/859 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 546YH UT WOS:000273850800068 ER PT J AU Robitaille, TP Whitney, BA AF Robitaille, Thomas P. Whitney, Barbara A. TI THE PRESENT-DAY STAR FORMATION RATE OF THE MILKY WAY DETERMINED FROM SPITZER-DETECTED YOUNG STELLAR OBJECTS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE Galaxy: fundamental parameters; infrared: stars; stars: formation; stars: pre-main-sequence ID FORMING REGIONS; EVOLUTION; MODEL; EXTINCTION; GALAXIES; DUST; GLIMPSE; DISK AB We present initial results from a population synthesis model aimed at determining the star formation rate (SFR) of the Milky Way. We find that a total SFR of 0.68-1.45 M(circle dot) yr(-1) is able to reproduce the observed number of young stellar objects (YSOs) in the Spitzer/IRAC GLIMPSE survey of the Galactic plane, assuming simple prescriptions for the three-dimensional Galactic distributions of YSOs and interstellar dust, and using model spectral energy distributions to predict the brightness and color of the synthetic YSOs at different wavelengths. This is the first Galaxy-wide measurement derived from pre-main-sequence objects theme elves, rather than global observables such as the total radio continuum, Ha, or FIR flux. The value obtained is slightly lower than, but generally consistent with previously determined values. We will extend this method in the future to fit the brightness, color, and angular distribution of YSOs, and simultaneously make use of multiple surveys, to place constraints on the input assumptions, and reduce uncertainties in the SFR estimate. Ultimately, this will be one of the most accurate methods for determining the Galactic SFR, as it makes use of stars of all masses (limited only by sensitivity) rather than solely massive stars or indirect tracers of massive stars. C1 [Robitaille, Thomas P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Whitney, Barbara A.] Space Sci Inst, Boulder, CO 80301 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 through the Spitzer Space Telescope Fellowship; Theoretical Research; Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA FX We thank the anonymous referee for useful suggestions which helped improve this Letter. Support for this work was provided by NASA through the Spitzer Space Telescope Fellowship (T.R.) and Theoretical Research (T.R., B.W.) Programs, through a contract issued by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. NR 25 TC 121 Z9 121 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD FEB 10 PY 2010 VL 710 IS 1 BP L11 EP L15 DI 10.1088/2041-8205/710/l/L11 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 554MI UT WOS:000274438700003 ER PT J AU Tang, SM Grindlay, J Los, E Laycock, S AF Tang, Sumin Grindlay, Jonathan Los, Edward Laycock, Silas TI DASCH DISCOVERY OF LARGE AMPLITUDE similar to 10-100 YEAR VARIABILITY IN K GIANTS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE methods: data analysis; stars: evolution; stars: variables: general; techniques: photometric ID CORONAE-BOREALIS STARS; SOLAR-TYPE STARS; II H-LINE; BRANCH STARS; ROTATION; HEMISPHERE; PHOTOMETRY; CATALOG; DISK; SUN AB Here we present the discovery of three unusual long-term variables found in the Digital Access to a Sky Century at Harvard project, with similar to 1 mag variations in their light curves on similar to 10-100 year timescales. They are all spectroscopically identified as K2III giant stars, probably in the thick disk. Their light curves do not match those previously measured for known types of variable stars, or any theoretical model reported for red giants, and instead suggest a new dust formation mechanism or the first direct observation of "short" timescale evolution-driven variability. More theoretical work on the lithium flash near the red giant branch bump an I the helium shell ignition in the lower asymptotic giant branch, as well as long-term monitoring of K2III thick-disk stars is needed. C1 [Tang, Sumin; Grindlay, Jonathan; Los, Edward] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Laycock, Silas] Gemini Observ, Hilo, HI 96720 USA. RP Tang, SM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM stang@cfa.harvard.edu FU NSF [AST-0407380, AST-0909073] FX We are grateful to the anonymous referee for helpful comments and suggestions which significantly improved the manuscript. We thank Alison Doane, Jaime Pepper, Bob Simcoe, George Champine, and Doug Mink at CfA for their work on DASCH. We thank Lars Bildsten, Andrea Dupree, Geoffrey Clayton, Anna Frebel, Warren Brown, Perry Belind, and Peter Edmonds for enlightening and helpful discussion. S.T. thanks the FLWO staff for their hospitality during the course of this work, Mark Everret for reducing the Keplercarn data; and Nathalie Martimbeau, Susan Tokarz, and Bill Wyatt for help on the wavelength calibrations of FAST spectra. This research has made use of the WEBDA, GSC 2.3.2, and 2MASS catalogs, SIMBAD, HEASARC, and the AAVSO database. The DASCH project gratefully acknowledges support from NSF grants AST-0407380 and AST-0909073. NR 38 TC 9 Z9 9 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD FEB 10 PY 2010 VL 710 IS 1 BP L77 EP L81 DI 10.1088/2041-8205/710/1/L77 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 554MI UT WOS:000274438700017 ER PT J AU Laurance, SGW Laurance, WF Andrade, A Fearnside, PM Harms, KE Vicentini, A Luizao, RCC AF Laurance, Susan G. W. Laurance, William F. Andrade, Ana Fearnside, Philip M. Harms, Kyle E. Vicentini, Alberto Luizao, Regina C. C. TI Influence of soils and topography on Amazonian tree diversity: a landscape-scale study SO JOURNAL OF VEGETATION SCIENCE LA English DT Article DE Density dependence; Distributional ecology; Fisher's alpha; Permanent plots; Rare species; Soil chemistry; Soil texture; Soil water; Species diversity; Species richness; Topography; Tropical trees ID TROPICAL FORESTS; SPECIES-DIVERSITY; RAIN-FOREST; PATTERNS; COMMUNITIES; DENSITY; BRAZIL; DISTRIBUTIONS; PHOSPHORUS; HYPOTHESIS AB Question: How do soils and topography influence Amazonian tree diversity, a region with generally nutrient-starved soils but some of the biologically richest tree communities on Earth? Location: Central Amazonia, near Manaus, Brazil. Methods: We evaluated the influence of 14 soil and topographic features on species diversity of rain forest trees (>= 10 cm diameter at breast height), using data from 63 1-ha plots scattered over an area of similar to 400 km(2). Results: An ordination analysis identified three major edaphic gradients: (1) flatter areas had generally higher nutrient soils (higher clay content, carbon, nitrogen, phosphorus, pH and exchangeable bases, and lower aluminium saturation) than did slopes and gullies; (2) sandier soils had lower water storage (plant available water capacity), phosphorus and nitrogen; and (3) soil pH varied among sites. Gradient 2 was the strongest predictor of tree diversity (species richness and Fisher's alpha values), with diversity increasing with higher soil fertility and water availability. Gradient 2 was also the best predictor of the number of rare (singleton) species, which accounted on average for over half (56%) of all species in each plot. Conclusions: Although our plots invariably supported diverse tree communities (>= 225 species ha(-1)), the most species-rich sites (up to 310 species ha(-1)) were least constrained by soil water and phosphorus availability. Intriguingly, the numbers of rare and common species were not significantly correlated in our plots, and they responded differently to major soil and topographic gradients. For unknown reasons rare species were significantly more frequent in plots with many large trees. C1 [Laurance, Susan G. W.; Laurance, William F.] James Cook Univ, Sch Marine & Trop Biol, Cairs, Qld 4870, Australia. [Laurance, Susan G. W.; Laurance, William F.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Andrade, Ana] Natl Inst Amazonian Res INPA, Biol Dynam Forest Fragments Project, BR-69011970 Manaus, Amazonas, Brazil. [Andrade, Ana] Smithsonian Trop Res Inst, BR-69011970 Manaus, Amazonas, Brazil. [Fearnside, Philip M.; Vicentini, Alberto; Luizao, Regina C. C.] Natl Inst Amazonian Res INPA, Dept Ecol, BR-69011970 Manaus, Amazonas, Brazil. [Harms, Kyle E.] Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA. RP Laurance, SGW (reprint author), James Cook Univ, Sch Marine & Trop Biol, Cairs, Qld 4870, Australia. EM susan.laurance@jcu.edu.au; bill.laurance@jcu.edu.au; titina@inpa.gov.br; pmfearn@inpa.gov.br; kharms@lsu.edu; vicentini.beto@gmail.com; rccl@inpa.gov.br RI Laurance, William/B-2709-2012; Vicentini, Alberto/F-7479-2012; Fearnside, Philip/D-6559-2011; Servamb, Inct/K-3437-2013; Laurance, Susan/G-6021-2011 OI Vicentini, Alberto/0000-0002-5906-9358; Fearnside, Philip/0000-0003-3672-9082; Laurance, Susan/0000-0002-2831-2933 FU US National Science Foundation; Marisla Foundation; Conservation, Food and Health Foundation; BlueMoon Fund; NASA-LBA program; Smithsonian Institution FX We thank John Terborgh, Egbert Leigh, Ben Turner, Richard Condit, Phyllis Coley, Meelis Partel and an anonymous referee for many useful comments on the manuscript. Support was provided by the US National Science Foundation, Marisla Foundation, Conservation, Food and Health Foundation, BlueMoon Fund, NASA-LBA program and the Smithsonian Institution. This is publication number 550 in the technical series of the Biological Dynamics of Forest Fragments Project. NR 73 TC 30 Z9 32 U1 5 U2 55 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1100-9233 J9 J VEG SCI JI J. Veg. Sci. PD FEB 10 PY 2010 VL 21 IS 1 BP 96 EP 106 DI 10.1111/j.1654-1103.2009.01122.x PG 11 WC Plant Sciences; Ecology; Forestry SC Plant Sciences; Environmental Sciences & Ecology; Forestry GA 544OS UT WOS:000273668300010 ER PT J AU Bentlage, B Cartwright, P Yanagihara, AA Lewis, C Richards, GS Collins, AG AF Bentlage, Bastian Cartwright, Paulyn Yanagihara, Angel A. Lewis, Cheryl Richards, Gemma S. Collins, Allen G. TI Evolution of box jellyfish (Cnidaria: Cubozoa), a group of highly toxic invertebrates SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE Cubozoa; box jellyfish; Irukandji; systematics; biogeography; phylogeography ID CARYBDEA-SIVICKISI CNIDARIA; IRUKANDJI-SYNDROME; LIFE-CYCLE; SEA WASP; PARTIAL-PURIFICATION; FATAL ENVENOMATION; CHIRONEX-FLECKERI; PROTEIN TOXIN; HABU-KURAGE; VENOM AB Cubozoa (Cnidaria: Medusozoa) represents a small clade of approximately 50 described species, some of which cause serious human envenomations. Our understanding of the evolutionary history of Cubozoa has been limited by the lack of a sound phylogenetic hypothesis for the group. Here, we present a comprehensive cubozoan phylogeny based on ribosomal genes coding for near-complete nuclear 18S (small subunit) and 28S (large subunit) and partial mitochondrial 16S. We discuss the implications of this phylogeny for our understanding of cubozoan venom evolution, biogeography and life-history evolution. Our phylogenetic hypothesis suggests that: (i) the last common ancestor of Carybdeida probably possessed the mechanism(s) underlying Irukandji syndrome, (ii) deep divergences between Atlantic and Indo-Pacific clades may be explained by ancient vicariant events, and (iii) sexual dimorphism evolved a single time in concert with complex sexual behaviour. Furthermore, several cubozoan taxa are either para-or polyphyletic, and we address some of these taxonomic issues by designating a new family, Carukiidae, a new genus, Copula, and by redefining the families Tamoyidae and Tripedaliidae. Lastly, cubozoan species identities have long been misunderstood and the data presented here support many of the recent scientific descriptions of cubozoan species. However, the results of a phylogeographic analysis of Alatina moseri from Hawai'i and Alatina mordens from Australia indicate that these two nominal species represent a single species that has maintained metapopulation cohesion by natural or anthropogenic dispersal. C1 [Bentlage, Bastian; Cartwright, Paulyn] Univ Kansas, Dept Ecol & Evolutionary Biol, Lawrence, KS 66045 USA. [Bentlage, Bastian; Lewis, Cheryl; Collins, Allen G.] Smithsonian Inst, Natl Museum Nat Hist, Natl Systemat Lab, NMFS, Washington, DC 20013 USA. [Yanagihara, Angel A.] Univ Hawaii, Pacific Biomed Res Ctr, Bekesy Lab Neurobiol, Honolulu, HI 96822 USA. [Richards, Gemma S.] Univ Queensland, Sch Biol Sci, Brisbane, Qld 4072, Australia. RP Bentlage, B (reprint author), Univ Kansas, Dept Ecol & Evolutionary Biol, 1200 Sunnyside Ave, Lawrence, KS 66045 USA. EM bentlage@ku.edu RI Collins, Allen/A-7944-2008; Yanagihara, Angel/O-5664-2016 OI Collins, Allen/0000-0002-3664-9691; Yanagihara, Angel/0000-0001-6908-8176 FU US NSF Assembling the Tree of Life [EF-053179]; PADI Foundation FX We thank the following for assistance in the field, facilitation of museum studies, donation of specimens and/or sharing of knowledge: A. C. Arneson, the Australian Volunteer Coastguard Association-Townsville Flotilla, K. Bayha, T. Beukes, T. Coffer, Jen Collins, John Collins, M. Daly, M. N. Dawson, M. Ekins, N. M. Evans, P. J. Fenner, L. Gershwin, B. Gillan, G. C. Gray, the Great Barrier Reef Marine Park Authority, L. Gusmao, R. Helm, J. O'Keefe, M. Kawahara, S. Keable, S. Kubota, D. Lindsay, A. E. Migotto, A. C. Morandini, P. & L. Richards, R. Satterlie, the Two Oceans Aquarium. M. Migita and the Watanuki family kindly translated the original description of C. brevipedalia. We gratefully acknowledge J. Seymour and T. Carrette who provided many of the samples included in our analyses. Thanks to A. M. Nawrocki for collecting a specimen and helping with multi-threaded ML analyses. Two anonymous reviewers provided constructive criticisms that improved the manuscript significantly. Collections and technical staff of the National Museum of Natural History and the National Systematics Lab of NOAA's Fisheries Service provided assistance with handling and cataloguing voucher specimens, extraction of some DNA and amplification and sequencing of some genetic markers. Funding was provided through US NSF Assembling the Tree of Life grant EF-053179 to P. C., A. G. C. and D. Fautin and a PADI Foundation grant to B. B. NR 76 TC 33 Z9 43 U1 8 U2 80 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 EI 1471-2954 J9 P ROY SOC B-BIOL SCI JI Proc. R. Soc. B-Biol. Sci. PD FEB 7 PY 2010 VL 277 IS 1680 BP 493 EP 501 DI 10.1098/rspb.2009.1707 PG 9 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 535WB UT WOS:000273001500020 PM 19923131 ER PT J AU Caldwell, MS McDaniel, JG Warkentin, KM AF Caldwell, Michael S. McDaniel, J. Gregory Warkentin, Karen M. TI Is it safe? Red-eyed treefrog embryos assessing predation risk use two features of rain vibrations to avoid false alarms SO ANIMAL BEHAVIOUR LA English DT Article DE Agalychnis callidryas; anura; detection theory; discrimination; decision rule; information; phenotypic plasticity; predator detection; predator-prey interaction; red-eyed treefrog ID EGG PREDATORS; TRADE-OFFS; CUES; ENVIRONMENT; INFORMATION; LEAFMINER; EVOLUTION; ANIMALS; SIGNALS AB Prey use predator cues to inform defensive decisions. Detecting these cues is often complicated by benign stimuli that resemble and can be mistaken for predators, leading prey to display costly defences incorrectly. One strategy that prey have evolved to reduce these 'false alarms' is to respond only to stimuli with characteristics consistent with predator cues. Decision errors might still be frequent, however, in cases where the probability distributions of benign stimulus properties completely overlap those of predator cues. In such cases, inhibition of defensive responses by characteristic features of benign stimuli could further improve discrimination. Red-eyed treefrog embryos, Agalychnis callidryas, hatch prematurely to escape egg predators. They detect predators using vibrations generated during attacks. However, common benign disturbances such as rainstorms generate vibrations with property probability distributions that largely overlap those of predators. We used vibration playbacks to test the hypotheses that embryos use two features of rainstorm vibrations not shared by predator attacks, characteristic high frequencies and an initial period of intensity buildup, to avoid hatching in response to this benign stimulus. The escape-hatching response to otherwise stimulatory vibrations is reduced in the presence of either feature characteristic of rainstorms. Either A. callidryas embryos use rainstorm features to inform their hatching decision or these features alter their perception of predator cues. Identifying likely sources of potential false alarms and comparing their stimulus characteristics to predator cues and prey decision rules will improve our understanding of both the information processing challenges facing prey and the ways they solve them. (C) 2009 The Association for the Study of Animal Behaviour. Published by Elsevier Ltd. All rights reserved. C1 [Caldwell, Michael S.; Warkentin, Karen M.] Boston Univ, Dept Biol, Boston, MA 02215 USA. [McDaniel, J. Gregory] Boston Univ, Dept Mech Engn, Boston, MA 02215 USA. [Warkentin, Karen M.] Smithsonian Trop Res Inst, Panama City, Panama. RP Caldwell, MS (reprint author), Boston Univ, Dept Biol, 5 Cummington St, Boston, MA 02215 USA. EM mpod3@bu.edu FU National Science Foundation [IBN-0234439]; Boston University; Smithsonian Tropical Research Institute FX We thank A. D'Amato, K. Wright, S. Poo and S. Galeano for assistance with playback experiments, as well as G. Rosenthal, M. Sorenson, C. Schneider and three anonymous referees for their comments on the manuscript. This research was funded by the National Science Foundation (IBN-0234439), Boston University and the Smithsonian Tropical Research Institute. NR 29 TC 13 Z9 13 U1 2 U2 22 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 FEB PY 2010 VL 79 IS 2 BP 255 EP 260 DI 10.1016/j.anbehav.2009.11.005 PG 6 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA 548SJ UT WOS:000273986300004 ER PT J AU Eberhard, WG AF Eberhard, William G. TI Recovery of spiders from the effects of parasitic wasps: implications for fine-tuned mechanisms of manipulation SO ANIMAL BEHAVIOUR LA English DT Article DE Allocyclosa bifurca; orb web; parasitic manipulation of host; parasitoid wasp; Polysphincta clade; Polysphincta gutfreundi ID HEAD PROTEOME; HYMENOPTERA; ARANEAE; ICHNEUMONIDAE; BEHAVIOR; ARANEIDAE; TETRAGNATHIDAE; PIMPLINAE; UCHIDA; BRAIN AB The larva of the ichneumonid wasp Polysphincta gutfreundi induces its host, the orb-weaving spider Allocyclosa bifurca, to build a highly modified, physically stable orb web, to which the larva then attaches its pupal cocoon, and to add an otherwise unusual linear silk stabilimentum to this web that may camouflage the cocoon. The effects of the larva are apparently due to a chemical product or products that it introduces into the spider. Behavioural modi. cation is gradual, and various behavioural effects arise in a consistent order. If the wasp larva is experimentally removed just before it kills the spider, the spider's behaviour recovers gradually in the reverse order. In addition, a greater delay in removing the larva leads to more pronounced and enduring behavioural changes, so the larval effects may depend on a cumulative or dose-dependent process. Changes in numbers and lengths of radii and numbers of sticky spiral loops could result from correlated larval effects on the reduction in the amount of silk in the spider's sticky spiral silk glands (or a signal thereof), but several other types of behavioural change are probably under separate controls; multiple larval products may be involved. The larvae may affect higher levels of behavioural decisions by spiders that determine overall web 'design', rather than lower levels, such as control of particular behaviour patterns, as may be affected by related wasps. The larva's effects are fine-tuned to details of the host's natural history. The Association for the Study of Animal Behaviour. Published by Elsevier Ltd. C1 [Eberhard, William G.] Univ Costa Rica, Smithsonian Trop Res Inst, San Pedro, Costa Rica. [Eberhard, William G.] Univ Costa Rica, Escuela Biol, San Pedro, Costa Rica. RP Eberhard, WG (reprint author), Univ Costa Rica, Smithsonian Trop Res Inst, Ciudad Univ, San Pedro, Costa Rica. EM william.eberhard@gmail.com FU Smithsonian Tropical Research Institute; Universidad de Costa Rica FX I thank Ian Gauld, Paul Hanson, and Herbert W. Levi for kindly identifying the wasps and spiders; Federico Bolanos and Jeremy Niven for help with statistics and literature; and M. J. West- Eberhard for comments on the manuscript. Financial support was provided by the Smithsonian Tropical Research Institute and the Universidad de Costa Rica. NR 30 TC 35 Z9 38 U1 7 U2 45 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0003-3472 EI 1095-8282 J9 ANIM BEHAV JI Anim. Behav. PD FEB PY 2010 VL 79 IS 2 BP 375 EP 383 DI 10.1016/j.anbehav.2009.10.033 PG 9 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA 548SJ UT WOS:000273986300017 ER PT J AU Walsh, JM AF Walsh, Jane MacLaren TI SKULL OF DOOM? SO APOLLO-THE INTERNATIONAL MAGAZINE FOR COLLECTORS LA English DT Article ID 2 CRYSTAL SKULLS C1 Smithsonian Inst, Washington, DC 20560 USA. RP Walsh, JM (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 15 TC 0 Z9 0 U1 0 U2 2 PU APOLLO MAGAZINE LTD PI LONDON PA 20 THEOBALD'S RD, LONDON WC1X 8PF, ENGLAND SN 0003-6536 J9 APOLLO JI Apollo PD FEB PY 2010 VL 171 IS 573 BP 42 EP 47 PG 6 WC Art SC Art GA 564SG UT WOS:000275236700007 ER PT J AU Demes, KW Littler, MM Littler, DS AF Demes, Kyle W. Littler, Mark M. Littler, Diane S. TI Comparative phosphate acquisition in giant-celled rhizophytic algae (Bryopsidales, Chlorophyta): Fleshy vs. calcified forms SO AQUATIC BOTANY LA English DT Article DE Bryopsidales; Calcification; Nutrient uptake; Phosphate; Rhizoids ID NUTRIENT-LIMITED PRODUCTIVITY; FLORIDA-KEYS; CAULERPA-CUPRESSOIDES; PRIMARY PRODUCERS; EPILITHIC FORMS; GREEN-ALGA; MACROALGAE; PHOSPHORUS; NITROGEN; PHOTOSYNTHESIS AB Phosphate uptake through above-ground thalli vs. subterranean rhizoids has been compared in siphonaceous rhizophytic green algal species from five globally distributed tropical genera: Avrainvillea nigricans Decaisne, Caulerpa lanuginosa J. Agardh, Halimeda incrassata (J. Ellis) J.V. Lamouroux, Penicillus capitatus Lamarck, and Udotea flabellum (J. Ellis & Solander) M. Howe. Plants were collected, acclimated to lab conditions for 3 days, and then incubated for 8 h at saturating light intensity with 30 mu M PO(4)(3-) added to their above-ground thallus or below-ground rhizoids. Percent tissue phosphorus was then compared to control specimens, which were run simultaneously in the absence of phosphate. The two fleshy species, A. nigricans and C. lanuginosa, showed no significant differences in tissue nutrient status, and displayed much larger variation among controls than the three calcified species. Calcified species showed greater phosphorus content after being exposed to either above- or below-ground thallus portions, indicating that these seaweeds can respond to short term increases in nutrient availability and have a more regulated nutrient acquisition mechanism. Results suggest that calcification may play an important role in phosphorus absorption. (C) 2009 Elsevier B.V. All rights reserved. C1 [Demes, Kyle W.] Moss Landing Marine Labs, Moss Landing, CA 95039 USA. [Littler, Mark M.; Littler, Diane S.] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. RP Demes, KW (reprint author), Moss Landing Marine Labs, Pob 450, Moss Landing, CA 95039 USA. EM kglenn@mlml.calstate.edu OI Glenn, Kyle/0000-0002-6276-8125 FU Smithsonian Institution; Smithsonian Marine Station at Fort Pierce (SMSFP) [806] FX We would like to thank Jonathan Pruitt, Arley Muth, Laura Eierman, and Stephanie Marquardt for help in the lab and with field collections, Sherry and John Reed for laboratory set-up and maintenance, and Jan Vermaat and two anonymous reviewers for constructive comments on earlier drafts of this manuscript. This work was funded by the Smithsonian Institution Link Fellowship and the Smithsonian Marine Station at Fort Pierce (SMSFP Contr. No. 806). NR 22 TC 3 Z9 4 U1 3 U2 15 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0304-3770 J9 AQUAT BOT JI Aquat. Bot. PD FEB PY 2010 VL 92 IS 2 BP 157 EP 160 DI 10.1016/j.aquabot.2009.10.012 PG 4 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA 553GF UT WOS:000274353600012 ER PT J AU Rines, K Diaferio, A AF Rines, Kenneth Diaferio, Antonaldo TI INFALL REGIONS AND SCALING RELATIONS OF X-RAY SELECTED GROUPS SO ASTRONOMICAL JOURNAL LA English DT Article DE cosmology: observations; galaxies: clusters: individual; galaxies: kinematics and dynamics ID DIGITAL SKY SURVEY; GALAXY CLUSTER SURVEY; MASS PROFILE; VELOCITY DISPERSION; RICH CLUSTERS; DATA RELEASE; LUMINOSITY FUNCTION; OPTICAL-PROPERTIES; FUTURE EVOLUTION; ABELL CLUSTERS AB We use the Fifth Data Release of the Sloan Digital Sky Survey (SDSS) to study X-ray-selected galaxy groups and compare their properties to clusters. We search for infall patterns around the groups and use these to measure group mass profiles to large radii. In previous work, we analyzed infall patterns for an X-ray-selected sample of 72 clusters from the ROSAT All-Sky Survey. Here, we extend this approach to a sample of systems with smaller X-ray fluxes selected from the 400 deg(2) serendipitous survey of clusters and groups in ROSAT pointed observations. We identify 16 groups with SDSS DR5 spectroscopy, search for infall patterns, and compute mass profiles out to 2-6 h(-1) Mpc from the group centers with the caustic technique. No other mass estimation methods are currently available at such large radii for these low-mass groups, because the virial estimate requires dynamical equilibrium and the gravitational lensing signal is too weak. Despite the small masses of these groups, most display recognizable infall patterns. We use caustic and virial mass estimates to measure the scaling relations between different observables, extending these relations to smaller fluxes and luminosities than many previous surveys. Close inspection reveals that three of the groups are subclusters in the outskirts of larger clusters. A fourth group is apparently undergoing a group-group merger. These four merging groups represent the most extreme outliers in the scaling relations. Excluding these groups, we find L(X) alpha sigma(3.1 +/- 1.6)(p), consistent with previous determinations for both clusters and groups. Understanding cluster and group scaling relations is crucial for measuring cosmological parameters from clusters. The complex environments of our group sample reinforce the idea that great care must be taken in determining the properties of low-mass clusters and groups. C1 [Rines, Kenneth] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rines, Kenneth] Western Washington Univ, Dept Phys & Astron, Bellingham, WA 98225 USA. [Diaferio, Antonaldo] Univ Turin, Dipartimento Fis Gen Amedeo Avogadro, Turin, Italy. [Diaferio, Antonaldo] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy. RP Rines, K (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 20, Cambridge, MA 02138 USA. EM kenneth.rines@wwu.edu; diaferio@ph.unito.it FU Italian Ministry of University and Scientific Research; INFN [PD51]; Alfred P. Sloan Foundation; National Aeronautics and Space Administration; National Science Foundation; U.S. Department of Energy; Japanese Monbukagakusho; Max Planck Society FX We thank the referee for a careful reading of the manuscript and for several helpful suggestions that significantly improved the presentation of the results. We thank Margaret Geller for useful discussions during early stages of this work and for insightful comments on early drafts. Support from the PRIN2006 grant "Costituenti fondamentali dell'Universo" of the Italian Ministry of University and Scientific Research and from the INFN grant PD51 is gratefully acknowledged. Funding for the SDSS has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Aeronautics and Space Administration, the National Science Foundation, the U.S. Department of Energy, the Japanese Monbukagakusho, and the Max Planck Society. The SDSS Web site is http://www.sdss.org/. The SDSS is managed by the Astrophysical Research Consortium (ARC) for the Participating Institutions. The Participating Institutions are The University of Chicago, Fermilab, the Institute for Advanced Study, the Japan Participation Group, The Johns Hopkins University, the Korean Scientist Group, Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the MaxPlanck-Institute for Astrophysics (MPA), New Mexico State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington. NR 87 TC 15 Z9 15 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD FEB PY 2010 VL 139 IS 2 BP 580 EP 593 DI 10.1088/0004-6256/139/2/580 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 544FY UT WOS:000273640200020 ER PT J AU Dai, Y Wilner, DJ Andrews, SM Ohashi, N AF Dai, Yu Wilner, David J. Andrews, Sean M. Ohashi, Nagayoshi TI MILLIMETER DUST EMISSION IN THE GQ LUP SYSTEM SO ASTRONOMICAL JOURNAL LA English DT Article DE circumstellar matter; protoplanetary disks; stars: individual (GQ Lup) ID T-TAURI STARS; SUB-STELLAR COMPANION; SUBSTELLAR COMPANION; CIRCUMSTELLAR DISKS; ACCRETION DISKS; YOUNG OBJECTS; GRAIN-GROWTH; SKY SURVEY; PLANETS; GAS AB We present SubMillimeter Array observations of the GQ Lup system at 1.3 mm wavelength with 0 ''.4 (similar to 60 AU) resolution. Emission is detected from the position of the primary star, GQ Lup A, and is marginally resolved. No emission is detected from the substellar companion, GQ Lup B, 0 ''.7 away. These data, together with models of the spectral energy distribution, suggest a compact disk around GQ Lup A with mass similar to 3 M(Jup), perhaps truncated by tidal forces. There is no evidence for a gap or hole in the disk that might be the signature of an additional inner companion body capable of scattering GQ Lup B out to similar to 100 AU separation from GQ Lup A. For GQ Lup B to have formed in situ, the disk must have been much more massive and extended. C1 [Dai, Yu] Boston Coll, Dept Phys, Chestnut Hill, MA 02467 USA. [Dai, Yu; Wilner, David J.; Andrews, Sean M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ohashi, Nagayoshi] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. RP Dai, Y (reprint author), Boston Coll, Dept Phys, 140 Commonwealth Ave, Chestnut Hill, MA 02467 USA. EM ydai@cfa.harvard.edu NR 39 TC 7 Z9 7 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD FEB PY 2010 VL 139 IS 2 BP 626 EP 629 DI 10.1088/0004-6256/139/2/626 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 544FY UT WOS:000273640200023 ER PT J AU Levesque, EM Berger, E Kewley, LJ Bagley, MM AF Levesque, Emily M. Berger, Edo Kewley, Lisa J. Bagley, Megan M. TI THE HOST GALAXIES OF GAMMA-RAY BURSTS. I. INTERSTELLAR MEDIUM PROPERTIES OF TEN NEARBY LONG-DURATION GAMMA-RAY BURST HOSTS SO ASTRONOMICAL JOURNAL LA English DT Review DE galaxies: ISM; gamma rays: bursts ID BLUE COMPACT GALAXIES; STAR-FORMING GALAXIES; COMBINED STELLAR STRUCTURE; DIGITAL SKY SURVEY; MASS-METALLICITY RELATION; REVISED IONIZING FLUXES; ACTIVE GALACTIC NUCLEI; METAL-POOR GALAXIES; H-II REGIONS; WOLF-RAYET AB We present the first observations from a large-scale survey of nearby (z < 1) long-duration gamma-ray burst (LGRB) host galaxies, which consist of eight rest-frame optical spectra obtained at Keck and Magellan. Along with two host galaxy observations from the literature, we use optical emission-line diagnostics to determine metallicities, ionization parameters, young stellar population ages, and star formation rates. We compare the LGRB host environments to a variety of local and intermediate-redshift galaxy populations, as well as the newest grid of stellar population synthesis and photoionization models generated with the Starburst99/Mappings codes. With these comparisons, we investigate whether the GRB host galaxies are consistent with the properties of the general galaxy population, and therefore whether they may be used as reliable tracers of star formation. Despite the limitations inherent in our small sample, we find strong evidence that LGRB host galaxies generally have low-metallicity interstellar medium (ISM) environments out to z similar to 1. The ISM properties of our GRB hosts, including metallicity and ionization parameter, are significantly different from the general galaxy population and host galaxies of nearby broad-lined Type Ic supernovae. However, these properties show better agreement with a sample of nearby metal-poor galaxies. C1 [Levesque, Emily M.; Kewley, Lisa J.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Levesque, Emily M.; Berger, Edo] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Bagley, Megan M.] Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA. RP Levesque, EM (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. EM emsque@ifa.hawaii.edu FU NSF [AST07-48559] FX We gratefully acknowledge useful correspondence with Warren Brown, Andy Fruchter, Margaret Geller, John Graham, Dan Kocevski, Aybuke Kupcu Yoldas, Claus Leitherer, Philip Massey, George Meynet, Maryam Modjaz, Daniel Schaerer, and Leonie Snijders regarding this work. We thank the anonymous referee for constructive and thoughtful comments on this manuscript. We are grateful for the hospitality and assistance of the W. M. Keck Observatories in Hawaii, in particular the guidance and assistance of Greg Wirth, as well as the Las Campanas Observatory in Chile. This paper made use of data from the Gamma-Ray Burst Coordinates Network (GCN) Circulars. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this sacred mountain. E. Levesque's participation was made possible in part by a Ford Foundation Predoctoral Fellowship. L. Kewley and E. Levesque gratefully acknowledge support by NSF EARLY CAREER AWARD AST07-48559. NR 107 TC 77 Z9 77 U1 1 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD FEB PY 2010 VL 139 IS 2 BP 694 EP 711 DI 10.1088/0004-6256/139/2/694 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 544FY UT WOS:000273640200029 ER PT J AU Kim, DW Protopapas, P Alcock, C Byun, YI Kyeong, J Lee, BC Wright, NJ Axelrod, T Bianco, FB Chen, WP Coehlo, NK Cook, KH Dave, R King, SK Lee, T Lehner, MJ Lin, HC Marshall, SL Porrata, R Rice, JA Schwamb, ME Wang, JH Wang, SY Wen, CY Zhang, ZW AF Kim, D. -W. Protopapas, P. Alcock, C. Byun, Y. -I. Kyeong, J. Lee, B. -C. Wright, N. J. Axelrod, T. Bianco, F. B. Chen, W. -P. Coehlo, N. K. Cook, K. H. Dave, R. King, S. -K. Lee, T. Lehner, M. J. Lin, H. -C. Marshall, S. L. Porrata, R. Rice, J. A. Schwamb, M. E. Wang, J. -H. Wang, S. -Y. Wen, C. -Y. Zhang, Z. -W. TI THE TAIWAN-AMERICAN OCCULTATION SURVEY PROJECT STELLAR VARIABILITY. I. DETECTION OF LOW-AMPLITUDE delta SCUTI STARS SO ASTRONOMICAL JOURNAL LA English DT Article DE stars: variables: delta Scuti; methods: data analysis; surveys ID VARIABLE-STARS; STROMGREN PHOTOMETRY; GAMMA-DORADUS; SCT STARS; CATALOG; ASTEROSEISMOLOGY; PULSATION; CLUSTER; CLASSIFICATION; SATELLITE AB We analyzed data accumulated during 2005 and 2006 by the Taiwan-American Occultation Survey (TAOS) in order to detect short-period variable stars (periods of less than or similar to 1 hr) such as delta Scuti. TAOS is designed for the detection of stellar occultation by small-size Kuiper Belt Objects and is operating four 50 cm telescopes at an effective cadence of 5 Hz. The four telescopes simultaneously monitor the same patch of the sky in order to reduce false positives. To detect short-period variables, we used the fast Fourier transform algorithm (FFT) in as much as the data points in TAOS light curves are evenly spaced. Using FFT, we found 41 short-period variables with amplitudes smaller than a few hundredths of a magnitude and periods of about an hour, which suggest that they are low-amplitude d Scuti stars. The light curves of TAOS d Scuti stars are accessible online at the Time Series Center Web site (http://timemachine.iic.harvard.edu). C1 [Kim, D. -W.; Protopapas, P.; Alcock, C.; Wright, N. J.; Bianco, F. B.; Lehner, M. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kim, D. -W.; Protopapas, P.; Dave, R.] Harvard Univ, Sch Engn & Appl Sci, Initiat Innovat Comp, Cambridge, MA 02138 USA. [Kim, D. -W.; Byun, Y. -I.] Yonsei Univ, Dept Astron, Seoul 120749, South Korea. [Kyeong, J.; Lee, B. -C.] Korea Astron & Space Sci Inst, Taejon 305348, South Korea. [Axelrod, T.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Bianco, F. B.; Lehner, M. J.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Chen, W. -P.; Lin, H. -C.; Wang, J. -H.; Zhang, Z. -W.] Natl Cent Univ, Inst Astron, Jhongli 320, Taoyuan County, Taiwan. [Coehlo, N. K.; Rice, J. A.] Univ Calif Berkeley, Dept Stat, Berkeley, CA 94720 USA. [Cook, K. H.; Marshall, S. L.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94550 USA. [King, S. -K.; Lee, T.; Lehner, M. J.; Wang, J. -H.; Wang, S. -Y.; Wen, C. -Y.; Zhang, Z. -W.] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. [Marshall, S. L.] Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA. [Porrata, R.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Schwamb, M. E.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. RP Kim, DW (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Lee, Typhoon/N-8347-2013; OI Lehner, Matthew/0000-0003-4077-0985 FU National Research Foundation of Korea [2009-0075376]; NSC [96-2112-M-008-024-MY3]; National Science Foundation [AST-0501681]; NASA [NNG04G113G]; U.S. Department of Energy by Lawrence Livermore National Laboratory [W-7405-Eng-48, DE-AC52-07NA27344]; Stanford Linear Accelerator Center [DE-AC02-76SF00515]; FAS Research Computing Group at the Harvard; [AS-88-TP-A02] FX Y.-I. Byun acknowledges the support of the National Research Foundation of Korea through Grant 2009-0075376. The work at National Central University was supported by the grant NSC 96-2112-M-008-024-MY3. Work at Academia Sinica was supported in part by the thematic research program AS-88-TP-A02. 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. S. L. M.'s 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 by Stanford Linear Accelerator Center under Contract DE-AC02-76SF00515. K. H. Cook's 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. We also thank J. D. Hartman at Harvard-Smithsonian Center for Astrophysics for useful discussion.; The detrending and the analysis of data sets in this paper were run on the Odyssey cluster supported by the FAS Research Computing Group at the Harvard. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. 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. NR 60 TC 6 Z9 6 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD FEB PY 2010 VL 139 IS 2 BP 757 EP 764 DI 10.1088/0004-6256/139/2/757 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 544FY UT WOS:000273640200033 ER PT J AU Di Stefano, R Primini, FA Liu, J Kong, A Patel, B AF Di Stefano, R. Primini, F. A. Liu, J. Kong, A. Patel, B. TI Populations of supersoft X-ray sources: Novae, tidal disruption, Type Ia supernovae, accretion-induced collapse, ionization, and intermediate-mass black holes? SO ASTRONOMISCHE NACHRICHTEN LA English DT Article DE black hole physics; galaxies: general; nova, cataclysmic variables; stars: neutron; supernovae: general; white dwarfs; X-rays: binaries; X-rays: ISM ID WHITE-DWARF; EXTERNAL GALAXIES; SOFT SOURCES; QUASI-SOFT; XMM-NEWTON; BINARY; EVOLUTION; CAL-87; STARS; OUTBURST AB Observations of hundreds of supersoft X-ray sources (SSSs) in external galaxies have shed light on the diversity of the class and on the natures of the sources. SSSs are linked to the physics of Type la supernovae and accretion-induced collapse, ultraluminous X-ray sources and black holes, the ionization of the interstellar medium, and tidal disruption by supermassive black holes. The class of SSSs has an extension to higher luminosities: ultraluminous SSSs have luminosities above 10(39) erg s(-1). There is also an extension to higher energies: quasisoft X-ray sources (QSSs) emit photons with energies above 1 keV, but few or none with energies above 2 keV. Finally, a significant fraction of the SSSs found in external galaxies switch states between observations, becoming either quasisoft or hard. For many systems "supersoft" refers to a temporary state; SSSs are sources, possibly including a variety of fundamentally different system types, that pass through such a state. We review those results derived from extragalactic data and related theoretical work that are most surprising and that suggest directions for future research. (C) 2010 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim C1 [Di Stefano, R.; Primini, F. A.; Liu, J.; Patel, B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kong, A.] Natl Tsing Hua Univ, Inst Astron, Hsinchu 30013, Taiwan. [Kong, A.] Natl Tsing Hua Univ, Dept Phys, Hsinchu 30013, Taiwan. [Patel, B.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08855 USA. RP Di Stefano, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rdistefano@cfa.harvard.edu OI Primini, Francis/0000-0002-6077-0643 FU NASA [AR-10948.01-A-R, GO8-9092X] FX Acknowledgements. This work was supported in part by NASA through AR-10948.01-A-R and GO8-9092X. NR 38 TC 12 Z9 12 U1 0 U2 2 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0004-6337 J9 ASTRON NACHR JI Astro. Nachr. PD FEB PY 2010 VL 331 IS 2 BP 205 EP 211 DI 10.1002/asna.200911328 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 564LC UT WOS:000275214700015 ER PT J AU Torres, G Andersen, J Gimenez, A AF Torres, G. Andersen, J. Gimenez, A. TI Accurate masses and radii of normal stars: modern results and applications SO ASTRONOMY AND ASTROPHYSICS REVIEW LA English DT Review DE Stars: fundamental parameters; Stars: binaries: eclipsing; Stars: binaries: spectroscopic; Stars: interiors; Stars: evolution ID ECLIPSING BINARY STAR; M-CIRCLE-DOT; SOLAR-TYPE STARS; DISENTANGLED COMPONENT SPECTRA; PHASES DIFFERENTIAL ASTROMETRY; STELLAR EVOLUTION MODELS; GENEVA-COPENHAGEN SURVEY; APSIDAL-MOTION TEST; MAIN-SEQUENCE STAR; A-TYPE SYSTEM AB This article presents and discusses a critical compilation of accurate, fundamental determinations of stellar masses and radii. We have identified 95 detached binary systems containing 190 stars (94 eclipsing systems, and alpha Centauri) that satisfy our criterion that the mass and radius of both stars be known within errors of +/- 3% accuracy or better. All of them are non-interacting systems, and so the stars should have evolved as if they were single. This sample more than doubles that of the earlier similar review by Andersen (Astron Astrophys Rev 3: 91-126, 1991), extends the mass range at both ends and, for the first time, includes an extragalactic binary. In every case, we have examined the original data and recomputed the stellar parameters with a consistent set of assumptions and physical constants. To these we add interstellar reddening, effective temperature, metal abundance, rotational velocity and apsidal motion determinations when available, and we compute a number of other physical parameters, notably luminosity and distance. These accurate physical parameters reveal the effects of stellar evolution with unprecedented clarity, and we discuss the use of the data in observational tests of stellar evolution models in some detail. Earlier findings of significant structural differences between moderately fast-rotating, mildly active stars and single stars, ascribed to the presence of strong magnetic and spot activity, are confirmed beyond doubt. We also show how the best data can be used to test prescriptions for the subtle interplay between convection, diffusion, and other non-classical effects in stellar models. The amount and quality of the data also allow us to analyse the tidal evolution of the systems in considerable depth, testing prescriptions of rotational synchronisation and orbital circularisation in greater detail than possible before. We show that the formulae for pseudo-synchronisation of stars in eccentric orbits predict the observed rotations quite well, except for very young and/or widely separated stars. Deviations do occur, however, especially for stars with convective envelopes. The superior data set finally demonstrates that apsidal motion rates as predicted from General Relativity plus tidal theory are in good agreement with the best observational data. No reliable binary data exist, which challenge General Relativity to any significant extent. The new data also enable us to derive empirical calibrations of M and R for single (post-) main-sequence stars above 0.6 M(circle dot). Simple, polynomial functions of T(eff), log g and [Fe/H] yield M and R within errors of 6 and 3%, respectively. Excellent agreement is found with independent determinations for host stars of transiting extrasolar planets, and good agreement with determinations of M and R from stellar models as constrained by trigonometric parallaxes and spectroscopic values of Teff and [Fe/H]. Finally, we list a set of 23 interferometric binaries with masses known to be better than 3%, but without fundamental radius determinations (except alpha Aur). We discuss the prospects for improving these and other stellar parameters in the near future. C1 [Torres, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Andersen, J.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Andersen, J.] Nord Opt Telescope Sci Assoc, La Palma, Spain. [Gimenez, A.] CSIC, INTA, Ctr Astrobiol, Madrid 28850, Spain. RP Torres, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,Mail Stop 20, Cambridge, MA 02138 USA. EM gtorres@cfa.harvard.edu; ja@astro.ku.dk; agimenez@rssd.esa.int NR 211 TC 494 Z9 497 U1 2 U2 22 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0935-4956 J9 ASTRON ASTROPHYS REV JI Astron. Astrophys. Rev. PD FEB PY 2010 VL 18 IS 1-2 BP 67 EP 126 DI 10.1007/s00159-009-0025-1 PG 60 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 546FO UT WOS:000273796800002 ER PT J AU Crouzet, N Guillot, T Agabi, A Rivet, JP Bondoux, E Challita, Z Fantei-Caujolle, Y Fressin, F Mekarnia, D Schmider, FX Valbousquet, F Blazit, A Bonhomme, S Abe, L Daban, JB Gouvret, C Fruth, T Rauer, H Erikson, A Barbieri, M Aigrain, S Pont, F AF Crouzet, N. Guillot, T. Agabi, A. Rivet, J. -P. Bondoux, E. Challita, Z. Fantei-Caujolle, Y. Fressin, F. Mekarnia, D. Schmider, F. -X. Valbousquet, F. Blazit, A. Bonhomme, S. Abe, L. Daban, J. -B. Gouvret, C. Fruth, T. Rauer, H. Erikson, A. Barbieri, M. Aigrain, S. Pont, F. TI ASTEP South: an Antarctic Search for Transiting ExoPlanets around the celestial south pole SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE methods: observational; methods: data analysis; site testing; techniques: photometric ID DOME-C; SKY BRIGHTNESS; SEEING MEASUREMENTS; PHOTOMETRY; PLANETS; STATISTICS AB Context. The Concordia base in Dome C, Antarctica, is an extremely promising site for photometric astronomy due to the 3-month long night during the Antarctic winter, favorable weather conditions, and low scintillation. Aims. The ASTEP project (Antarctic Search for Transiting ExoPlanets) is a pilot project to discover transiting planets and understand the limits of visible photometry from the Concordia site. Methods. ASTEP South is the first phase of the ASTEP project. The instrument is a fixed 10 cm refractor with a 4k x 4k CCD camera in a thermalized box, pointing continuously a 3.88 x 3.88 degrees(2) field of view centered on the celestial south pole. We describe the project and report results of a preliminary data analysis. Results. ASTEP South became fully functional in June 2008 and obtained 1592 hours of data during the 2008 Antarctic winter. The data are of good quality but the analysis has to account for changes in the PSF (point spread function) due to rapid ground seeing variations and instrumental effects. The pointing direction is stable within 10 arcsec on a daily timescale and drifts by only 34 arcsec in 50 days. A truly continuous photometry of bright stars is possible in June ( the noon sky background peaks at a magnitude R approximate to 15 arcsec(-2) on June 22), but becomes challenging in July (the noon sky background magnitude is R approximate to 12.5 arcsec(-2) on July 20). The weather conditions are estimated from the number of stars detected in the field. For the 2008 winter, the statistics are between 56.3% and 68.4% of excellent weather, 17.9% to 30% of veiled weather (when the probable presence of thin clouds implies a lower number of detected stars) and 13.7% of bad weather. Using these results in a probabilistic analysis of transit detection, we show that the detection efficiency of transiting exoplanets in one given field is improved at Dome C compared to a temperate site such as La Silla. For example we estimate that a year-long campaign of 10 cm refractor could reach an efficiency of 69% at Dome C versus 45% at La Silla for detecting 2-day period giant planets around target stars from magnitude 10 to 15. The detection efficiency decreases for planets with longer orbital periods, but in relative sense it is even more favorable to Dome C. Conclusions. This shows the high potential of Dome C for photometry and future planet discoveries. C1 [Crouzet, N.; Guillot, T.; Rivet, J. -P.; Bonhomme, S.] Univ Nice Sophia Antipolis, CNRS, UMR 6202, Observ Cote Azur, F-06304 Nice 4, France. [Agabi, A.; Bondoux, E.; Challita, Z.; Fantei-Caujolle, Y.; Mekarnia, D.; Schmider, F. -X.; Blazit, A.; Abe, L.; Daban, J. -B.; Gouvret, C.] Univ Nice Sophia Antipolis, CNRS, UMR 6525, Observ Cote Azur, F-06108 Nice 2, France. [Fressin, F.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Valbousquet, F.] Opt & Vis, F-06162 Juan Les Pins, France. [Bondoux, E.; Challita, Z.] Concordia Stn, Dome C, France. [Rauer, H.] TU Berlin, Ctr Astron & Astrophys, D-10623 Berlin, Germany. [Fruth, T.; Rauer, H.; Erikson, A.] DLR Inst Planetary Res, D-12489 Berlin, Germany. [Barbieri, M.] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy. [Aigrain, S.; Pont, F.] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England. RP Crouzet, N (reprint author), Univ Nice Sophia Antipolis, CNRS, UMR 6202, Observ Cote Azur, F-06304 Nice 4, France. EM Nicolas.Crouzet@oca.eu RI Schmider, Francois-Xavier/C-5435-2012; OI Barbieri, Mauro/0000-0001-8362-3462 FU Agence Nationale de la Recherche (ANR); Institut National des Sciences de l'Univers (INSU); Programme National de Planetologie (PNP); Plan Pluri-Formation OPERA between the Observatoire de la Cote d'Azur; Universite de Nice-Sophia Antipolis; French Institut Paul-Emile Victor (IPEV); Italian Programma Nazionale di Ricerche in Antartide (PNRA) FX The ASTEP project is funded by the Agence Nationale de la Recherche (ANR), the Institut National des Sciences de l'Univers (INSU), the Programme National de Planetologie (PNP), and the Plan Pluri-Formation OPERA between the Observatoire de la Cote d'Azur and the Universite de Nice-Sophia Antipolis. The entire logistics at Concordia is handled by the French Institut Paul-Emile Victor (IPEV) and the Italian Programma Nazionale di Ricerche in Antartide (PNRA). The research grant for N. Crouzet is supplied by the Region Provence Alpes Cote d'Azur and the Observatoire de la Cote d'Azur. We wish to further thank E. Fossat for his helpful remarks on the manuscript. See http://fizeau.unice.fr/astep/ for more information about the ASTEP project. NR 34 TC 14 Z9 14 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 FEB-MAR PY 2010 VL 511 AR A36 DI 10.1051/0004-6361/200913629 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 571LD UT WOS:000275752400092 ER PT J AU Perina, S Cohen, JG Barmby, P Beasley, MA Bellazzini, M Brodie, JP Federici, L Pecci, FF Galleti, S Hodge, PW Huchra, JP Kissler-Patig, M Puzia, TH Strader, J AF Perina, S. Cohen, J. G. Barmby, P. Beasley, M. A. Bellazzini, M. Brodie, J. P. Federici, L. Pecci, F. Fusi Galleti, S. Hodge, P. W. Huchra, J. P. Kissler-Patig, M. Puzia, T. H. Strader, J. TI An HST/WFPC2 survey of bright young clusters in M 31 IV. Age and mass estimates SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: star clusters; galaxies: individual: M 31; supergiants; stars: evolution ID LARGE-MAGELLANIC-CLOUD; COLOR-MAGNITUDE DIAGRAMS; EXTRAGALACTIC GLOBULAR-CLUSTERS; RESOLVED STELLAR POPULATIONS; TELESCOPE WFPC2 PHOTOMETRY; LOCAL GROUP GALAXIES; STAR-CLUSTERS; MILKY-WAY; LUMINOSITY FUNCTION; STRUCTURAL PARAMETERS AB Aims. We present the main results of an imaging survey of possible young massive clusters (YMC) in M 31 performed with the Wide Field and Planetary Camera 2 (WFPC2) on the Hubble Space Telescope (HST), with the aim of estimating their age and their mass. We obtained shallow ( to B similar to 25) photometry of individual stars in 19 clusters ( of the 20 targets of the survey). We present the images and color magnitude diagrams (CMDs) of all of our targets. Methods. Point spread function fitting photometry of individual stars was obtained for all the WFPC2 images of the target clusters, and the completeness of the final samples was estimated using extensive sets of artificial stars experiments. The reddening, age, and metallicity of the clusters were estimated by comparing the observed CMDs and luminosity functions (LFs) with theoretical models. Stellar masses were estimated by comparison with theoretical models in the log( Age) vs. absolute integrated magnitude plane, using ages estimated from our CMDs and integrated J, H, K magnitudes from 2MASS-6X. Results. Nineteen of the twenty surveyed candidates were confirmed to be real star clusters, while one turned out to be a bright star. Three of the clusters were found not to be good YMC candidates from newly available integrated spectroscopy and were in fact found to be old from their CMD. Of the remaining sixteen clusters, fourteen have ages between 25 Myr and 280 Myr, two have older ages than 500 Myr ( lower limits). By including ten other YMC with HST photometry from the literature, we assembled a sample of 25 clusters younger than 1 Gyr, with mass ranging from 0.6 x 10(4) M-circle dot to 6 x 10(4) M-circle dot, with an average of similar to 3 x 10(4) M-circle dot. Our estimates of ages and masses well agree with recent independent studies based on integrated spectra. Conclusions. The clusters considered here are confirmed to have masses significantly higher than Galactic open clusters (OC) in the same age range. Our analysis indicates that YMCs are relatively common in all the largest star-forming galaxies of the Local Group, while the lack of known YMC older than 20 Myr in the Milky Way may stem from selection effects. C1 [Perina, S.; Bellazzini, M.; Federici, L.; Pecci, F. Fusi; Galleti, S.] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy. [Perina, S.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. [Barmby, P.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [Beasley, M. A.; Brodie, J. P.] Univ Calif Santa Cruz, Lick Observ, UCO, Santa Cruz, CA 95064 USA. [Beasley, M. A.] Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Canary Islands, Spain. [Cohen, J. G.] CALTECH, Palomar Observ, Pasadena, CA 91125 USA. [Hodge, P. W.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Huchra, J. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kissler-Patig, M.] European So Observ, D-85748 Garching, Germany. RP Perina, S (reprint author), Osservatorio Astron Bologna, INAF, Via Ranzani 1, I-40127 Bologna, Italy. EM sibilla.perina2@unibo.it; jlc@astro.caltech.edu RI Bellazzini , Michele/O-9373-2015; Barmby, Pauline/I-7194-2016 OI Bellazzini , Michele/0000-0001-8200-810X; Barmby, Pauline/0000-0003-2767-0090 NR 141 TC 17 Z9 17 U1 1 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB-MAR PY 2010 VL 511 AR A23 DI 10.1051/0004-6361/200913459 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 571LD UT WOS:000275752400018 ER PT J AU Rygl, KLJ Brunthaler, A Reid, MJ Menten, KM van Langevelde, HJ Xu, Y AF Rygl, K. L. J. Brunthaler, A. Reid, M. J. Menten, K. M. van Langevelde, H. J. Xu, Y. TI Trigonometric parallaxes of 6.7 GHz methanol masers SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE techniques: interferometric; astrometry; masers; stars: formation; ISM: molecules; Galaxy: kinematics and dynamics ID VLBA CALIBRATOR SURVEY; STAR-FORMING REGION; H-II REGIONS; IRAS SOURCES; GALACTIC PLANE; GENERAL CATALOG; CO OBSERVATIONS; PROPER MOTIONS; ROTATION CURVE; ORION NEBULA AB Aims. Emission from the 6.7 GHz methanol maser transition is very strong, is relatively stable, has small internal motions, and is observed toward numerous massive star-forming regions in the Galaxy. Our goal is to perform high-precision astrometry using this maser transition to obtain accurate distances to their host regions. Methods. Eight strong masers were observed during five epochs of VLBI observations with the European VLBI Network between 2006 June, and 2008 March. Results. We report trigonometric parallaxes for five star-forming regions, with accuracies as good as similar to 22 mu as. Distances to these sources are 2.57(-0.27)(+0.34) kpc for ON 1, 0.776(-0.083)(+0.104) kpc for L 1206, 0.929(-0.033)(+0.034) kpc for L 1287, 2.38(-0.12)(+0.13) kpc for NGC 281-W, and 1.59(-0.06)(+0.07) kpc for S 255. The distances and proper motions yield the full space motions of the star-forming regions hosting the masers, and we find that these regions lag circular rotation on average by similar to 17 km s(-1), a value comparable to those found recently by similar studies. C1 [Rygl, K. L. J.; Brunthaler, A.; Menten, K. M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Reid, M. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [van Langevelde, H. J.] Joint Inst VLBI Europe, NL-7990 AA Dwingeloo, Netherlands. [van Langevelde, H. J.] Leiden Univ, Sterrewacht Leiden, NL-2300 RA Leiden, Netherlands. [Xu, Y.] Chinese Acad Sci, Purple Mt Observ, Nanjing 21008, Peoples R China. RP Rygl, KLJ (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. EM kazi@mpifr-bonn.mpg.de; brunthal@mpifr-bonn.mpg.de; reid@cfa.harvard.edu; kmenten@mpifr-bonn.mpg.de; langevelde@jive.nl; xuye@pmo.ac.cn OI van Langevelde, Huib Jan/0000-0002-0230-5946 FU national research councils; International Max Planck Research School (IMPRS) for Astronomy and Astrophysics at the Universities of Bonn and Cologne; Chinese NSF [NSF 10673024, NSF 10703010, NSF 10621303] FX The European VLBI Network is a joint facility of European, Chinese, South African, and other radio astronomy institutes funded by their national research councils. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. We thank the staff at JIVE, especially Bob Campbell, for technical help and support. We thank Amy Mioduszewski (NRAO) for her help with VLA frequency setup. K.L.J.R. 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. Y.X. was supported by Chinese NSF through grants NSF 10673024, 10703010, and 10621303. NR 64 TC 73 Z9 74 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 FEB-MAR PY 2010 VL 511 AR A2 DI 10.1051/0004-6361/200913135 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 571LD UT WOS:000275752400032 ER PT J AU Bongiorno, A Mignoli, M Zamorani, G Lamareille, F Lanzuisi, G Miyaji, T Bolzonella, M Carollo, CM Contini, T Kneib, JP Le Fevre, O Lilly, SJ Mainieri, V Renzini, A Scodeggio, M Bardelli, S Brusa, M Caputi, K Civano, F Coppa, G Cucciati, O de la Torre, S de Ravel, L Franzetti, P Garilli, B Halliday, C Hasinger, G Koekemoer, AM Iovino, A Kampczyk, P Knobel, C Kovac, K Le Borgne, JF Le Brun, V Maier, C Merloni, A Nair, P Pello, R Peng, Y Montero, EP Ricciardelli, E Salvato, M Silverman, J Tanaka, M Tasca, L Tresse, L Vergani, D Zucca, E Abbas, U Bottini, D Cappi, A Cassata, P Cimatti, A Guzzo, L Leauthaud, A Maccagni, D Marinoni, C McCracken, HJ Memeo, P Meneux, B Oesch, P Porciani, C Pozzetti, L Scaramella, R AF Bongiorno, A. Mignoli, M. Zamorani, G. Lamareille, F. Lanzuisi, G. Miyaji, T. Bolzonella, M. Carollo, C. M. Contini, T. Kneib, J. P. Le Fevre, O. Lilly, S. J. Mainieri, V. Renzini, A. Scodeggio, M. Bardelli, S. Brusa, M. Caputi, K. Civano, F. Coppa, G. Cucciati, O. de la Torre, S. de Ravel, L. Franzetti, P. Garilli, B. Halliday, C. Hasinger, G. Koekemoer, A. M. Iovino, A. Kampczyk, P. Knobel, C. Kovac, K. Le Borgne, J. -F. Le Brun, V. Maier, C. Merloni, A. Nair, P. Pello, R. Peng, Y. Perez Montero, E. Ricciardelli, E. Salvato, M. Silverman, J. Tanaka, M. Tasca, L. Tresse, L. Vergani, D. Zucca, E. Abbas, U. Bottini, D. Cappi, A. Cassata, P. Cimatti, A. Guzzo, L. Leauthaud, A. Maccagni, D. Marinoni, C. McCracken, H. J. Memeo, P. Meneux, B. Oesch, P. Porciani, C. Pozzetti, L. Scaramella, R. TI The [O III] emission line luminosity function of optically selected type-2 AGN from zCOSMOS SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE surveys; galaxies: active ID ACTIVE GALACTIC NUCLEI; DIGITAL SKY SURVEY; HARD X-RAY; WIDE-FIELD SURVEY; XMM-NEWTON OBSERVATIONS; HIGH-REDSHIFT QUASARS; COSMOS FIELD; SEYFERT-GALAXIES; SPECTRAL CLASSIFICATION; STARBURST GALAXIES AB Aims. We present a catalog of 213 type-2 AGN selected from the zCOSMOS survey. The selected sample covers a wide redshift range (0.15 < z < 0.92) and is deeper than any other previous study, encompassing the luminosity range 10(5.5) L-circle dot < L-[OIII] < 10(9.1) L-circle dot. We explore the intrinsic properties of these AGN and the relation to their X-ray emission (derived from the XMM-COSMOS observations). We study their evolution by computing the [OIII]lambda 5007 angstrom line luminosity function (LF) and we constrain the fraction of obscured AGN as a function of luminosity and redshift. Methods. The sample was selected on the basis of the optical emission line ratios, after applying a cut to the signal-to-noise ratio (S/N) of the relevant lines. We used the standard diagnostic diagrams ([O III]/H beta versus [N II]/H alpha and [OIII]/H beta versus [S II]/H alpha) to isolate AGN in the redshift range 0.15 < z < 0.45 and the diagnostic diagram [O III]/H beta versus [O II]/H beta to extend the selection to higher redshift (0.5 < z < 0.92). Results. Combining our sample with one drawn from SDSS, we found that the best description of the evolution of type-2 AGN is a luminosity-dependent density evolution model. Moreover, using the type-1 AGN LF we were able to constrain the fraction of type-2 AGN to the total (type-1 + type-2) AGN population. We found that the type-2 fraction decreases with luminosity, in agreement with the most recent results, and shows signs of a slight increase with redshift. However, the trend with luminosity is visible only after combining the SDSS+zCOSMOS samples. From the COSMOS data points alone, the type-2 fraction seems to be quite constant with luminosity. C1 [Bongiorno, A.; Brusa, M.; Hasinger, G.; Merloni, A.; Meneux, B.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Bongiorno, A.] Univ Maryland, Baltimore, MD 21250 USA. [Mignoli, M.; Zamorani, G.; Bolzonella, M.; Bardelli, S.; Coppa, G.; Nair, P.; Vergani, D.; Zucca, E.; Cappi, A.; Pozzetti, L.] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy. [Lamareille, F.; Contini, T.; Le Borgne, J. -F.; Pello, R.; Perez Montero, E.] Univ Toulouse, CNRS, Lab Astrophys Toulouse Tarbes, F-31400 Toulouse, France. [Lanzuisi, G.; Civano, F.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lanzuisi, G.] Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy. [Miyaji, T.] Univ Nacl Autonoma Mexico, Inst Astron, Ensenada, Baja California, Mexico. [Miyaji, T.] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. [Carollo, C. M.; Lilly, S. J.; Caputi, K.; Kampczyk, P.; Knobel, C.; Kovac, K.; Maier, C.; Peng, Y.; Silverman, J.; Oesch, P.; Porciani, C.] ETH, Dept Phys, CH-8093 Zurich, Switzerland. [Kneib, J. P.; Le Fevre, O.; Cucciati, O.; de la Torre, S.; de Ravel, L.; Le Brun, V.; Tasca, L.; Tresse, L.; Abbas, U.; Cassata, P.; Leauthaud, A.] Univ Aix Marseille, Lab Astrophys Marseille, CNRS, F-13388 Marseille 13, France. [Mainieri, V.; Tanaka, M.] ESO, D-85748 Garching, Germany. [Renzini, A.] Osserv Astron Padova, INAF, Padua, Italy. [Scodeggio, M.; de la Torre, S.; Franzetti, P.; Garilli, B.; Iovino, A.; Tasca, L.; Bottini, D.; Maccagni, D.; Memeo, P.] Ist Astrofis Spaziale & Fis Cosm Milano, INAF, I-20133 Milan, Italy. [Coppa, G.; Cimatti, A.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. [de la Torre, S.] Osserv Astron Brera, INAF, I-20121 Milan, Italy. [Halliday, C.; Guzzo, L.] Osserv Astrofis Arcetri, I-50125 Florence, Italy. [Hasinger, G.; Salvato, M.] Max Planck Inst Plasma Phys, D-85748 Garching, Germany. [Koekemoer, A. M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Merloni, A.; Salvato, M.] TUM, Excellence Cluster Universe, D-85748 Garching, Germany. [Perez Montero, E.] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. [Ricciardelli, E.] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy. [Salvato, M.] CALTECH, Pasadena, CA 91125 USA. [Cassata, P.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Marinoni, C.] Ctr Phys Theor, Marseille, France. [McCracken, H. J.] Univ Paris 06, Inst Astrophys Paris, Paris, France. [Scaramella, R.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy. RP Bongiorno, A (reprint author), Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85748 Garching, Germany. EM angelab@mpe.mpg.de RI Lanzuisi, Giorgio/K-4378-2013; Kneib, Jean-Paul/A-7919-2015; Cappi, Alberto/O-9391-2015; Zucca, Elena/O-9396-2015; Bardelli, Sandro/O-9369-2015; Mignoli, Marco/O-9426-2015; Bolzonella, Micol/O-9495-2015; Pello, Roser/G-4754-2010; Le Fevre, Olivier/G-7389-2011 OI Oesch, Pascal/0000-0001-5851-6649; Maier, Christian/0000-0001-6405-2182; Garilli, Bianca/0000-0001-7455-8750; Zamorani, Giovanni/0000-0002-2318-301X; Koekemoer, Anton/0000-0002-6610-2048; Perez Montero, E/0000-0003-3985-4882; Brusa, Marcella/0000-0002-5059-6848; Iovino, Angela/0000-0001-6958-0304; bottini, dario/0000-0001-6917-041X; Pozzetti, Lucia/0000-0001-7085-0412; Bongiorno, Angela/0000-0002-0101-6624; Scodeggio, Marco/0000-0002-2282-5850; Franzetti, Paolo/0000-0002-6986-0127; Vergani, Daniela/0000-0003-0898-2216; Scaramella, Roberto/0000-0003-2229-193X; Lanzuisi, Giorgio/0000-0001-9094-0984; Kneib, Jean-Paul/0000-0002-4616-4989; Cappi, Alberto/0000-0002-9200-7167; Zucca, Elena/0000-0002-5845-8132; Bardelli, Sandro/0000-0002-8900-0298; Mignoli, Marco/0000-0002-9087-2835; Bolzonella, Micol/0000-0003-3278-4607; FU INAF [PRIN/2007/1.06.10.08]; ASI [ASI/COFIS/WP3110 I/026/07/0]; NASA [ADP NNX07AT02G]; CONACyT [83564]; ESA Member States; USA (NASA); [175]; [A-0839]; [PAPIITIN110209] FX A. B. wishes to thank the referee for the useful suggestions that significantly improved the manuscript. A. B. also thank H. Netzer for the the stimulating discussion, R. Fassbender for helping to improve the manuscript and S. Savaglio for sharing the expertise. This work is based on the zCOSMOS ESO Large Program Number 175. A-0839 and was supported by an INAF contract PRIN/2007/1.06.10.08, and an ASI grant ASI/COFIS/WP3110 I/026/07/0, Partial support of this work is provided by NASA ADP NNX07AT02G, CONACyT 83564, and PAPIITIN110209. These results are also based in part on observations obtained with XMM-Newton, an ESA Science Mission with instruments and contributions directly funded by ESA Member States and the USA (NASA). NR 86 TC 36 Z9 36 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 FEB PY 2010 VL 510 AR A56 DI 10.1051/0004-6361/200913229 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 574RB UT WOS:000276009100014 ER PT J AU Palau, A Sanchez-Monge, A Busquet, G Estalella, R Zhang, Q Ho, PTP Beltran, MT Beuther, H AF Palau, Aina Sanchez-Monge, A. Busquet, G. Estalella, R. Zhang, Q. Ho, P. T. P. Beltran, M. T. Beuther, H. TI Three intermediate-mass young stellar objects with different properties emerging from the same natal cloud in IRAS 00117+6412 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: formation; dust, extinction; HII regions; ISM: individual objects: IRAS 00117+6412; radio continuum: ISM ID PROTOSTELLAR CANDIDATES; STAR-FORMATION; CO OUTFLOWS; MOLECULAR OUTFLOWS; PRESTELLAR CORE; MAIN-SEQUENCE; EVOLUTION; CLUSTER; REGION; N2H+ AB Aims. Our main aim is to study the influence of the initial conditions of a cloud in the intermediate/high-mass star formation process. Methods. We observed with the VLA, PdBI, and SMA the centimeter and millimeter continuum, N2H+ (1-0), and CO(2-1) emission associated with a dusty cloud harboring a nascent cluster with intermediate-mass protostars. Results. At centimeter wavelengths we found a strong source, tracing a UCHII region, at the eastern edge of the dusty cloud, with a shell-like structure, and with the near-infrared counterpart falling in the center of the shell. This is presumably the most massive source of the forming cluster. About 15 '' to the west of the UCHII region and well embedded in the dusty cloud, we detected a strong millimeter source, MM1, associated with centimeter and near-infrared emission. MM1 seems to be driving a prominent high-velocity CO bipolar outflow elongated in the northeast-southwest direction, and is embedded in a ridge of dense gas traced by N2H+, elongated roughly in the same direction as the outflow. We estimated that MM1 is an intermediate-mass source in the Class 0/I phase. About 15 '' to the south of MM1, and still more deeply embedded in the dusty cloud, we detected a compact millimeter source, MM2, with neither centimeter nor near-infrared emission, but with water maser emission. MM2 is associated with a clump of N2H+, whose kinematics reveal a clear velocity gradient and additionally we found signposts of infall motions. MM2, being deeply embedded within the dusty cloud, with an associated water maser but no hints of CO outflow emission, is an intriguing object, presumably of intermediate mass. Conclusions. The UCHII region is found at the border of a dusty cloud which is currently undergoing active star formation. Two intermediate-mass protostars in the dusty cloud seem to have formed after the UCHII region and have different properties related to the outflow phenomenon. Thus, a single cloud with similar dust emission and similar dense gas column densities seems to be forming objects with different properties, suggesting that the initial conditions in the cloud are not determining all the star formation process. C1 [Palau, Aina] INTA CSIC, Ctr Astrobiol, Lab Astrofis Estelar & Exoplanetas, Madrid 28691, Spain. [Sanchez-Monge, A.; Busquet, G.; Estalella, R.] Univ Barcelona, Dept Astron & Meteorol IEEC UB, Inst Ciencies Cosmos, E-08028 Barcelona, Spain. [Zhang, Q.; Ho, P. T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ho, P. T. P.] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. [Beltran, M. T.] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. [Beuther, H.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. RP Palau, A (reprint author), INTA CSIC, Ctr Astrobiol, Lab Astrofis Estelar & Exoplanetas, LAEFF Campus,POB 78, Madrid 28691, Spain. EM palau@ieec.uab.es OI Beltran Sorolla, Maria Teresa/0000-0003-3315-5626; Zhang, Qizhou/0000-0003-2384-6589 FU MICINN [ESP2007-65475C02- 02]; La Comunidad de Madrid [ASTRID S0505/ESP-0361]; Europan Social Fund; Spanish MICINN [CSD2006-00070, AYA2005-08523-C03, AYA2008-06189-C03]; National Aeronautics and Space Administration; National Science Foundation FX A. P. is grateful to Itziar de Gregorio-Monsalvo for useful discussions. A. P. is partially supported by the MICINN grant ESP2007-65475C02- 02, the program ASTRID S0505/ESP-0361 from La Comunidad de Madrid and the Europan Social Fund, and the Spanish MICINN under the ConsoliderIngenio 2010 Program grant CSD2006-00070. A. P., A. S.-M., G. B. and R. E. are supported by the Spanish MICINN grant AYA2005-08523-C03, and the MICINN grant AYA2008-06189-C03 (co-funded with FEDER funds). 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 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 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2010 VL 510 AR A5 DI 10.1051/0004-6361/200913215 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 552PI UT WOS:000274305100006 ER PT J AU Papadakis, IE Brinkmann, W Gliozzi, M Raeth, C Nicastro, F Conciatore, ML AF Papadakis, I. E. Brinkmann, W. Gliozzi, M. Raeth, C. Nicastro, F. Conciatore, M. L. TI XMM-Newton long-look observation of the narrow line Seyfert 1 galaxy PKS 0558-504 I. Spectral analysis SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: active; galaxies: Seyfert; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; X-RAY VARIABILITY; QUASAR PKS-0558-504; ACCRETION FLOW; BLACK-HOLES; EMISSION; MODELS; AGN; COMPTONIZATION; MCG-6-30-15 AB Context. PKS 0558-504 has been observed repeatedly by XMM-Newton as a calibration and performance verification (PV) target. In this work, we present results from the spectral analysis of a long XMM-Newton observation of the radio loud Narrow Line Seyfert 1 galaxy PKS 0558-504. Aims. To study the soft excess component in this object, the spectral variations it exhibits in both the hard and soft X-ray bands, and their correlation. Methods. We used mainly the PN data, and we fitted various spectral models to the time average spectra of the individual orbits as well as the spectra from data segments of shorter duration. We also used the RGS data to search for signs of a warm absorber in the source. Results. The source is highly variable, on all sampled time scales. We did not observe any absorption features in either the soft or hard band. We found weak evidence for the presence of an iron line at similar to 6.8 keV, which is indicative of emission from highly ionized iron. The 2-10 keV band spectrum of the source is well fitted by a simple power law model, whose slope steepens with increasing flux, similar to what is observed in other Seyferts as well. The soft excess is variable both in flux and shape, and it can be well described by a low-temperature Comptonisation model, whose slope flattens with increasing flux. Finally, the soft excess flux variations are moderately correlated with the hard band variations, and we found weak evidence that they are leading them by similar to 20 ks. Conclusions. Our results rule out a jet origin for the bulk of the X-ray emission in this object. We found no signals of a warm absorber. The observed hard band spectral variations suggest intrinsic continuum slope variations, caused by changes in the "heating/cooling" ratio of the hot corona. The low-temperature Comptonising medium, responsible for the soft excess emission, could be a hot layer in the inner disc of the source, which appears due to the fact that the source is accreting at a super-Eddington rate. The soft excess flux and spectral variations could be caused by random variations of the accretion rate. C1 [Papadakis, I. E.] Univ Crete, Dept Phys, Iraklion 71003, Crete, Greece. [Papadakis, I. E.; Nicastro, F.] Fdn Res & Technol Hellas, IESL, Iraklion 71110, Crete, Greece. [Brinkmann, W.; Raeth, C.] Max Planck Inst Extraterr Phys, D-85740 Garching, Germany. [Gliozzi, M.] George Mason Univ, Dept Phys & Astron, Fairfax, VA 22030 USA. [Nicastro, F.] INAF, Osservatorio Astron Roma, Rome, Italy. [Nicastro, F.; Conciatore, M. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Papadakis, IE (reprint author), Univ Crete, Dept Phys, POB 2208, Iraklion 71003, Crete, Greece. EM jhep@physics.uoc.gr RI Papadakis, Iossif/C-3235-2011; OI Nicastro, Fabrizio/0000-0002-6896-1364 FU EU ToK [39965, FP7-REGPOT 206469]; NASA [201593]; ESA Member States; USA (NASA) FX I. E. and W. P. B. acknowledge partial support from the EU ToK grant 39965 and FP7-REGPOT 206469. M. G. acknowledges support by the XMM-Newton Guest Investigator Program under NASA grant 201593. This work is based on observations with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and the USA (NASA). This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 50 TC 8 Z9 8 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 FEB PY 2010 VL 510 AR A65 DI 10.1051/0004-6361/200913289 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 574RB UT WOS:000276009100018 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 Brusa, M Capak, P Caputi, K Carollo, CM Civano, F Elvis, M Faure, C Hasinger, G Koekemoer, AM Lee, N Lilly, S Liu, CT McCracken, HJ Schinnerer, E Smolcic, V Taniguchi, Y Thompson, DJ Trump, J 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. Brusa, M. Capak, P. Caputi, K. Carollo, C. M. Civano, F. Elvis, M. Faure, C. Hasinger, G. Koekemoer, A. M. Lee, N. Lilly, S. Liu, C. T. McCracken, H. J. Schinnerer, E. Smolcic, V. Taniguchi, Y. Thompson, D. J. Trump, J. TI A MULTIWAVELENGTH STUDY OF A SAMPLE OF 70 mu m SELECTED GALAXIES IN THE COSMOS FIELD. I. SPECTRAL ENERGY DISTRIBUTIONS AND LUMINOSITIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; galaxies: active; galaxies: evolution; galaxies: high-redshift; infrared: galaxies; surveys ID ULTRALUMINOUS INFRARED GALAXIES; ACTIVE GALACTIC NUCLEUS; STAR-FORMING GALAXIES; SPITZER-SPACE-TELESCOPE; HIGH-REDSHIFT GALAXIES; 1ST-LOOK SURVEY; SOURCE CATALOG; OPTICAL SPECTROSCOPY; RADIO PROPERTIES; NEARBY GALAXIES AB We present a large robust sample of 1503 reliable and unconfused 70 mu m selected sources from the multiwavelength data set of the Cosmic Evolution Survey. Using the Spitzer IRAC and MIPS photometry, we estimate the total infrared (IR) luminosity, L(IR) (8-1000 mu m), by finding the best-fit template from several different template libraries. The long-wavelength 70 and 160 mu m data allow us to obtain a reliable estimate of L(IR), accurate to within 0.2 and 0.05 dex, respectively. The 70 mu m data point enables a significant improvement over the luminosity estimates possible with only a 24 mu m detection. The full sample spans a wide range in IR luminosity, L(IR) approximate to 10(8)-10(14) L(circle dot), with a median luminosity of 10(11.4) L(circle dot). We identify a total of 687 luminous, 303 ultraluminous, and 31 hyperluminous infrared galaxies (LIRGs, ULIRGs, and HyLIRGs) over the redshift range 0.01 < z < 3.5 with a median redshift of 0.5. Presented here are the full spectral energy distributions (SEDs) for each of the sources compiled from the extensive multiwavelength data set from the ultraviolet (UV) to the far-infrared. A catalog of the general properties of the sample (including the photometry, redshifts, and L(IR)) is included with this paper. We find that the overall shape of the SED and trends with L(IR) (e.g., IR color temperatures and optical-IR ratios) are similar to what has been seen in studies of local objects; however, our large sample allows us to see the extreme spread in UV to near-infrared colors spanning nearly 3 orders of magnitude. In addition, using SED fits we find possible evidence for a subset of cooler ultraluminous objects than observed locally. However, until direct observations at longer wavelengths are obtained, the peak of emission and the dust temperature cannot be well constrained. We use these SEDs, along with the deep radio and X-ray coverage of the field, to identify a large sample of candidate active galactic nuclei (AGNs). We find that the fraction of AGNs increases strongly with L(IR), as it does in the local universe, and that nearly 70% of ULIRGs and all HyLIRGs likely host a powerful AGN. C1 [Frayer, D. T.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Aussel, H.] Univ Paris 07, CNRS, CEA, AIM Unite Mixte Rech,UMR 7158, F-91191 Gif Sur Yvette, France. [Arnouts, S.] Canada France Hawaii Telescope Corp, Kamuela, HI 96743 USA. [Ilbert, O.] Lab Astrophys Marseille, F-13376 Marseille 12, France. [Surace, J.; Yan, L.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Brusa, M.; Hasinger, G.] Max Planck Inst Extraterr Phys, D-85478 Garching, Germany. [Caputi, K.; Carollo, C. M.; Lilly, S.] ETH, Dept Phys, CH-8093 Zurich, Switzerland. [Civano, F.; Elvis, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Faure, C.] Observ Sauverny, EPFL, Astrophys Lab, CH-1290 Versoix, Switzerland. [Koekemoer, A. M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Liu, C. T.] CUNY Coll Staten Isl, Astrophys Observ, Staten Isl, NY 10314 USA. [McCracken, H. J.] Univ Paris 06, CNRS, UMR7095, Inst Astrophys Paris, F-75014 Paris, France. [Schinnerer, E.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Taniguchi, Y.] Ehime Univ, Grad Sch Sci, Dept Phys, 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. [Kartaltepe, Jeyhan S.; Sanders, D. B.; Le Floc'h, E.; Ilbert, O.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. RP Kartaltepe, JS (reprint author), Natl Opt Astron Observ, 950 N Cherry Ave, Tucson, AZ 85719 USA. EM jeyhan@ifa.hawaii.edu OI Koekemoer, Anton/0000-0002-6610-2048 FU NASA [1282612, 1298213, 1344920]; NSF [AST-0071048]; Alfred P. Sloan Foundation; Participating Institutions; National Science Foundation; U.S. Department of Energy; National Aeronautics and Space Administration; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England FX Support for this work was provided in part by NASA through contracts 1282612, 1298213, and 1344920 issued by the Jet Propulsion Laboratory. 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 multiwavelength 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/. NR 88 TC 60 Z9 60 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 FEB 1 PY 2010 VL 709 IS 2 BP 572 EP 596 DI 10.1088/0004-637X/709/2/572 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 543LT UT WOS:000273579800003 ER PT J AU Dunn, JP Bautista, M Arav, N Moe, M Korista, K Costantini, E Benn, C Ellison, S Edmonds, D AF Dunn, Jay P. Bautista, Manuel Arav, Nahum Moe, Max Korista, Kirk Costantini, Elisa Benn, Chris Ellison, Sara Edmonds, Doug TI THE QUASAR OUTFLOW CONTRIBUTION TO AGN FEEDBACK: VLT MEASUREMENTS OF SDSS J0318-0600 SO ASTROPHYSICAL JOURNAL LA English DT Article DE quasars: absorption lines; quasars: individual (SDSS J0318-0600) ID DIGITAL SKY SURVEY; ABSORPTION-LINE QUASARS; SPACE-TELESCOPE OBSERVATIONS; KECK HIRES OBSERVATIONS; FE-II; BLACK-HOLES; DATA RELEASE; INTRINSIC ABSORPTION; GASEOUS NEBULAE; COLLISION STRENGTHS AB We present high spectral resolution Very Large Telescope observations of the broad absorption line quasar SDSS J0318-0600. This high-quality data set allows us to extract accurate ionic column densities and determine an electron number density of n(e) = 10(3.3 +/- 0.2) cm(-3) for the main outflow absorption component. The heavily reddened spectrum of SDSS J0318-0600 requires purely silicate dust with a reddening curve characteristic of predominately large grains, from which we estimate the bolometric luminosity. We carry out photoionization modeling to determine the total column density, ionization parameter, and distance of the gas and find that the photoionization models suggest abundances greater than solar. Due to the uncertainty in the location of the dust extinction, we arrive at two viable distances for the main ouflow component from the central source, 6 and 17 kpc, where we consider the 6 kpc location as somewhat more physically plausible. Assuming the canonical global covering of 20% for the outflow and a distance of 6 kpc, our analysis yields a mass flux of 120 M(circle dot) yr(-1) and a kinetic luminosity that is similar to 0.1% of the bolometric luminosity of the object. Should the dust be part of the outflow, then these values are similar to 4x larger. The large mass flux and kinetic luminosity make this outflow a significant contributor to active galactic nucleus feedback processes. C1 [Dunn, Jay P.; Bautista, Manuel; Arav, Nahum; Edmonds, Doug] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA. [Bautista, Manuel; Korista, Kirk] Western Michigan Univ, Dept Phys, Kalamazoo, MI 49008 USA. [Moe, Max] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Moe, Max] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Moe, Max] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Costantini, Elisa] SRON Natl Inst Space Res, NL-3584 CA Utrecht, Netherlands. [Benn, Chris] Isaac Newton Grp, E-38700 Santa Cruz De La Palma, Spain. [Ellison, Sara] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 1A1, Canada. RP Dunn, JP (reprint author), Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA. EM jdunn77@vt.edu; manuel.bautista@wmich.edu; arav@vt.edu; mmoe@cfa.harvard.edu; kirk.korista@wmich.edu; edmonds@vt.edu FU NSF [AST 0507772]; NASA [NAG5-12867, NNX09AB99G] FX We acknowledge support from NSF grant AST 0507772 and from NASA LTSA grant NAG5-12867. M.A.B. received partial support for this work from the NASA Award No. NNX09AB99G. NR 93 TC 109 Z9 110 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 FEB 1 PY 2010 VL 709 IS 2 BP 611 EP 631 DI 10.1088/0004-637X/709/2/611 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 543LT UT WOS:000273579800006 ER PT J AU Eze, RNC Luna, GJM Smith, RK AF Eze, R. N. C. Luna, G. J. M. Smith, R. K. TI HIGH-RESOLUTION X-RAY SPECTRA OF THE SYMBIOTIC STAR SS73 17 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; binaries: symbiotic; line: formation ID HELIUM-LIKE IONS; WHITE-DWARFS; EMISSION; DIAGNOSTICS; ACCRETION; CATALOG; WIND AB SS73 17 was an innocuous Mira-type symbiotic star until the International Gamma-Ray Astrophysics Laboratory and Swift discovered its bright hard X-ray emission, adding it to the small class of "hard X-ray emitting symbiotics." Suzaku observations in 2006 then showed it emits three bright iron lines as well, with little to no emission in the 0.3-2.0 keV bandpass. We present here follow-up observations with the Chandra High Energy Transmission Grating and Suzaku that confirm the earlier detection of strong emission lines of Fe K alpha fluorescence, Fe XXV and Fe XXVI but also show significantly more soft X-ray emission. The high-resolution spectrum also shows emission lines of other highly ionized ions as Si XIV and possibly S XVI. In addition, a re-analysis of the 2006 Suzaku data using the latest calibration shows that the hard (15-50 keV) X-ray emission is brighter than previously thought and remains constant in both the 2006 and 2008 data. The G ratio calculated from the Fe xxv lines shows that these lines are thermal, not photoionized, in origin. With the exception of the hard X-ray emission, the spectra from both epochs can be fit using thermal radiation assuming a differential emission measure based on a cooling-flow model combined with a full and partial absorber. We show that acceptable fits can be obtained for all the data in the 1-10 keV band varying only the partial absorber. Based on the temperature and accretion rate, the thermal emission appears to be arising from the boundary layer between the accreting white dwarf and the accretion disk. C1 [Eze, R. N. C.; Luna, G. J. M.; Smith, R. K.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Eze, R. N. C.] Univ Nigeria, Nsukka, Enugu, Nigeria. RP Eze, RNC (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM reze@head.cfa.harvard.edu RI XRAY, SUZAKU/A-1808-2009 FU Chandra [GO8-9032X] FX We gratefully acknowledge helpful discussions with Koji Mukai, Norbert Schulz, David Huenemoerder, Richard Mushotzky, Tim Kallman, and Scott Kenyon. Financial support for this work was made possible by Chandra grant GO8-9032X. NR 26 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 FEB 1 PY 2010 VL 709 IS 2 BP 816 EP 822 DI 10.1088/0004-637X/709/2/816 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 543LT UT WOS:000273579800022 ER PT J AU Geller, MJ Kurtz, MJ Dell'Antonio, IP Ramella, M Fabricant, DG AF Geller, Margaret J. Kurtz, Michael J. Dell'Antonio, Ian P. Ramella, Massimo Fabricant, Daniel G. TI SHELS: TESTING WEAK-LENSING MAPS WITH REDSHIFT SURVEYS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: individual (CXOU J091551+293637, CXOU J091554+293316, CXOU J091601+292750, XMMU J091935+303155, A781, CXOU J09202+302938, CXOU J092053+302800, CXOU J092110+302751); galaxies: distances and redshifts; gravitational lensing: weak; large-scale structure of universe ID FIBER-FED SPECTROGRAPH; DIGITAL SKY SURVEY; DARK-MATTER HALOS; GALAXY CLUSTERS; PHOTOMETRIC REDSHIFTS; LUMINOSITY FUNCTION; MASS PROFILES; DEEP; HECTOSPEC; CATALOG AB Weak-lensing surveys are emerging as an important tool for the construction of "mass-selected" clusters of galaxies. We evaluate both the efficiency and completeness of a weak-lensing selection by combining a dense, complete redshift survey, the Smithsonian Hectospec Lensing Survey (SHELS), with a weak-lensing map from the Deep Lens Survey (DLS). SHELS includes 11,692 redshifts for galaxies with R <= 20.6 in the 4 deg(2) DLS field; the survey is a solid basis for identifying massive clusters of galaxies with redshift z less than or similar to 0.55. The range of sensitivity of the redshift survey is similar to the range for the DLS convergence map. Only four of the 12 convergence peaks with signal to noise >= 3.5 correspond to clusters of galaxies with M greater than or similar to 1.7 x 10(14) M(circle dot). Four of the eight massive clusters in SHELS are detected in the weak-lensing map yielding a completeness of similar to 50%. We examine the seven known extended cluster X-ray sources in the DLS field: three can be detected in the weak-lensing map, three should not be detected without boosting from superposed large-scale structure, and one is mysteriously undetected even though its optical properties suggest that it should produce a detectable lensing signal. Taken together, these results underscore the need for more extensive comparisons among different methods of massive cluster identification. C1 [Geller, Margaret J.; Kurtz, Michael J.; Fabricant, Daniel G.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Dell'Antonio, Ian P.] Brown Univ, Dept Phys, Providence, RI 02912 USA. [Ramella, Massimo] Osserv Astron Trieste, INAF, I-34131 Trieste, Italy. RP Geller, MJ (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM mgeller@cfa.harvard.edu; mkurtz@cfa.harvard.edu; ian@het.brown.edu; ramella@oats.inaf.it; dfabricant@cfa.harvard.edu RI KURTZ, Michael /B-3890-2009; OI Ramella, Massimo/0000-0001-5446-4749; Kurtz, Michael/0000-0002-6949-0090 FU Smithsonian Institution; Lucent Technologies; NSF [AST 04-41-72, AST 01-34753, AST-0708433] FX We thank P. Berlind and M. Calkins for their expert operation of the Hectospec. D. Mink, J. Roll, S. Tokarz, and W. Wyatt constructed and ran the Hectospec pipeline. We thank H. Khiabanian and J. Kubo for guidance in using the DLS convergence maps. We thank the anonymous referee for insightful, careful, gracious comments that inspired us to improve the paper. We also thank S. Kenyon and M. Zaldarriaga for many insightful discussions. The Smithsonian Institution generously supported Hectospec and SHELS. Lucent Technologies and NSF grants AST 04-41-72 and AST 01-34753 generously supported the DLS. We appreciate generous allocations of telescope time on the Kitt Peak National Observatory 4 m telescope and on the MMT. I. Dell'Antonio is supported by NSF-AST grant AST-0708433. NR 48 TC 30 Z9 30 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 FEB 1 PY 2010 VL 709 IS 2 BP 832 EP 850 DI 10.1088/0004-637X/709/2/832 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 543LT UT WOS:000273579800024 ER PT J AU Sehgal, N Bode, P Das, S Hernandez-Monteagudo, C Huffenberger, K Lin, YT Ostriker, JP Trac, H AF Sehgal, Neelima Bode, Paul Das, Sudeep Hernandez-Monteagudo, Carlos Huffenberger, Kevin Lin, Yen-Ting Ostriker, Jeremiah P. Trac, Hy TI SIMULATIONS OF THE MICROWAVE SKY SO ASTROPHYSICAL JOURNAL LA English DT Review DE cosmic microwave background; galaxies: clusters: general; galaxies: general; intergalactic medium; large-scale structure of universe; methods: N-body simulations ID HOT INTERGALACTIC MEDIUM; ZELDOVICH EFFECT SURVEYS; LARGE-SCALE STRUCTURE; TREE PARTICLE-MESH; DEEP FIELD-SOUTH; GALAXY CLUSTERS; RADIO-SOURCES; SOURCE COUNTS; POWER SPECTRUM; 1.4 GHZ AB We create realistic, full-sky, half-arcminute resolution simulations of the microwave sky matched to the most recent astrophysical observations. The primary purpose of these simulations is to test the data reduction pipeline for the Atacama Cosmology Telescope (ACT) experiment; however, we have widened the frequency coverage beyond the ACT bands and utilized the easily accessible HEALPix map format to make these simulations applicable to other current and near future microwave background experiments. Some of the novel features of these simulations are that the radio and infrared galaxy populations are correlated with the galaxy cluster and group populations, the primordial microwave background is lensed by the dark matter structure in the simulation via a ray-tracing code, the contribution to the thermal and kinetic Sunyaev-Zel'dovich (SZ) signals from galaxy clusters, groups, and the intergalactic medium has been included, and the gas prescription to model the SZ signals has been refined to match the most recent X-ray observations. The cosmology adopted in these simulations is also consistent with the WMAP 5-year parameter measurements. From these simulations we find a slope for the Y-200-M-200 relation that is only slightly steeper than self-similar, with an intrinsic scatter in the relation of similar to 14%. Regarding the contamination of cluster SZ flux by radio galaxies, we find for 148 GHz (90 GHz) only 3% (4%) of halos have their SZ decrements contaminated at a level of 20% or more. We find the contamination levels higher for infrared galaxies. However, at 90 GHz, less than 20% of clusters with M-200 > 2.5 x 10(14) M-circle dot and z < 1.2 have their SZ decrements filled in at a level of 20% or more. At 148 GHz, less than 20% of clusters with M-200 > 2.5 x 10(14) M-circle dot and z < 0.8 have their SZ decrements filled in at a level of 50% or larger. Our models also suggest that a population of very high flux infrared galaxies, which are likely lensed sources, contribute most to the SZ contamination of very massive clusters at 90 and 148 GHz. These simulations are publicly available and should serve as a useful tool for microwave surveys to cross-check SZ cluster detection, power spectrum, and cross-correlation analyses. C1 [Sehgal, Neelima] Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Bode, Paul; Das, Sudeep; Ostriker, Jeremiah P.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Das, Sudeep] Princeton Univ, Dept Phys, Princeton, NJ 08540 USA. [Hernandez-Monteagudo, Carlos] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Huffenberger, Kevin] Univ Miami, Dept Phys, Coral Gables, FL 33146 USA. [Lin, Yen-Ting] Univ Tokyo, Inst Phys & Math Universe, Tokyo 1138654, Japan. [Trac, Hy] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Sehgal, N (reprint author), Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. RI Trac, Hy/N-8838-2014; OI Trac, Hy/0000-0001-6778-3861; Huffenberger, Kevin/0000-0001-7109-0099 FU U. S. Department of Energy [DE-AC3-76SF00515]; NSF [0707731, AST070015, OISE/0530095]; NASA ATP [NNX08AH30G]; World Premier International Research Center Initiative, MEXT, Japan; Institute for Theory and Computation Fellowship; Princeton Institute for Computational Science and Engineering and the Princeton University Office of Information Technology; PIRE FX N. S. thanks Steve Allen, Olivier Dore, Joanna Dunkley, Joe Fowler, Gil Holder, Andrew Lawrence, Toby Marriage, Danica Marsden, Lyman Page, and David Spergel for useful discussions. S. D. thanks David Spergel, Chris Hirata, Paul Bode, and Hy Trac for help and guidance during the development of the original lensing code. C. H. M. is grateful to R. E. Smith for insightful comments on the power spectrummodeling. H. T. thanks Kavi Moodley and Ryan Warne for helpful discussions. N. S. is supported by the U. S. Department of Energy contract to SLAC no. DE-AC3-76SF00515. P. B. was partially supported by NSF grant 0707731. S. D. acknowledges support from NASA ATP grant NNX08AH30G. Y. T. L. acknowledges support from the World Premier International Research Center Initiative, MEXT, Japan. H. T. is supported by the Institute for Theory and Computation Fellowship. Computer simulations and analysis were supported by the National Science Foundation through TeraGrid resources provided by the Pittsburgh Supercomputing Center and the National Center for Supercomputing Applications under grant AST070015; computations were also performed at the TIGRESS high performance computer center at Princeton University, which is jointly supported by the Princeton Institute for Computational Science and Engineering and the Princeton University Office of Information Technology. We acknowledge support from the PIRE program and NSF grant OISE/0530095. Some of the results in this paper have been derived using the HEALPix package (Gorski et al. 2005). We also 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 110 TC 102 Z9 102 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 FEB 1 PY 2010 VL 709 IS 2 BP 920 EP 936 DI 10.1088/0004-637X/709/2/920 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 543LT UT WOS:000273579800029 ER PT J AU D'Onghia, E Springel, V Hernquist, L Keres, D AF D'Onghia, Elena Springel, Volker Hernquist, Lars Keres, Dusan TI SUBSTRUCTURE DEPLETION IN THE MILKY WAY HALO BY THE DISK SO ASTROPHYSICAL JOURNAL LA English DT Article DE dark matter; Galaxy: disk; Galaxy: formation ID DARK-MATTER SUBSTRUCTURE; HIERARCHICAL TREE METHOD; GROUP DWARF SPHEROIDALS; LOCAL GROUP; SINKING SATELLITES; DENSITY PROFILES; GALAXIES; SIMULATIONS; EVOLUTION; RESOLUTION AB We employ numerical simulations and simple analytical estimates to argue that dark matter substructures orbiting in the inner regions of the Galaxy can be efficiently destroyed by disk shocking, a dynamical process known to affect globular star clusters. We carry out a set of fiducial high-resolution collisionless simulations in which we adiabatically grow a disk, allowing us to examine the impact of the disk on the substructure abundance. We also track the orbits of dark matter satellites in high-resolution Aquarius simulations and analytically estimate the cumulative halo and disk-shocking effect. Our calculations indicate that the presence of a disk with only 10% of the total Milky Way mass can significantly alter the mass function of substructures in the inner parts of halos. This has important implications especially for the relatively small number of satellites seen within similar to 30 kpc of the Milky Way center, where disk shocking is expected to reduce the substructure abundance by a factor of 2 at 10(9) M(circle dot) and a factor of 3 at 10(7) M(circle dot). The most massive subhalos with 10(10) M(circle dot) survive even in the presence of the disk. This suggests that there is no inner missing satellite problem and calls into question whether these substructures can produce transient features in disks, like multi-armed spiral patterns. Also, the depletion of dark matter substructures through shocking on the baryonic structures of the disk and central bulge may aggravate the problem to fully account for the observed flux anomalies in gravitational lens systems, and significantly reduces the dark matter annihilation signal expected from nearby substructures in the inner halo. C1 [D'Onghia, Elena; Hernquist, Lars; Keres, Dusan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [D'Onghia, Elena] Univ Zurich, Inst Theoret Phys, CH-8057 Zurich, Switzerland. [Springel, Volker] Max Planck Inst Astrophys, D-85740 Garching, Germany. RP D'Onghia, E (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM edonghia@cfa.harvard.edu OI Springel, Volker/0000-0001-5976-4599 FU EU [MEIF-041569]; ITC FX This research was partly supported by the EU Marie Curie Intra-European Fellowship under contract MEIF-041569. D. K. acknowledges support by the ITC fellowship. Numerical simulations were performed on the Odyssey supercomputer at Harvard University. The simulations of the Aquarius project were carried out at the Leibniz Computing Center and the Computing Center of the Max-Planck-Society in Garching, Germany. NR 53 TC 71 Z9 71 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 FEB 1 PY 2010 VL 709 IS 2 BP 1138 EP 1147 DI 10.1088/0004-637X/709/2/1138 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 543LT UT WOS:000273579800045 ER PT J AU Yeates, AR Attrill, GDR Nandy, D Mackay, DH Martens, PCH van Ballegooijen, AA AF Yeates, A. R. Attrill, G. D. R. Nandy, Dibyendu Mackay, D. H. Martens, P. C. H. van Ballegooijen, A. A. TI COMPARISON OF A GLOBAL MAGNETIC EVOLUTION MODEL WITH OBSERVATIONS OF CORONAL MASS EJECTIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: corona; Sun: coronal mass ejections (CMEs); Sun: evolution; Sun: magnetic topology ID SOLAR ACTIVE-REGION; FILAMENT CHANNELS; HEMISPHERIC PATTERN; NULL POINTS; FLUX ROPES; FIELDS; SUN; SIMULATIONS; PROMINENCES; CHIRALITY AB The relative importance of different initiation mechanisms for coronal mass ejections (CMEs) on the Sun is uncertain. One possible mechanism is the loss of equilibrium of coronal magnetic flux ropes formed gradually by large-scale surface motions. In this paper, the locations of flux rope ejections in a recently developed quasi-static global evolution model are compared with observed CME source locations over a 4.5 month period in 1999. Using extreme ultraviolet data, the low-coronal source locations are determined unambiguously for 98 out of 330 CMEs. An alternative method of determining the source locations using recorded Ha events was found to be too inaccurate. Despite the incomplete observations, positive correlation (with coefficient up to 0.49) is found between the distributions of observed and simulated ejections, but only when binned into periods of 1 month or longer. This binning timescale corresponds to the time interval at which magnetogram data are assimilated into the coronal simulations, and the correlation arises primarily from the large-scale surface magnetic field distribution; only a weak dependence is found on the magnetic helicity imparted to the emerging active regions. The simulations are limited in two main ways: they produce fewer ejections, and they do not reproduce the strong clustering of observed CME sources into active regions. Due to this clustering, the horizontal gradient of radial photospheric magnetic field is better correlated with the observed CME source distribution (coefficient 0.67). Our results suggest that while the gradual formation of magnetic flux ropes over weeks can account for many observed CMEs, especially at higher latitudes, there exists a second class of CMEs (at least half) for which dynamic active region flux emergence on shorter timescales must be the dominant factor. Improving our understanding of CME initiation in future will require both more comprehensive observations of CME source regions and more detailed magnetic field simulations. C1 [Yeates, A. R.; Attrill, G. D. R.; Martens, P. C. H.; van Ballegooijen, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Nandy, Dibyendu] Indian Inst Sci Educ & Res, Dept Phys Sci, Mohanpur 741252, W Bengal, India. [Mackay, D. H.] 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; gattrill@cfa.harvard.edu; dnandi@iiserkol.ac.in; duncan@mcs.st-and.ac.uk; pmartens@cfa.harvard.edu; vanballe@cfa.harvard.edu RI Yeates, Anthony/D-1338-2014 OI Yeates, Anthony/0000-0002-2728-4053 FU NASA/LWS [NNG05GK32G, NNM07AB07C]; NASA/ROSES [NNX09AB11G]; Department of Science and Technology of the Government of India; SRIF/STFC; Royal Society FX We thank M.J. Wills-Davey for useful suggestions. A.R.Y. was supported by NASA/LWS grant NNG05GK32G and contract NNM07AB07C to SAO. G. D. R. A. acknowledges the NASA/ROSES grant NNX09AB11G, and D.N. support from the Department of Science and Technology of the Government of India through the Ramanujan Fellowship. Simulations used the UKMHD parallel computer in St. Andrews ( funded jointly by SRIF/STFC), and support from the Royal Society through a research grant to D. H. M. We acknowledge the use of data from the LASCO and EIT consortia (SOHO is a project of international cooperation between ESA and NASA), and of the online EIT MPEG Movies Archive maintained by F. Auchere. The CDAW CME catalog is generated and maintained at the CDAW Data Center by NASA and The Catholic University of America in cooperation with the Naval Research Laboratory. The Solar Geophysical Database is maintained by NOAA and made available courtesy of the Solar-Terrestrial Physics Division. Synoptic magnetogram data from NSO/Kitt Peak were produced cooperatively by NSF/NOAO, NASA/GSFC, and NOAA/SEL, and made available on the World Wide Web. NR 73 TC 17 Z9 17 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2010 VL 709 IS 2 BP 1238 EP 1248 DI 10.1088/0004-637X/709/2/1238 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 543LT UT WOS:000273579800054 ER PT J AU Tommasin, S Spinoglio, L Malkan, MA Fazio, G AF Tommasin, Silvia Spinoglio, Luigi Malkan, Matthew A. Fazio, Giovanni TI SPITZER-IRS HIGH-RESOLUTION SPECTROSCOPY OF THE 12 mu m SEYFERT GALAXIES. II. RESULTS FOR THE COMPLETE DATA SET SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: starburst; infrared: galaxies ID ACTIVE GALACTIC NUCLEI; ULTRALUMINOUS INFRARED GALAXIES; SPECTRAL ENERGY-DISTRIBUTIONS; EMISSION-LINE SPECTRA; SPACE-TELESCOPE; OPTICAL SPECTROSCOPY; STARBURST GALAXIES; X-RAY; MOLECULAR-HYDROGEN; SPIRAL GALAXIES AB We present our Spitzer-Infrared Spectrometer (IRS) spectroscopic survey from 10 mu m to 37 mu m of the Seyfert galaxies of the 12 mu m Galaxy Sample, collected in a high-resolution mode (R similar to 600). The new spectra of 61 galaxies, together with the data we already published, give us a total of 91 12 mu m Seyfert galaxies observed, out of 112. We discuss the mid-IR emission lines and features of the Seyfert galaxies, using an improved active galactic nucleus (AGN) classification scheme: instead of adopting the usual classes of Seyfert 1's and Seyfert 2's, we use the spectropolarimetric data from the literature to divide the objects into categories "AGN 1" and "AGN 2," where AGN 1's include all broad-line objects, including the Seyfert 2's showing hidden broad lines in polarized light. The remaining category, AGN2's, contains only Seyferts with no detectable broad lines in either direct or polarized spectroscopy. We present various mid-IR observables, such as ionization-sensitive and density-sensitive line ratios, the polycyclic aromatic hydrocarbon (PAH) 11.25 mu m feature and the H(2)S(1) rotational line equivalent widths (EWs), the (60-25 mu m) spectral index, and the source extendedness at 19 mu m, to characterize similarities and differences in the AGN populations, in terms of AGN dominance versus star formation dominance. We find that the mid-IR emission properties characterize all the AGN 1's objects as a single family, with strongly AGN-dominated spectra. In contrast, the AGN 2's can be divided into two groups, the first one with properties similar to the AGN 1's except without detected broad lines, and the second with properties similar to the non-Seyfert galaxies, such as LINERs or starburst galaxies. We computed a semianalytical model to estimate the AGN and the starburst contributions to the mid-IR galaxy emission at 19 mu m. For 59 galaxies with appropriate data, we can separate the 19 mu m emission into AGN and starburst components using the measured mid-IR spectral features. We use these to quantify the brightness thresholds that an AGN must meet to satisfy our classifications: AGN 1's have an AGN contribution >= 73% and AGN 2 >= 45% of their total emission at 19 mu m. The detection of [Ne v] lines turns out to be an almost perfect signature of energy production by an AGN. Only four (similar to 7.5%) of 55 AGN 1's and two (10%) out of 20 AGN 2's do not have [Ne v] 14.3 mu m down to a flux limit of similar to 4 x 10(-15) erg s(-1) cm(-2). We present mean spectra of the various AGN categories. Passing from AGN-dominated to starburst-dominated objects, the continuum steepens, especially at wavelengths shorter than 20 mu m, while the PAH feature increases in its EW and the high ionization lines decrease. We estimate H(2) mass and excitation temperature through the measurement of the S(1) rotational line of this molecule. Finally, we derive the first local luminosity functions for the brightest mid-IR lines and the PAH feature at 11.25 mu m. No statistical difference is apparent in the space densities for Seyfert 1's and 2's of a given line luminosity, or for the new classes of AGN 1's and 2's. We use the correlation between [Ne v] line and non-stellar IR continuum luminosity to derive the global output of accretion-powered galactic nuclei in the local universe. C1 [Tommasin, Silvia; Spinoglio, Luigi] INAF, Ist Fis Spazio Interplanetario, I-00133 Rome, Italy. [Malkan, Matthew A.] Univ Calif Los Angeles, Astron Div, Los Angeles, CA 90095 USA. [Fazio, Giovanni] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Tommasin, Silvia] Univ Roma La Sapienza, Dept Phys, I-00185 Rome, Italy. RP Tommasin, S (reprint author), INAF, Ist Fis Spazio Interplanetario, Via Fosso Cavaliere 100, I-00133 Rome, Italy. NR 72 TC 65 Z9 64 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 FEB 1 PY 2010 VL 709 IS 2 BP 1257 EP 1283 DI 10.1088/0004-637X/709/2/1257 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 543LT UT WOS:000273579800056 ER PT J AU Milisavljevic, D Fesen, RA Gerardy, CL Kirshner, RP Challis, P AF Milisavljevic, Dan Fesen, Robert A. Gerardy, Christopher L. Kirshner, Robert P. Challis, Peter TI DOUBLETS AND DOUBLE PEAKS: LATE-TIME [O I] lambda lambda 6300, 6364 LINE PROFILES OF STRIPPED-ENVELOPE, CORE-COLLAPSE SUPERNOVAE SO ASTROPHYSICAL JOURNAL LA English DT Article DE supernovae: general; supernovae: individual (SN 2008ax, SN 2008bo, SN 2007uy, SN 2007rz, SN 2007gr) ID OPTICAL SPECTROSCOPY; NEBULAR SPECTRA; PHOTOSPHERIC-PHASE; IB/C SUPERNOVAE; OXYGEN LINES; SN 1998BW; 1993J; EXPLOSIONS; EJECTA; NUCLEOSYNTHESIS AB We present optical spectra of SN 2007gr, SN 2007rz, SN 2007uy, SN 2008ax, and SN 2008bo obtained in the nebular phase when line profiles can lead to information about the velocity distribution of the exploded cores. We compare these to 13 other published spectra of stripped-envelope core-collapse supernovae (Type IIb, Ib, and Ic) to investigate properties of their double-peaked [OI] lambda lambda 6300, 6364 emission. These 18 supernovae are divided into two empirical line profile types: (1) profiles showing two conspicuous emission peaks nearly symmetrically centered on either side of 6300 angstrom and spaced approximate to 64 angstrom apart, close to the wavelength separation between the [OI] lambda 6300, 6364 doublet lines, and (2) profiles showing asymmetric [OI] line profiles consisting of a pronounced emission peak near 6300 angstrom plus one or more blueshifted emission peaks. Examination of these emission profiles, as well as comparison with profiles in the lines of [OI] lambda 5577, OI lambda 7774, and Mg I] lambda 4571, leads us to conclude that neither type of [OI] double-peaked profile is necessarily the signature of emission from front and rear faces of ejecta arranged in a toroidal disk or elongated shell geometry as previously suggested. We propose possible alternative interpretations of double-peaked emission for each profile type, test their feasibility with simple line-fitting models, and discuss their strengths and weaknesses. The underlying cause of the observed predominance of blueshifted emission peaks is unclear, but may be due to internal scattering or dust obscuration of emission from far side ejecta. C1 [Milisavljevic, Dan; Fesen, Robert A.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA. [Gerardy, Christopher L.] Florida State Univ, Dept Phys, Tallahassee, FL 32306 USA. [Kirshner, Robert P.; Challis, Peter] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Milisavljevic, D (reprint author), Dartmouth Coll, Dept Phys & Astron, 6127 Wilder Lab, Hanover, NH 03755 USA. FU National Science Foundation [AST-0606772, AST-0907903]; Canadian NSERC award FX This work has made use of data from many previous observers which proved invaluable in our analysis. We thank M. Modjaz for many helpful comments and kindly providing spectra for SN 2004ao, SN 2006T, SN 2005bf, SN 2004gt, SN 2004dk, and SN 2008D. We also thank P. Hoflich for additional helpful discussions, and the referee for constructive suggestions. Some data presented here were obtained at the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona. Supernova research at the Harvard College Observatory is supported by the National Science Foundation through grants AST-0606772 and AST-0907903. D.M.'s research was supported in part by a Canadian NSERC award. NR 51 TC 37 Z9 37 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 FEB 1 PY 2010 VL 709 IS 2 BP 1343 EP 1355 DI 10.1088/0004-637X/709/2/1343 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 543LT UT WOS:000273579800062 ER PT J AU Acciari, VA Aliu, E Beilicke, M Benbow, W Boltuch, D Bottcher, M Bradbury, SM Bugaev, V Byrum, K Cesarini, A Ciupik, L Cogan, P Cui, W Dickherber, R Duke, C Falcone, A Finley, JP Finnegan, G Fortson, L Furniss, A Galante, N Gall, D Gibbs, K Guenette, R Gillanders, GH Godambe, S Grube, J Hanna, D Hui, CM Humensky, TB Imran, A Kaaret, P Karlsson, N Kertzman, M Kieda, D Krawczynski, H Krennrich, F Lang, MJ LeBohec, S Maier, G McArthur, S McCann, A Moriarty, P Nagai, T Ong, RA Otte, AN Pandel, D Perkins, JS Pichel, A 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 Thibadeau, S Vassiliev, VV Vincent, S Wakely, SP Weekes, TC Weinstein, A Weisgarber, T Williams, DA AF Acciari, V. A. Aliu, E. Beilicke, M. Benbow, W. Boltuch, D. Boettcher, M. Bradbury, S. M. Bugaev, V. Byrum, K. Cesarini, A. Ciupik, L. Cogan, P. Cui, W. Dickherber, R. Duke, C. Falcone, A. Finley, J. P. Finnegan, G. Fortson, L. Furniss, A. Galante, N. Gall, D. Gibbs, K. Guenette, R. Gillanders, G. H. Godambe, S. Grube, J. Hanna, D. Hui, C. M. Humensky, T. B. Imran, A. Kaaret, P. Karlsson, N. Kertzman, M. Kieda, D. Krawczynski, H. Krennrich, F. Lang, M. J. LeBohec, S. Maier, G. McArthur, S. McCann, A. Moriarty, P. Nagai, T. Ong, R. A. Otte, A. N. Pandel, D. Perkins, J. S. Pichel, A. 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. Thibadeau, S. Vassiliev, V. V. Vincent, S. Wakely, S. P. Weekes, T. C. Weinstein, A. Weisgarber, T. Williams, D. A. TI DISCOVERY OF VARIABILITY IN THE VERY HIGH ENERGY gamma-RAY EMISSION OF 1ES 1218+304 WITH VERITAS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE BL Lacertae objects: individual (1ES 1218+304=VER J1221+301); galaxies: active; gamma rays: galaxies ID ACTIVE GALACTIC NUCLEI; EXTRAGALACTIC BACKGROUND LIGHT; PEAKED BL-LACERTAE; W-COMAE; BLAZARS; SPECTRA; ACCELERATION; JET; CONSTRAINTS; TELESCOPE AB We present results from an intensive VERITAS monitoring campaign of the high-frequency peaked BL Lac object 1ES 1218+304 in 2008/2009. Although 1ES 1218+304 was detected previously by MAGIC and VERITAS at a persistent level of similar to 6% of the Crab Nebula flux, the new VERITAS data reveal a prominent flare reaching similar to 20% of the Crab. While very high energy (VHE) flares are quite common in many nearby blazars, the case of 1ES 1218+304 (redshift z = 0.182) is particularly interesting since it belongs to a group of blazars that exhibit unusually hard VHE spectra considering their redshifts. When correcting the measured spectra for absorption by the extragalactic background light, 1ES 1218+304 and a number of other blazars are found to have differential photon indices Gamma <= 1.5. The difficulty in modeling these hard spectral energy distributions in blazar jets has led to a range of theoretical gamma-ray emission scenarios, one of which is strongly constrained by these new VERITAS observations. We consider the implications of the observed light curve of 1ES 1218+304, which shows day scale flux variations, for shock acceleration scenarios in relativistic jets, and in particular for the viability of kiloparsec-scale jet emission scenarios. C1 [Acciari, V. A.; Benbow, W.; Galante, N.; Gibbs, K.; Perkins, J. S.; Roache, E.; Theiling, M.; Weekes, T. C.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Aliu, E.] Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. [Beilicke, M.; Bugaev, V.; Dickherber, R.; Krawczynski, H.; McArthur, S.; Thibadeau, S.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Boltuch, D.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Boltuch, D.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Boettcher, M.] Ohio Univ, Dept Phys & Astron, Inst Astrophys, Athens, OH 45701 USA. [Bradbury, S. M.; Rose, H. J.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [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.; Karlsson, N.; Steele, D.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA. [Cogan, P.; Guenette, R.; Hanna, D.; Maier, G.; McCann, A.; Ragan, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Cui, W.; Finley, J. P.; Gall, D.; Sembroski, G. H.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Duke, C.] Grinnell Coll, Dept Phys, Grinnell, IA 50112 USA. [Falcone, A.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 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. [Furniss, A.; Otte, A. N.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Furniss, A.; Otte, A. N.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Grube, J.; Pandel, D.; Quinn, J.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Humensky, T. B.; Swordy, S. P.; Wakely, S. P.; Weisgarber, T.] 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.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Kertzman, M.] Depaul Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. [Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland. [Ong, R. A.; Vassiliev, V. V.; Weinstein, A.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Pichel, A.] Inst Astron & Fis Espacio, RA-1428 Buenos Aires, DF, Argentina. [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. 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; STFC in the U.K.; Science Foundation Ireland FX This research is supported by grants from the U.S. Department of Energy, the U.S. National Science Foundation, the Smithsonian Institution, by NSERC in Canada, by STFC in the U.K. and by Science Foundation Ireland. 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. NR 36 TC 28 Z9 28 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD FEB 1 PY 2010 VL 709 IS 2 BP L163 EP L167 DI 10.1088/2041-8205/709/2/L163 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 551LD UT WOS:000274209300015 ER PT J AU Miyake, S Stancil, PC Sadeghpour, HR Dalgarno, A McLaughlin, BM Forrey, RC AF Miyake, S. Stancil, P. C. Sadeghpour, H. R. Dalgarno, A. McLaughlin, B. M. Forrey, R. C. TI RESONANT H- PHOTODETACHMENT: ENHANCED PHOTODESTRUCTION AND CONSEQUENCES FOR RADIATIVE FEEDBACK SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE atomic processes; cosmology: theory; early universe; galaxies: formation; galaxies: high-redshift ID MOLECULAR-HYDROGEN; GAS CLOUDS; PHOTOIONIZATION; REIONIZATION; SIMULATIONS; GALAXIES; OBJECTS AB The hydrogen negative ion plays a crucial role in the formation of hydrogen molecules in the early universe. Cooling through excitation of H-2 drives the formation of the first cosmological objects. The H-2 molecules are produced primarily by a reaction sequence initiated by H-. We explore the influence of enhanced photodestruction rates that arise due to absorption by resonance states of H- lying near 11 eV. We examine the feedback effects that occur in radiation fields characteristic of Population III stars, blackbody sources, power-law spectra, and the hydrogen Lyman modulated sawtooth spectra of the high-redshift intergalactic medium. C1 [Miyake, S.; Stancil, P. C.] Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA. [Miyake, S.; Stancil, P. C.] Univ Georgia, Ctr Simulat Phys, Athens, GA 30602 USA. [Sadeghpour, H. R.; Dalgarno, A.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. [McLaughlin, B. M.] Queens Univ Belfast, Sch Math & Phys, Belfast BT7 1NN, Antrim, North Ireland. [Forrey, R. C.] Penn State Univ, Dept Phys, Reading, PA 19610 USA. RP Miyake, S (reprint author), Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA. EM shinyam@physast.uga.edu; stancil@physast.uga.edu; hrs@cfa.harvard.edu; adalgarno@cfa.harvard.edu; b.mclaughlin@qub.ac.uk; rcf6@psu.edu FU NSF [AST-0607733, AST-0607532, PHY-0554794]; Pennsylvania State University FX S.M. and P.C.S. acknowledge support from NSF Grant AST-0607733, while A.D. acknowledges NSF Grant AST-0607532. The work of B.M.McL. and R.C.F. was supported by a research development grant from the Pennsylvania State University and NSF grant No. PHY-0554794. P.C.S., B.M.McL., and R.C.F thank the Institute for Theoretical Atomic, Molecular, and Optical Physics at the Harvard-Smithsonian Center for Astrophysics for travel support. NR 21 TC 16 Z9 16 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 FEB 1 PY 2010 VL 709 IS 2 BP L168 EP L171 DI 10.1088/2041-8205/709/2/L168 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 551LD UT WOS:000274209300016 ER PT J AU Currie, T Hernandez, J Irwin, J Kenyon, SJ Tokarz, S Balog, Z Bragg, A Berlind, P Calkins, M AF Currie, Thayne Hernandez, Jesus Irwin, Jonathan Kenyon, Scott J. Tokarz, Susan Balog, Zoltan Bragg, Ann Berlind, Perry Calkins, Mike TI THE STELLAR POPULATION OF h AND chi PERSEI: CLUSTER PROPERTIES, MEMBERSHIP, AND THE INTRINSIC COLORS AND TEMPERATURES OF STARS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE open clusters and associations: individual (NGC 869, NGC 884); stars: pre-main sequence ID LOW-MASS STARS; MAIN-SEQUENCE EVOLUTION; YOUNG OPEN CLUSTERS; GAS GIANT PLANETS; M-CIRCLE-DOT; B-TYPE STARS; MONITOR PROJECT; THEORETICAL ISOCHRONES; CHEMICAL-COMPOSITION; PHOTOMETRIC SYSTEMS AB From photometric observations of similar to 47,000 stars and spectroscopy of similar to 11,000 stars, we describe the first extensive study of the stellar population of the famous Double Cluster, h and chi Persei, down to subsolar masses. By analyzing optical spectra and optical/infrared photometry, we constrain the distance moduli (dM), reddening (E(B - V)), and ages for h Persei, chi Persei, and the low-density halo population surrounding both cluster cores. With the exception of mass and spatial distribution, the clusters are nearly identical in every measurable way. Both clusters have E(B - V) similar to 0.52-0.55 and dM = 11.8-11.85; the halo population, while more poorly constrained, likely has identical properties. As determined from the main-sequence turnoff, the luminosity of M supergiants, and pre-main-sequence isochrones, ages for h Persei, chi Persei, and the halo population all converge on approximate to 14 Myr, thus showing a stunning agreement between estimates based on entirely different physics. From these data, we establish the first spectroscopic and photometric membership lists of cluster stars down to early/mid M dwarfs. At minimum, there are similar to 5000 members within 10' of the cluster centers, while the entire h and chi Persei region has at least similar to 13,000 and as many as 20,000 members. The Double Cluster contains approximate to 8400 M(circle dot) of stars within 10' of the cluster centers. We estimate a total mass of at least 20,000 M(circle dot). We conclude our study by outlining outstanding questions regarding the past and present properties of h and chi Persei. From comparing recent work, we compile a list of intrinsic colors and derive a new effective temperature scale for O-M dwarfs, giants, and supergiants. C1 [Currie, Thayne; Irwin, Jonathan; Kenyon, Scott J.; Tokarz, Susan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Currie, Thayne] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hernandez, Jesus] Ctr Invest Astron CIDA, Merida 5101A, Venezuela. [Irwin, Jonathan] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Balog, Zoltan] MPIA Heidelberg, Heidelberg, Germany. [Bragg, Ann] Marietta Coll, Dept Phys, Marietta, OH USA. [Berlind, Perry; Calkins, Mike] Fred Lawrence Whipple Observ, Tucson, AZ USA. RP Currie, T (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM tcurrie@cfa.harvard.edu; jhernan@umich.edu; jirwin@cfa.harvard.edu NR 96 TC 40 Z9 40 U1 0 U2 1 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 FEB PY 2010 VL 186 IS 2 BP 191 EP 221 DI 10.1088/0067-0049/186/2/191 PG 31 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 552IU UT WOS:000274283900002 ER PT J AU Rup, MP Bailey, SA Wiley, CJ Minton, MS Miller, AW Ruiz, GM MacIsaac, HJ AF Rup, Michael P. Bailey, Sarah A. Wiley, Chris J. Minton, Mark S. Miller, A. Whitman Ruiz, Gregory M. MacIsaac, Hugh J. TI Domestic ballast operations on the Great Lakes: potential importance of Lakers as a vector for introduction and spread of nonindigenous species SO CANADIAN JOURNAL OF FISHERIES AND AQUATIC SCIENCES LA English DT Article ID BIOLOGICAL INVASIONS; WATER; INVADERS; MANAGEMENT AB Ballast water is recognized globally as a major vector of aquatic nonindigenous species (NIS) introductions; domestic ballast water transfers, however, have generally been considered low risk in North America. We characterize ballast operations of domestic ships in the Great Lakes - St. Lawrence River system (Lakers) during 2005-2007 to examine the risk of primary and secondary introductions associated with ballast water transfers over short distances. Results indicate that Lakers transported at least 68 million tonnes of ballast water annually. Approximately 71% of ballast water transfers were interregional, with net movement being from lower to upper lakes. A small proportion of ballast water discharged in the Great Lakes (<1%) originated from ports in the St. Lawrence River that may serve as sources for new NIS. These results indicate that domestic ballast water transfers may contribute to NIS introductions and are likely the most important ballast-mediated pathway of secondary spread within the Great Lakes. Future efforts to reduce invasion impacts should consider both primary and secondary introduction mechanisms. C1 [Rup, Michael P.; Bailey, Sarah A.; MacIsaac, Hugh J.] Univ Windsor, Great Lakes Inst Environm Res, Windsor, ON N9H 2L2, Canada. [Wiley, Chris J.] Fisheries & Oceans Canada, Transport Canada Marine Safety, Sarnia, ON N7T 2M4, Canada. [Minton, Mark S.; Miller, A. Whitman; Ruiz, Gregory M.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Bailey, SA (reprint author), Fisheries & Oceans Canada, Great Lakes Lab Fisheries & Aquat Sci, Burlington, ON L7R 4A6, Canada. EM sarah.bailey@dfo-mpo.gc.ca RI Bailey, Sarah/E-8356-2010; OI Ruiz, Gregory/0000-0003-2499-441X; Minton, Mark/0000-0002-9439-4930 FU Fisheries and Oceans Canada; Transport Canada; Natural Sciences and Engineering Research Council of Canada Canadian Aquatic Invasive Species Network; US Coast Guard FX We thank M. Deneau, L. Quiring, K. Ryan, S. Sontavy, and the US Lake Carriers' and Canadian Shipowners Associations for assistance with data acquisition. Y. de Lafontaine, N. Simard, and A. Ricciardi provided background information on community composition of the St. Lawrence River. Funding was provided by Fisheries and Oceans Canada, Transport Canada (S.A.B,), the Natural Sciences and Engineering Research Council of Canada Canadian Aquatic Invasive Species Network (H.J.M.), and the US Coast Guard (G.M.R. and A.W.M.). NR 35 TC 21 Z9 21 U1 3 U2 18 PU NATL RESEARCH COUNCIL CANADA-N R C RESEARCH PRESS PI OTTAWA PA BUILDING M 55, OTTAWA, ON K1A 0R6, CANADA SN 0706-652X J9 CAN J FISH AQUAT SCI JI Can. J. Fish. Aquat. Sci. PD FEB PY 2010 VL 67 IS 2 BP 256 EP 268 DI 10.1139/F09-180 PG 13 WC Fisheries; Marine & Freshwater Biology SC Fisheries; Marine & Freshwater Biology GA 553FU UT WOS:000274352400004 ER PT J AU Greenberg, R Olsen, BJ Etterson, MA AF Greenberg, Russell Olsen, Brian J. Etterson, Matthew A. TI PATTERNS OF SEASONAL ABUNDANCE AND SOCIAL SEGREGATION IN INLAND AND COASTAL PLAIN SWAMP SPARROWS IN A DELAWARE TIDAL MARSH SO CONDOR LA English DT Article DE migration; subspecies; Melospiza georgiana; tidal marsh; social segregation; geographic variation; species recognition; Swamp Sparrow ID HYBRID ZONES; FLYCATCHERS; RANGE AB The Coastal Plain Swamp Sparrow (Melospiza georgiana nigrescens) breeds in coastal marshes of the mid-Atlantic United States. During the nonbreeding season, these marshes are occupied by this subspecies and the two interior-breeding subspecies M. g. georgiana and M. g. ericrypta (collectively, interior Swamp Sparrows). From September to May, 2005-2006 and 2007-2008, we surveyed marshes in which nigrescens breeds; > 90% of these birds had been color-banded by the end of the previous breeding season. This allowed us to determine the nonbreeding occupancy of the breeding site by individuals that bred locally, Coastal Plain Swamp Sparrows that did not breed there, and interior Swamp Sparrows. Locally breeding birds disappeared from the breeding site by mid-October, although nonlocal nigrescens occupied it from October to late November. Locally breeding birds reappeared in April without any pulse of migration of nigrescens. Interior-breeding sparrows were abundant in the autumn and appeared in smaller numbers later in the nonbreeding season. The seasonal pattern of nigrescens was similar in both years, and its departure and arrival dates appear to coincide with changes in the frequency of freezing temperatures. The temporal pattern of interior Swamp Sparrows in the two years was more varied. Finally, during the autumn peak of Swamp Sparrow migration, the subspecies tended strongly to segregate in subspecies-specific flocks, suggesting that Swamp Sparrows preferentially interact with morphologically similar birds, a behavior which may have implications for divergence in species recognition mechanisms and speciation. C1 [Greenberg, Russell] Smithsonian Inst, Natl Zool Pk, Smithsonian Migratory Bird Ctr, Washington, DC 20008 USA. [Olsen, Brian J.] Univ Maine, Sch Biol & Ecol, Orono, ME 04473 USA. [Etterson, Matthew A.] US EPA, Midcontinent Ecol Div, Duluth, MN 55803 USA. RP Greenberg, R (reprint author), Smithsonian Inst, Natl Zool Pk, Smithsonian Migratory Bird Ctr, Washington, DC 20008 USA. EM greenbergr@si.edu OI Olsen, Brian/0000-0001-5608-2779 NR 26 TC 2 Z9 2 U1 1 U2 3 PU COOPER ORNITHOLOGICAL SOC PI LAWRENCE PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 USA SN 0010-5422 EI 1938-5129 J9 CONDOR JI Condor PD FEB PY 2010 VL 112 IS 1 BP 159 EP 167 DI 10.1525/cond.2010.080060 PG 9 WC Ornithology SC Zoology GA 576ED UT WOS:000276126200017 ER PT J AU Venter, O Watson, JEM Meijaard, E Laurance, WF Possingham, HP AF Venter, Oscar Watson, James E. M. Meijaard, Erik Laurance, William F. Possingham, Hugh P. TI Avoiding Unintended Outcomes from REDD SO CONSERVATION BIOLOGY LA English DT Letter ID DEFORESTATION; FORESTS C1 [Venter, Oscar; Watson, James E. M.; Possingham, Hugh P.] Univ Queensland, Ctr Ecol, Brisbane, Qld 4072, Australia. [Meijaard, Erik] People & Nat Consulting Int, Badung, Bali, Indonesia. [Laurance, William F.] James Cook Univ, Sch Marine & Trop Biol, Cairns, Qld 4870, Australia. [Laurance, William F.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Venter, O (reprint author), Univ Queensland, Ctr Ecol, Brisbane, Qld 4072, Australia. EM oventer@uq.edu.au RI Possingham, Hugh/B-1337-2008; Venter, Oscar/G-6893-2011; Laurance, William/B-2709-2012; Meijaard, Erik/A-2687-2016; Watson, James/D-8779-2013 OI Possingham, Hugh/0000-0001-7755-996X; Meijaard, Erik/0000-0001-8685-3685; Watson, James/0000-0003-4942-1984 NR 14 TC 11 Z9 11 U1 1 U2 11 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0888-8892 J9 CONSERV BIOL JI Conserv. Biol. PD FEB PY 2010 VL 24 IS 1 BP 5 EP 6 PG 2 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 544VF UT WOS:000273686700003 PM 20121835 ER PT J AU Reding, DM Freed, LA Cann, RL Fleischer, RC AF Reding, Dawn M. Freed, Leonard A. Cann, Rebecca L. Fleischer, Robert C. TI Spatial and temporal patterns of genetic diversity in an endangered Hawaiian honeycreeper, the Hawaii Akepa (Loxops coccineus coccineus) SO CONSERVATION GENETICS LA English DT Article DE Hawaiian honeycreepers; Ancient DNA; Habitat fragmentation; Landscape genetics; Population bottleneck; Effective population size ID EFFECTIVE POPULATION-SIZE; CONTROL-REGION SEQUENCES; MITOCHONDRIAL-DNA; STATISTICAL TESTS; MUSEUM SPECIMENS; NUCLEAR GENOME; CANIS-LUPUS; GROWTH; CONSERVATION; POLYMORPHISMS AB As a result of disease, habitat destruction, and other anthropogenic factors, the Hawaii Akepa (Loxops coccineus coccineus) currently occupies <10% of its original range and exists in five disjunct populations, raising concerns about what effect such reduction and fragmentation has had on the connectivity and diversity of Akepa populations. In this study, we used both historical and contemporary samples to assess genetic diversity and structure in this endangered Hawaiian honeycreeper. We generated sequence data from two mtDNA regions (ND2, control region) and two nuclear introns for contemporary samples representing three of the five current populations. We also generated control region sequence data for museum specimens collected over 100 years ago from throughout the historical range of the bird. Results indicate that despite recent declines and fragmentation, genetic diversity has not been lost. We detected a modest level of genetic differentiation, which followed a combined pattern of isolation-by-barriers and isolation-by-distance, across the historical range of Akepa. The similarly low level of differentiation observed between the contemporary populations indicates that not much divergence, if any, has occurred post-fragmentation. Rather, the present structure seen likely reflects the historical pattern of distribution. Ironically, this declining species exhibits the genetic signal of an expanding population, demonstrating that earlier demographic events are outweighing the effects of recent changes in population size, and genetic estimates of Ne, though crude, suggest Hawaii Akepa were at least an order of magnitude more abundant prior to the decline. C1 [Reding, Dawn M.] Iowa State Univ, Dept Ecol Evolut & Organismal Biol, Ames, IA 50011 USA. [Reding, Dawn M.; Freed, Leonard A.] Univ Hawaii Manoa, Dept Zool, Honolulu, HI 96822 USA. [Reding, Dawn M.; Fleischer, Robert C.] Smithsonian Inst, Natl Zool Pk, Washington, DC 20008 USA. [Reding, Dawn M.; Fleischer, Robert C.] Natl Museum Nat Hist, Genet Program, Washington, DC 20008 USA. [Cann, Rebecca L.] Univ Hawaii Manoa, John A Burns Sch Med, Dept Cell & Mol Biol, Honolulu, HI 96822 USA. RP Reding, DM (reprint author), Iowa State Univ, Dept Ecol Evolut & Organismal Biol, 253 Bessey Hall, Ames, IA 50011 USA. EM reding@iastate.edu FU National Wildlife Refuge Centennial Scholarship Program; Walt Disney Company; National Fish and Wildlife Foundation; Jessie D. Kay Memorial fund; University of Hawaii EECB Program; National Science Foundation [DGE02-32016]; Smithsonian Institution Short-Term Visitor; Environmental Protection Agency [R82-9093]; NSF [0083944]; American Museum of Natural History; Bernice P. Bishop Museum; California Academy of Sciences; Los Angeles County Museum; Museum of Vertebrate Zoology; National Museum of Natural History; Royal Ontario Museum; University Museum of Zoology, Cambridge; and Zoological Museum, Kopenhagen FX Financial support for this project was provided by the National Wildlife Refuge Centennial Scholarship Program, Walt Disney Company, National Fish and Wildlife Foundation, Jessie D. Kay Memorial fund, University of Hawaii EECB Program, National Science Foundation (DGE02-32016 awarded to K. Kaneshiro), Sigma Xi Grant-In-Aid of Research, Smithsonian Institution Short-Term Visitor Grant and Genetics Program, and the Environmental Protection Agency (R82-9093 awarded to L. Freed, R. Cann, and M. Goff). For providing samples, we thank the Hawaii Biocomplexity Project (supported by NSF under Grant No. 0083944 awarded to D. Duffy and by USGS) and the staff of the following museums: American Museum of Natural History; Bernice P. Bishop Museum; California Academy of Sciences; Los Angeles County Museum; Museum of Vertebrate Zoology; National Museum of Natural History; Royal Ontario Museum; University Museum of Zoology, Cambridge; and Zoological Museum, Kopenhagen. Special thanks to Ben Wollenzien, Chris Jager, Alex Frank, Wendy Kuntz, and Eldridge Naboa for field assistance and to Hawaii State Division of Forestry and Wildlife and the National Park Service for field site access. We are grateful to R. Toonen, J. Groombridge, and three anonymous reviewers for providing helpful comments on earlier drafts of this manuscript. NR 86 TC 17 Z9 17 U1 2 U2 43 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1566-0621 EI 1572-9737 J9 CONSERV GENET JI Conserv. Genet. PD FEB PY 2010 VL 11 IS 1 BP 225 EP 240 DI 10.1007/s10592-009-0025-8 PG 16 WC Biodiversity Conservation; Genetics & Heredity SC Biodiversity & Conservation; Genetics & Heredity GA 545OQ UT WOS:000273744300019 ER PT J AU Faaborg, J Holmes, RT Anders, AD Bildstein, KL Dugger, KM Gauthreaux, SA Heglund, P Hobson, KA Jahn, AE Johnson, DH Latta, SC Levey, DJ Marra, PP Merkord, CL Nol, E Rothstein, SI Sherry, TW Sillett, TS Thompson, FR Warnock, N AF Faaborg, John Holmes, Richard T. Anders, Angela D. Bildstein, Keith L. Dugger, Katie M. Gauthreaux, Sidney A., Jr. Heglund, Patricia Hobson, Keith A. Jahn, Alex E. Johnson, Douglas H. Latta, Steven C. Levey, Douglas J. Marra, Peter P. Merkord, Christoper L. Nol, Erica Rothstein, Stephen I. Sherry, Thomas W. Sillett, T. Scott Thompson, Frank R., III Warnock, Nils TI Recent advances in understanding migration systems of New World land birds SO ECOLOGICAL MONOGRAPHS LA English DT Review DE austral migration; breeding season population limitation; carry-over effects; connectivity; en route ecology; intratropical migration; land birds; migration; soure-sink demography; winter population limitation ID THROATED BLUE WARBLERS; HABITAT-SPECIFIC DEMOGRAPHY; WHITE-CROWNED SPARROWS; MIXED-SPECIES FLOCKS; ZONOTRICHIA-LEUCOPHRYS-GAMBELII; NEOTROPICAL MIGRANT SONGBIRDS; CURRENT REPRODUCTIVE EFFORT; TEMPERATE DECIDUOUS FOREST; ESTIMATING SITE OCCUPANCY; SANDPIPER CALIDRIS-MAURI AB Our understanding of migratory birds' year-round ecology and evolution remains patchy despite recent fundamental advances. Periodic reviews focus future research and inform conservation and management; here, we take advantage of our combined experiences working on Western Hemisphere avian migration systems to highlight recent lessons and critical gaps in knowledge. Among topics discussed are: (1) The pipeline from pure to applied researchers leaves room for improvement. (2) Population limitation and regulation includes both seasonal and between-season interactions. (3) The study of movements of small-bodied species remains a major research frontier. (4) We must increase our understanding of population connectivity. (5) With few exceptions, population regulation has barely been investigated. (6) We have increasingly integrated landscape configuration of habitats, large-scale habitat disturbances, and habitat quality impacts into models of seasonal and overall demographic success. (7) The post-breeding season (late summer for latitudinal migrants) is increasingly appreciated for its impacts on demography. (8) We recognize the diverse ways that avian brood parasites, nest predators, and food availability affect demography. (9) Source-sink and meta-population models help us understand migratory avian distributions among fragmented habitats. (10) Advances in modeling have improved estimates of annual survival and fecundity, but for few species. (11) Populations can be limited by ecological conditions in winter, but habitat needs are poorly known for most species at this time. (12) Migration tends to occupy broad spatial fronts that may change seasonally or when migrants cross major barriers. (13) En route conditions can limit migrant populations; linking migration habitat quality indicators to fitness or population consequences presents a major challenge. (14) A variety of intra-tropical Neotropical migration patterns are recognizable,. but almost nothing is known about these systems beyond descriptions of a few typical species' movements. (15) Global climate change scenarios predict range and phenology shifts of Neotropical migrant bird populations that must be considered in conservation plans. Future studies will depend on new technologies and the integration of modeling with sophisticated, large-spatial-scale measurement and parameter estimation; whether the pace of research and management involving migratory birds can match the growth of environmental threats remains to be seen. C1 [Faaborg, John; Merkord, Christoper L.] Univ Missouri, Div Biol Sci, Columbia, MO 65211 USA. [Holmes, Richard T.] Dartmouth Coll, Dept Biol Sci, Hanover, NH 03755 USA. [Anders, Angela D.] Clancy Environm Consultants, Papahanaumokuakea Natl Monument, Honolulu, HI 96825 USA. [Bildstein, Keith L.] Hawk Mt Sanctuary, Acopian Ctr Conservat Learning, Orwigsburg, PA 17961 USA. [Dugger, Katie M.] Oregon State Univ, Dept Fisheries & Wildlife, Corvallis, OR 97331 USA. [Gauthreaux, Sidney A., Jr.] Clemson Univ, Dept Biol Sci, Clemson, SC 29634 USA. [Heglund, Patricia] US Fish & Wildlife Serv, La Crosse, WI 54603 USA. [Hobson, Keith A.] Environm Canada, Canadian Wildlife Serv, Saskatoon, SK S7N 0X4, Canada. [Jahn, Alex E.; Johnson, Douglas H.] Univ Florida, Dept Zool, Gainesville, FL 32611 USA. [Johnson, Douglas H.] USGS No Prairie Wildlife Res Ctr, St Paul, MN 55108 USA. [Latta, Steven C.] Natl Aviary, Dept Conservat & Field Res, Pittsburgh, PA 15212 USA. [Marra, Peter P.; Sillett, T. Scott] Natl Zool Pk, Smithsonian Migratory Bird Ctr, Washington, DC 20013 USA. [Nol, Erica] Trent Univ, Ecol & Conservat Grp, Environm & Life Sci Grad Program, Peterborough, ON K9J 7B8, Canada. [Nol, Erica] Trent Univ, Dept Biol, Peterborough, ON K9J 7B8, Canada. [Rothstein, Stephen I.] Univ Calif Santa Barbara, Dept Ecol Evolut & Marine Biol, Santa Barbara, CA 93106 USA. [Sherry, Thomas W.] Tulane Univ, Dept Ecol & Evolutionary Biol, New Orleans, LA 70118 USA. [Thompson, Frank R., III] Univ Missouri, USDA, US Forest Serv, No Res Stn, Columbia, MO 65211 USA. [Warnock, Nils] PRBO Conservat Sci, Petaluma, CA 94954 USA. RP Faaborg, J (reprint author), Univ Missouri, Div Biol Sci, Columbia, MO 65211 USA. EM faaborgj@missouri.edu OI Merkord, Chris/0000-0003-2825-1904 NR 458 TC 116 Z9 121 U1 24 U2 177 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 0012-9615 EI 1557-7015 J9 ECOL MONOGR JI Ecol. Monogr. PD FEB PY 2010 VL 80 IS 1 BP 3 EP 48 DI 10.1890/09-0395.1 PG 46 WC Ecology SC Environmental Sciences & Ecology GA 572GW UT WOS:000275816800002 ER PT J AU Heckel, CD Bourg, NA McShea, WJ Kalisz, S AF Heckel, Christopher D. Bourg, Norman A. McShea, William J. Kalisz, Susan TI Nonconsumptive effects of a generalist ungulate herbivore drive decline of unpalatable forest herbs SO ECOLOGY LA English DT Article DE Arisaema triphyllum; biodiversity; generalist herbivores; indirect effects; indirect facilitation; Odocoileus virginianus; overbrowsing; palatable plants; Pennsylvania, USA; species interactions; Trillium; unbrowsed and unpalatable plants ID WHITE-TAILED DEER; TRIPHYLLUM L. SCHOTT; IN-THE-PULPIT; SOIL COMPACTION; TRILLIUM-GRANDIFLORUM; GRAZING INTENSITY; PERENNIAL HERB; PLANT; POPULATIONS; DYNAMICS AB High herbivore pressure is expected to benefit unpalatable species that co-occur with palatable browsed species. However, for five unpalatable understory species we found no evidence of benefit from deer browse. Detailed Studies of one species in natural populations, Arisaema triphyllum, revealed surprising changes in its Population structure and demography: deer browse level on a palatable species significantly correlates with reduced plant size and seed rain and male-biased sex ratios of co-occurring Arisaema populations. Analyses of individual size in five unpalatable forest plant species in long-term experimental paired deer exclosure/deer access plots corroborate the natural site results; all five species were smaller in deer access plots. Analyses of abiotic variables in natural and experimental sites suggest one potential mechanism for indirect effects of deer. Deer-mediated soil quality declines included increased soil penetration resistance and decreased leaf litter depth, which are known to hinder plant growth. Our results are likely applicable to other unpalatable forest species and have clear consequences for understory biodiversity. Unpalatable plant species in forests experiencing high deer numbers may be in decline along with their palatable neighbors. Our study implicates deer overabundance in the cascade of forest species decline and the urgency of this conservation issue in North America. C1 [Heckel, Christopher D.; Kalisz, Susan] Univ Pittsburgh, Dept Biol Sci, Pittsburgh, PA 15260 USA. [Bourg, Norman A.; McShea, William J.] Smithsonian Inst Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA 22630 USA. RP Heckel, CD (reprint author), Hillsdale Acad, 1 Acad Lane, Hillsdale, MI 49242 USA. EM cdh8@pitt.edu OI Heckel, Christopher/0000-0002-6072-3935; Bourg, Norman/0000-0002-7443-1992 FU NSF [DEB 0108208]; University of Pittsburgh's Pymatuning Laboratory of Ecology FX This study was supported by NSF grant DEB 0108208 to S. Kalisz and by Phipps Conservatory and Botanical Garden Botany-in-Action Fellowship and McKinley/Darbaker/Pape Funds from the University of Pittsburgh's Pymatuning Laboratory of Ecology to C. D. Heckel. We thank J. R. Paul and H. B. Schumacher for in-depth discussions; J. R. Auld, W. P. Carson,. J. L. Dunn, A. N. Hale, T. H. Pendergast IV, A. M. Randle, R. B. Spigler, A. L. Tonsor, S. J. Tonsor IV, and two anonymous reviewers for comments on draft manuscripts; A. Cantor, J. L. Dilrin, A. Hale, A. Hansgate, P. Heckel, T. O'Day, R. Unks, and J. Winkler for fieldwork assistance; and R. Gubler, Shenandoah National Park Biologist, for deer density information for the Park. This is contribution number 233 of the Pymatuning Laboratory of Ecology. NR 57 TC 31 Z9 31 U1 7 U2 47 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 FEB PY 2010 VL 91 IS 2 BP 319 EP 326 DI 10.1890/09-0628.1 PG 8 WC Ecology SC Environmental Sciences & Ecology GA 572GX UT WOS:000275816900002 PM 20391995 ER PT J AU Burns, KC Zotz, G AF Burns, K. C. Zotz, G. TI A hierarchical framework for investigating epiphyte assemblages: networks, meta-communities, and scale SO ECOLOGY LA English DT Article DE checkerboard distribution; co-occurrence; epiphyte; host trees; meta-community; nestedness; network; null model; Panamanian rain forest; plant assemblages; seale-dependent patterns; spatiotemporal variation ID AMAZONIAN RAIN-FOREST; VASCULAR EPIPHYTES; MUTUALISTIC NETWORKS; SPECIES COMPOSITION; LOWLAND FOREST; NEUTRAL MODELS; TREE SIZE; NESTEDNESS; ECOLOGY; DIVERSITY AB Epiphytes are an important component of many forested ecosystems, yet our understanding of epiphyte communities lags far behind that of terrestrial-based plant communities. This discrepancy is exacerbated by the lack of a theoretical context to assess patterns in epiphyte community structure. We attempt to fill this gap by developing an analytical framework to investigate epiphyte assemblages, which we then apply to a data set on epiphyte distributions in a Panamanian rain forest. On a coarse scale, interactions between epiphyte species and host tree species can be viewed as bipartite networks, similar to pollination and seed dispersal networks. On a finer scale, epiphyte communities on individual host trees can be viewed as meta-communities, or suites of local epiphyte Communities connected by dispersal. Similar analytical tools are typically employed to investigate species interaction networks and meta-communities, thus providing a unified analytical framework to investigate coarse-scale (network) and fine-scale (meta-community) patterns in epiphyte distributions. Coarse-scale analysis of the Panamanian data set showed that most epiphyte species interacted with fewer host species than expected by chance. Fine-scale analyses showed that epiphyte species richness on individual trees was lower than null model expectations. Therefore, epiphyte distributions were clumped at both scales, perhaps as a result of dispersal. limitations. Scale-dependent patterns in epiphyte species composition were observed. Epiphyte-host networks showed evidence of negative co-occurrence patterns, which Could arise from adaptations among epiphyte species to avoid competition for host species, while most epiphyte meta-communi ties were distributed at random. Application Of our "meta-network" analytical framework in other locales may help to identify general patterns in the structure of epiphyte assemblages and their variation in space and time. C1 [Burns, K. C.] Victoria Univ Wellington, Sch Biol Sci, Wellington, New Zealand. [Zotz, G.] Carl von Ossietzky Univ Oldenburg, Inst Environm & Biol Sci, D-26111 Oldenburg, Germany. [Zotz, G.] Smithsonian Trop Res Inst, Balboa, Panama. RP Burns, KC (reprint author), Victoria Univ Wellington, Sch Biol Sci, POB 600, Wellington, New Zealand. EM kevin.burns@vuw.ac.nz NR 64 TC 31 Z9 33 U1 2 U2 36 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 FEB PY 2010 VL 91 IS 2 BP 377 EP 385 DI 10.1890/08-2004.1 PG 9 WC Ecology SC Environmental Sciences & Ecology GA 572GX UT WOS:000275816900010 PM 20392003 ER PT J AU McCoy, TJ AF McCoy, Timothy J. TI Mineralogical Evolution of Meteorites SO ELEMENTS LA English DT Article DE mineral evolution; meteorites; asteroids; metamorphism; differentiation; shock ID CHONDRITE; OXIDE AB The approximately 250 mineral species found in meteorites record the earliest stages of the birth of our solar system. Refractory minerals that formed during the violent deaths of other stars and during condensation of our own solar nebula mixed with a wide range of silicates, sulfides, and metals to form the most primitive chondritic meteorites. Subsequent aqueous alteration, thermal metamorphism, and shock metamorphism further diversified the minerals found in meteorites. Asteroidal melting at first Increased and then dramatically decreased mineralogical diversity, before a new phase of igneous differentiation that presaged the processes that would occur in terrestrial planets. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. RP McCoy, TJ (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. EM mccoyt@si.edu NR 27 TC 7 Z9 7 U1 1 U2 4 PU MINERALOGICAL SOC AMER PI CHANTILLY PA 3635 CONCORDE PKWY STE 500, CHANTILLY, VA 20151-1125 USA SN 1811-5209 J9 ELEMENTS JI Elements PD FEB PY 2010 VL 6 IS 1 BP 19 EP 23 DI 10.2113/gselements.6.1.19 PG 5 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA 576ND UT WOS:000276150400005 ER PT J AU Taerum, SJ Cafaro, MJ Currie, CR AF Taerum, S. J. Cafaro, M. J. Currie, C. R. TI Presence of Multiparasite Infections Within Individual Colonies of Leaf-Cutter Ants SO ENVIRONMENTAL ENTOMOLOGY LA English DT Article DE coevolution; parasites; leaf-cutting ants; superinfection ID FUNGUS-GROWING ANTS; PARASITE VIRULENCE; MICROBE SYMBIOSIS; MULTIPLE INFECTIONS; NEMATODE PARASITES; FIG WASPS; EVOLUTION; HOST; COMPETITION; MUTUALISM AB Host-parasite dynamics can be altered when a host is infected by multiple parasite genotypes. The different strains of parasite are expected to compete for the limited host resources, potentially affecting the survival and reproduction of the host as well as the infecting parasites. Fungus-growing ants, including the well-known leaf-cutters, are an emerging model system for studying the evolution and ecology of symbiosis and host-parasite dynamics. We examine whether the fungus gardens of leaf-cutter ants can be simultaneously infected by multiple strains of the fungal pathogen Escovopsis. Intensive sampling of Escovopsis was conducted from individual gardens, as well as between different garden chambers within individual colonies of leaf-cutting ants. Isolates obtained were genotyped by DNA sequencing. We found that, minimally, 67% of the individual colonies of the leaf-cutter ant genera Atta and Acromyrmex and 50% of the At. colombica garden chambers studied were simultaneously infected by multiple distinct Escovopsis strains. Experimental challenges showed that different Escavopsis strains do not exhibit obvious antagonism toward each other, suggesting that coinfecting strains of the parasite do not engage in interference competition, although interactions were not studied at the cellular level. Further research is needed to understand interparasite interactions between coinfecting Escovopsis strains and to understand the impact of multiparasite infections on the survival of leaf-cutter ant gardens. C1 [Taerum, S. J.; Cafaro, M. J.; Currie, C. R.] Univ Kansas, Dept Ecol & Evolutionary Biol, Lawrence, KS 66045 USA. [Taerum, S. J.; Currie, C. R.] Smithsonian Trop Res Inst, Balboa, Panama. [Cafaro, M. J.; Currie, C. R.] Univ Wisconsin, Dept Bacteriol, Madison, WI 53706 USA. [Cafaro, M. J.] Univ Puerto Rico, Dept Biol, Mayaguez, PR 00681 USA. RP Currie, CR (reprint author), Univ Kansas, Dept Ecol & Evolutionary Biol, Lawrence, KS 66045 USA. EM currie@bact.wisc.edu RI Rinaldi2, Carlos/D-4479-2011 FU NSF [DEB-0110073, CAREER 0747002]; Smithsonian Tropical Research Institute; University of Kansas Plant Biology FX This work was supported by NSF (DEB-0110073 and CAREER 0747002) to C.R.C., a Smithsonian Tropical Research Institute short-term fellowship to S.J.T., and a University of Kansas Plant Biology research fellowship to S.J.T. We thank the Smithsonian Tropical Research Institute and the Autoridad Nacional del Ambiente of the Republic of Panama for research pen-nits. We also thank H. Alexander, O. Arosemena, A. Bilgray, K. Bolton, P. Cartwright, H. Fernandez, N. Gerardo, N. Gorosito, A. Herre, H. Herz, A. Himler, S. Ingram, G. Jarome, M. Leone, A. Little, R. Lichtwardt, C. Martin, E. McClain, E. McGee, U. Mueller, M. Poulsen, S. Price, S. Rehner, H. Reynolds, T. Schultz, J. Scott, T. Scott, D. Smith, S. Solomon, W. Weislo, and M. White for research assistance and/or invaluable comments. NR 52 TC 9 Z9 9 U1 4 U2 33 PU ENTOMOLOGICAL SOC AMER PI LANHAM PA 10001 DEREKWOOD LANE, STE 100, LANHAM, MD 20706-4876 USA SN 0046-225X J9 ENVIRON ENTOMOL JI Environ. Entomol. PD FEB PY 2010 VL 39 IS 1 BP 105 EP 113 DI 10.1603/EN09137 PG 9 WC Entomology SC Entomology GA 555GX UT WOS:000274498000011 PM 20146845 ER PT J AU Vincent, AG Turner, BL Tanner, EVJ AF Vincent, A. G. Turner, B. L. Tanner, E. V. J. TI Soil organic phosphorus dynamics following perturbation of litter cycling in a tropical moist forest SO EUROPEAN JOURNAL OF SOIL SCIENCE LA English DT Article ID P-31 NMR-SPECTROSCOPY; LOWLAND RAIN FORESTS; MULU-NATIONAL-PARK; NUTRIENT LIMITATION; VANCOUVER-ISLAND; TRANSFORMATIONS; PEDOGENESIS; EXTRACTION; GROWTH; IDENTIFICATION AB The productivity of tropical lowland moist forests is often considered to be limited by the availability of phosphorus. Organic phosphorus is often abundant in tropical soils, but its role in forest nutrition is largely unknown. We addressed this by using a large-scale litter manipulation experiment to investigate the stability of soil organic phosphorus in a tropical lowland forest in Central Panama. Three years of litter removal reduced the organic phosphorus concentration in the surface 2 cm of mineral soil by 23%, as determined by NaOH-EDTA extraction and 31P-NMR spectroscopy; this included decreases in phosphate monoesters (20%) and DNA (30%). Three years of litter addition (equivalent to adding 6 kg P ha-1 per year) increased soil organic phosphorus by 16%, which included a 31% increase in DNA. We did not detect higher-order inositol phosphates, despite their abundance in mineral soils of temperate ecosystems. Our observed turnover rate suggests that even the 0-2-cm layer of the mineral soil contributes a fifth of the total phosphorus needed to sustain above-ground growth in this forest. Soil organic phosphorus is thus likely to make a more important contribution to the nutrition of semi-evergreen forest plants than has hitherto been acknowledged. C1 [Vincent, A. G.; Tanner, E. V. J.] Univ Cambridge, Dept Plant Sci, Cambridge CB2 3EA, England. [Vincent, A. G.; Turner, B. L.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Vincent, AG (reprint author), Univ Cambridge, Dept Plant Sci, Cambridge CB2 3EA, England. EM andrea.vincent@emg.umu.se RI Turner, Benjamin/E-5940-2011; Vincent, Andrea /C-3989-2013 OI Turner, Benjamin/0000-0002-6585-0722; FU Smithsonian Tropical Research Institute (STRI); Mellon Foundation FX We thank Tania Romero (STRI) for help with laboratory analysis, Dr O. Phillips (University of Leeds, UK) and collaborators for access to their dataset on soil nutrient concentrations for South American forests and Drs Charles Shand (Macaulay Institute, Scotland) and David Coomes (University of Cambridge, UK) for valuable comments on the manuscript. Dr Emma Sayer (STRI) was the principal manager of the litter manipulation experiment. This work was funded by a Smithsonian Tropical Research Institute (STRI) fellowship to AGV and a Mellon Foundation grant to EVJT. This work was conducted at STRI in Panama, to whom we are grateful for logistical support. NR 59 TC 59 Z9 61 U1 4 U2 50 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1351-0754 J9 EUR J SOIL SCI JI Eur. J. Soil Sci. PD FEB PY 2010 VL 61 IS 1 BP 48 EP 57 DI 10.1111/j.1365-2389.2009.01200.x PG 10 WC Soil Science SC Agriculture GA 541XN UT WOS:000273454800005 ER PT J AU Ross, C Ritson-Williams, R Pierce, R Bullington, JB Henry, M Paul, VJ AF Ross, Cliff Ritson-Williams, Raphael Pierce, Richard Bullington, J. Bradley Henry, Michael Paul, Valerie J. TI Effects of the Florida red tide dinoflagellate, Karenia brevis, on oxidative stress and metamorphosis of larvae of the coral Porites astreoides SO HARMFUL ALGAE LA English DT Article DE Brevetoxin; Coral; Karenia brevis; Oxidative stress; Porites astreoides; Red tide ID MOLECULAR BIOMARKER SYSTEM; OYSTER CRASSOSTREA-VIRGINICA; MONTASTRAEA-FAVEOLATA; ANTHROPOGENIC STRESSORS; UV-RADIATION; BREVETOXINS; TEMPERATURE; RESPONSES; HEALTH; SETTLEMENT AB Florida red tides, caused by the dinoflagellate Karenia brevis, produce a series of neurotoxins, brevetoxins, which have historically had a negative impact on coastal communities along the South Florida coast. While much work has examined the effects of K. brevis blooms or exposure to brevetoxins on a diverse array of marine organisms, there have been no reports studying the impact of K. brevis on coral physiology. We provide evidence that short-term exposure of naturally occurring concentrations of K. brevis and their associated toxins can induce oxidative stress in the coral larvae of Porites astreoides. Larvae of A astreoides were exposed to aliquots of intact K. brevis cells at naturally occurring concentrations (6 x 10(5) - 4 x 10(6) cells L-1) or cellular lysates (containing 5.4-15.0 mu g L-1 brevetoxin) for 20 h and a variety of larval physiological biomarkers were measured. in the presence of bloom scale concentrations of K. brevis larval respiration of A astreoides was inhibited. This was accompanied with an increase in lipid hydroperoxide content and catalase activity indicating oxidative damage and a subsequent antioxidant response were occurring. However, when larvae were exposed to intact cells of K. brevis or their sonicated, lysed exudates stress indices including zooxanthellae expulsion (bleaching), larval protein carbonylation, and superoxide dismutase activity were not significantly altered. Even though there was evidence for short-term oxidative stress in larvae that were exposed to K. brevis there was no change in survival or settlement rates of larvae of P. astrecrides. (C) 2009 Elsevier B.V. All rights reserved. C1 [Ross, Cliff; Bullington, J. Bradley] Univ N Florida, Dept Biol, Jacksonville, FL 32246 USA. [Ritson-Williams, Raphael; Paul, Valerie J.] Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. [Pierce, Richard; Henry, Michael] Mote Marine Lab, Ctr Ecotoxicol, Sarasota, FL 34236 USA. RP Ross, C (reprint author), Univ N Florida, Dept Biol, 1 UNF Dr, Jacksonville, FL 32246 USA. EM cliff.ross@unf.edu RI Ross, Cliff/B-8291-2011 FU Mote Marine Laboratory [POR-2006-23] FX We thank Koty Sharp, Jason Kwan, Kathy Morrow, and Karen Arthur for assistance with coral collection and larval husbandry. We also thank Erich Bartels and Corey Walter for field assistance and brevetoxin extraction. We appreciate the efforts of Marc Hanke for GIS work. This work was supported by the "Protect Our Reefs" program through Mote Marine Laboratory, grant # POR-2006-23. This is contribution #797 of the Smithsonian Marine Station at Ft. Pierce.[SS] NR 49 TC 15 Z9 16 U1 3 U2 19 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1568-9883 EI 1878-1470 J9 HARMFUL ALGAE JI Harmful Algae PD FEB PY 2010 VL 9 IS 2 BP 173 EP 179 DI 10.1016/j.hal.2009.09.001 PG 7 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 549ZB UT WOS:000274093500006 ER PT J AU Archie, EA Henry, T Maldonado, JE Moss, CJ Poole, JH Pearson, VR Murray, S Alberts, SC Fleischer, RC AF Archie, Elizabeth A. Henry, Tammy Maldonado, Jesus E. Moss, Cynthia J. Poole, Joyce H. Pearson, Virginia R. Murray, Suzan Alberts, Susan C. Fleischer, Robert C. TI Major histocompatibility complex variation and evolution at a single, expressed DQA locus in two genera of elephants SO IMMUNOGENETICS LA English DT Article DE African elephant; Asian elephant; DQA; Major histocompatibility complex; Coding sequence; Molecular evolution ID WILD AFRICAN ELEPHANTS; CLASS-II LOCI; LOXODONTA-AFRICANA; KIN RECOGNITION; ENDOTHELIOTROPIC HERPESVIRUSES; NATIONAL-PARK; AMINO-ACID; MHC GENES; SELECTION; POLYMORPHISM AB Genes of the vertebrate major histocompatibility complex (MHC) are crucial to defense against infectious disease, provide an important measure of functional genetic diversity, and have been implicated in mate choice and kin recognition. As a result, MHC loci have been characterized for a number of vertebrate species, especially mammals; however, elephants are a notable exception. Our study is the first to characterize patterns of genetic diversity and natural selection in the elephant MHC. We did so using DNA sequences from a single, expressed DQA locus in elephants. We characterized six alleles in 30 African elephants (Loxodonta africana) and four alleles in three Asian elephants (Elephas maximus). In addition, for two of the African alleles and three of the Asian alleles, we characterized complete coding sequences (exons 1-5) and nearly complete non-coding sequences (introns 2-4) for the class II DQA loci. Compared to DQA in other wild mammals, we found moderate polymorphism and allelic diversity and similar patterns of selection; patterns of non-synonymous and synonymous substitutions were consistent with balancing selection acting on the peptides involved in antigen binding in the second exon. In addition, balancing selection has led to strong trans-species allelism that has maintained multiple allelic lineages across both genera of extant elephants for at least 6 million years. We discuss our results in the context of MHC diversity in other mammals and patterns of evolution in elephants. C1 [Archie, Elizabeth A.] Univ Notre Dame, Dept Biol Sci, Notre Dame, IN 46556 USA. [Archie, Elizabeth A.; Henry, Tammy; Maldonado, Jesus E.; Fleischer, Robert C.] Smithsonian Inst, Natl Zool Pk, Ctr Conservat & Evolutionary Genet, Washington, DC 20008 USA. [Archie, Elizabeth A.; Henry, Tammy; Maldonado, Jesus E.; Fleischer, Robert C.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. [Henry, Tammy] George Mason Univ, Dept Environm Sci & Policy, Fairfax, VA 22030 USA. [Moss, Cynthia J.; Poole, Joyce H.] Amboseli Trust Elephants, Nairobi, Kenya. [Pearson, Virginia R.] Philadelphia Zoo, Philadelphia, PA USA. [Alberts, Susan C.] Duke Univ, Dept Biol, Durham, NC USA. RP Archie, EA (reprint author), Univ Notre Dame, Dept Biol Sci, Notre Dame, IN 46556 USA. EM earchie@nd.edu FU Kenya Wildlife Service; Amboseli Elephant Research; Smithsonian Institution Abbott Endowment Fund; National Zoo's Institution Center for Conservation and Evolutionary Genetics; National Zoo; National Science Foundation [IBN0091612]; Amboseli Trust, Duke University FX We thank the Office of the President of Kenya for permission to work in Amboseli National Park under permit number MOES&T 13/001/30C 72/7. We thank the Kenya Wildlife Service for local sponsorship. We thank the Amboseli Elephant Research project for invaluable scientific and logistical support, particularly the team of N. Njiraini, K. Sayialel, and S. Sayialel who contributed greatly to the collection of genetic samples. We thank the Smithsonian National Zoo, the Philadelphia Zoo in Philadelphia, PA, the Gladys Porter Zoo in Brownsville, TX, and the Six Flags Wild Safari Park in Jackson, NJ for their support and cooperation in sample collection. This research was supported by the Smithsonian Institution Abbott Endowment Fund, the National Zoo's Institution Center for Conservation and Evolutionary Genetics, the Friends of the National Zoo, the National Science Foundation (IBN0091612 to SCA), the Amboseli Trust for Elephants, the Amboseli Elephant Research Project, and Duke University. NR 55 TC 12 Z9 12 U1 2 U2 18 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0093-7711 EI 1432-1211 J9 IMMUNOGENETICS JI Immunogenetics PD FEB PY 2010 VL 62 IS 2 BP 85 EP 100 DI 10.1007/s00251-009-0413-8 PG 16 WC Genetics & Heredity; Immunology SC Genetics & Heredity; Immunology GA 550ED UT WOS:000274110200003 PM 20058003 ER PT J AU Didham, RK Basset, Y Leather, SR AF Didham, Raphael K. Basset, Yves Leather, Simon R. TI Research needs in insect conservation and diversity SO INSECT CONSERVATION AND DIVERSITY LA English DT Editorial Material ID FOOD WEBS; HABITAT MODIFICATION; SPECIES-DIVERSITY; SAMPLING METHODS; RAIN-FOREST; DISTURBANCE; COMMUNITIES; BUTTERFLIES; LANDSCAPES; ECOSYSTEMS C1 [Didham, Raphael K.] Univ Western Australia, Sch Anim Biol, Crawley, WA 6009, Australia. [Didham, Raphael K.] Ctr Environm & Life Sci, CSIRO Entomol, Floreat, WA, Australia. [Didham, Raphael K.] Univ Canterbury, Sch Biol Sci, Christchurch 1, New Zealand. [Basset, Yves] Smithsonian Trop Res Inst, Panama City, Panama. [Leather, Simon R.] Imperial Coll London, Div Biol, Ascot, Berks, England. RP Didham, RK (reprint author), Univ Western Australia, Sch Anim Biol, 35 Stirling Highway, Crawley, WA 6009, Australia. EM raphael.didham@uwa.edu.au RI Didham, Raphael/B-5953-2011; Basset, Yves/B-6642-2014; OI Leather, Simon/0000-0003-3007-8514 NR 40 TC 12 Z9 12 U1 3 U2 16 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 1752-458X J9 INSECT CONSERV DIVER JI Insect. Conserv. Divers. PD FEB PY 2010 VL 3 IS 1 BP 1 EP 4 DI 10.1111/j.1752-4598.2009.00076.x PG 4 WC Biodiversity Conservation; Entomology SC Biodiversity & Conservation; Entomology GA 540CW UT WOS:000273309400001 ER PT J AU Harbaugh, DT Nepokroeff, M Rabeler, RK McNeill, J Zimmer, EA Wagner, WL AF Harbaugh, Danica T. Nepokroeff, Molly Rabeler, Richard K. McNeill, John Zimmer, Elizabeth A. Wagner, Warren L. TI A NEW LINEAGE-BASED TRIBAL CLASSIFICATION OF THE FAMILY CARYOPHYLLACEAE SO INTERNATIONAL JOURNAL OF PLANT SCIENCES LA English DT Article DE Alsinoideae; Caryophyllaceae; Eremogoneae; molecular phylogeny; Schiedea ID PHYLOGENETIC ANALYSIS; SILENEAE CARYOPHYLLACEAE; CHLOROPLAST DNA; SEQUENCE DATA; ALSINIDENDRON CARYOPHYLLACEAE; NUCLEAR RDNA; GENE; EVOLUTION; MATK; SCHIEDEA AB Understanding the relationships within the Caryophyllaceae has been difficult, in part because of arbitrarily and poorly defined genera and difficulty in determining phylogenetically useful morphological characters. This study represents the most complete phylogenetic analysis of the family to date, with particular focus on the genera and relationships within the large subfamily Alsinoideae, using molecular characters to examine the monophyly of taxa and the validity of the current taxonomy as well as to resolve the obscure origins of divergent taxa such as the endemic Hawaiian Schiedea. Maximum parsimony and maximum likelihood analyses of three chloroplast gene regions (matK, trnL-F, and rps16) from 81 newly sampled and 65 GenBank specimens reveal that several tribes and genera, especially within the Alsinoideae, are not monophyletic. Large genera such as Arenaria and Minuartia are polyphyletic, as are several smaller genera. The phylogenies reveal that the closest relatives to Schiedea are a pair of widespread, largely Arctic taxa, Honckenya peploides and Wilhelmsia physodes. More importantly, the three traditional subfamilies (Alsinoideae, Caryophylloideae, and Paronychioideae) are not reflective of natural groups; we propose abandoning this classification in favor of a new system that recognizes major lineages of the molecular phylogeny at the tribal level. A new tribe, Eremogoneae Rabeler & W.L. Wagner, is described here. C1 [Harbaugh, Danica T.; Zimmer, Elizabeth A.; Wagner, Warren L.] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. [Nepokroeff, Molly] Univ S Dakota, Dept Biol, Vermillion, SD 57069 USA. [Rabeler, Richard K.] Univ Michigan Herbarium, Ann Arbor, MI 48108 USA. [McNeill, John] Royal Bot Garden, Edinburgh EH3 5LR, Midlothian, Scotland. RP Harbaugh, DT (reprint author), Univ Calif Berkeley, Univ & Jepson Herbaria, Dept Integrat Biol, 1001 Valley Life Sci Bldg, Berkeley, CA 94720 USA. EM danicah@berkeley.edu RI Zimmer, Elizabeth/G-3890-2011 FU Smithsonian Institution Scholarly Studies program; Botany Department; Office of Research, University of South Dakota; National Tropical Botanical Garden McBryde Senior Research Fellowship; NSF [DEB 0445410] FX This study was funded in part by a grant from the Smithsonian Institution Scholarly Studies program to W. L. Wagner, M. Nepokroeff, and E. A. Zimmer and a fellowship from the Botany Department to D. T. Harbaugh, as well as by funds from the Office of Research, University of South Dakota, to M. Nepokroeff. In addition, M. Nepokroeff was supported by the National Tropical Botanical Garden McBryde Senior Research Fellowship program during analysis of these data and by funds from NSF grant DEB 0445410. We thank B. Jacobs, C. Krogman, and C. Griffith at the University of South Dakota, as well as M. Van Horn and C. McCracken at the Smithsonian, for laboratory assistance. We also thank the following individuals, who supplied leaf material for this study: L. Ahart, F. Ashby, C. Best, B. Castro, M. Chase, L. Consaul, S. Downie, L. Gillespie, S. Gonzales, J. R. Grant, M. Hershkovitz, L. Janeway, D. Lorence, K. McCue, R. Muriillo, D. Murray, C. Parker, S. Perlman, A. Sakai, A. Santos, P. Sklenar, R. Smissen, R. Soreng, M. E. Timana, S. Weller, R. Worthington, and S. Zamudio. Finally, we thank B. Baldwin and C. Hobbs for assisting D. T. Harbaugh with phylogenetic analyses and P. Julian and T. Wendt for assisting W. L. Wagner with field collections. NR 70 TC 44 Z9 53 U1 3 U2 24 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 FEB PY 2010 VL 171 IS 2 BP 185 EP 198 DI 10.1086/648993 PG 14 WC Plant Sciences SC Plant Sciences GA 543YB UT WOS:000273616100006 ER PT J AU Gingerich, O AF Gingerich, Owen TI Astrology, Print Works (1472-1900). 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. NR 1 TC 0 Z9 0 U1 0 U2 1 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 FEB PY 2010 VL 41 BP 143 EP 144 PN 1 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA 576FQ UT WOS:000276130100021 ER PT J AU Gingerich, O AF Gingerich, Owen TI Galileo: Images of the Universe from Antiquity to the Telescope 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. NR 1 TC 0 Z9 0 U1 1 U2 1 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 FEB PY 2010 VL 41 BP 145 EP 146 PN 1 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA 576FQ UT WOS:000276130100023 ER PT J AU Zeder, MA Pilaar, SE AF Zeder, Melinda A. Pilaar, Suzanne E. TI Assessing the reliability of criteria used to identify mandibles and mandibular teeth in sheep, Ovis, and goats, Capra SO JOURNAL OF ARCHAEOLOGICAL SCIENCE LA English DT Review DE Ovicaprids; Dental taxonomic criteria harvest profiles ID MORPHOLOGICAL DISTINCTIONS AB Criteria developed to distinguish between the mandibles and mandibular teeth of sheep and goats are evaluated using modern specimens from the collections of the National Museum of Natural History and the Field Museum of Natural History. Certain teeth prove to be quite reliable in this regard (dP3, P3, P4). Other dental elements, however, are not reliable and should not be used in dental based identifications of these closely related species (dP4, M1, and mandibular bones). Overall, the identification of sheep dentition using these criteria is more reliable than it is for goats. However, the generally greater likelihood of incorrect identification of goat teeth and mandibles means that specimens identified as sheep are likely to contain high proportion of misidentified goats. Both the proportion of remains that can only be classified as 'Ovis-Capra' and the proportion of incorrectly identified teeth and mandibular bones varies with age, with identifications of younger and older animals less reliable than those of animals in the 1.5-6 year age range. Reliability of identifications increases when more criteria and more elements are used. Identifications based on whole mandibles with complete tooth rows are quite reliable. However, the proportion of specimens likely to be classified as 'Ovis-Capra' also increases in whole mandible identifications, especially in goats. Systematic differences in the proportions of indeterminate and incorrect identifications have a significant impact on species-level dentition-based harvest profiles. Recommendations are made for the use of dentition and long bone based harvest profiles in the study of sheep and goat exploitation strategies. Published by Elsevier Ltd. C1 [Zeder, Melinda A.] Smithsonian Inst, Natl Museum Nat Hist, Archaeobiol Program, Washington, DC 20560 USA. [Pilaar, Suzanne E.] Univ Cambridge, Dept Archaeol, Cambridge CB2 3D, England. RP Zeder, MA (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Archaeobiol Program, Washington, DC 20560 USA. EM zederm@si.edu OI Pilaar Birch, Suzanne/0000-0003-1544-5881 FU NMNH FX The authors would like to thank the Department of Vertebrate Zoology, NMNH and the Department of Zoology, FMNH for access to collections used in this study; the NMNH Research Training Program for Pilaar's support while at the Smithsonian: and Marcia Bakry for her work on the figures. This paper has benefited from the thoughtful comments of Umberto Albarella, jean-Denis Vigne, and one annonymous reviewer. NR 27 TC 30 Z9 30 U1 1 U2 2 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 FEB PY 2010 VL 37 IS 2 BP 225 EP 242 DI 10.1016/j.jas.2009.10.002 PG 18 WC Anthropology; Archaeology; Geosciences, Multidisciplinary SC Anthropology; Archaeology; Geology GA 536WA UT WOS:000273073400001 ER PT J AU Messner, TC Schindler, B AF Messner, Timothy C. Schindler, Bill TI Plant processing strategies and their affect upon starch grain survival when rendering Peltandra virginica (L.) Kunth, Araceae edible SO JOURNAL OF ARCHAEOLOGICAL SCIENCE LA English DT Article DE Paleoethnobotany; Starch grain analysis; Experimental archaeology; Eastern North America; Plant processing; Archaeobotany ID REAL-ALTO SITE; STONE TOOLS; MAIZE; ECUADOR; AGRICULTURE; PHYTOLITHS; ESCULENTA; COOKING; PANAMA; ROOT AB There is a long history of human interaction with plants of the Aroideae subfamily (Araceae). Despite these plants' chemical defenses against animal and vegetal predation, humans have targeted their starchy corms, tubers and rhizomes for dietary purposes. In the Eastern Woodlands of North America, early Europeans described the Native population as utilizing the highly acridic Peltandra virginica (arrow arum) for subsistence needs. In order to render this resource edible, however, the acridic principle first needs to be eliminated. Our study investigates the affect these processing activities have on the integrity of arrow arum starch grains. Findings from this study demonstrate that environmental variables specific to individual processing procedures may be more influential on starch grain survival than simply the temperatures reached during cooking. (C) 2009 Elsevier Ltd. All rights reserved. C1 [Messner, Timothy C.] Smithsonian NMNH, Suitland, MD 20746 USA. [Schindler, Bill] Washington Coll, Chestertown, MD 21620 USA. RP Messner, TC (reprint author), Smithsonian NMNH, 4210 Silver Hill Rd, Suitland, MD 20746 USA. EM messnert@si.edu FU National Science Foundation FX Thanks are extended to Wayne Henderick and staff at Washington's Crossing State Park, NJ for use of their facilities. Dr. Dolores Piperno, Dr. Sandhya Ganapathy and Christina Schindler for their comments on drafts of this paper. Also, thanks to the Department of Anthropology at Temple University for use of their laboratory facilities. TCM was funded in part by a National Science Foundation dissertation improvement grant. NR 44 TC 12 Z9 13 U1 0 U2 14 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 FEB PY 2010 VL 37 IS 2 BP 328 EP 336 DI 10.1016/j.jas.2009.09.044 PG 9 WC Anthropology; Archaeology; Geosciences, Multidisciplinary SC Anthropology; Archaeology; Geology GA 536WA UT WOS:000273073400011 ER PT J AU Andersen, KM Turner, BL Dalling, JW AF Andersen, Kelly M. Turner, Benjamin L. Dalling, James W. TI Soil-based habitat partitioning in understorey palms in lower montane tropical forests SO JOURNAL OF BIOGEOGRAPHY LA English DT Article DE Arecaceae; base cations; community assembly; floristic similarity; habitat associations; nitrogen; Panama ID AMAZONIAN RAIN-FOREST; BETA-DIVERSITY; EDAPHIC SPECIALIZATION; RECRUITMENT LIMITATION; MESOSCALE DISTRIBUTION; DISTRIBUTION PATTERNS; GEONOMA-MACROSTACHYS; SPECIES COMPOSITION; DNA-SEQUENCES; ARECACEAE AB Aim Dispersal assembly and niche assembly are two competing theories proposed to explain the maintenance of species diversity in tropical forests. Dispersal theory emphasizes the role of chance colonization events and distance-limited seed dispersal in explaining species abundance and distribution, whereas niche theory emphasizes differences among species in requirements for potentially limiting resources. Species distribution patterns in tropical forests often correlate with geology and topography, but tests of the relative importance of dispersal and niche partitioning have been hampered by an inadequate characterization of resource availability. The aim of this study was to explore how soil chemical and physical properties, climate, and geographic distance affect understorey palm communities in lower montane forests. Location Fortuna Forest Reserve, Chiriqui Province, and Palo Seco Forest Reserve, Bocas del Toro Province, in western Panama. Methods Understorey palms and soil nutrient concentrations were surveyed within 10 sites on different soil types across a 13-km transect. Variation in palm community composition was examined in relation to spatial and environmental variables. Results The 25 understorey palm species recorded in the study were non-randomly distributed among forests differing in soil nutrient availability. In support of dispersal theory, floristic similarity decreased predictably with increasing geographic distance. However, environmental and soil variables were also correlated with geographic distance. Floristic similarity was also highly associated with a subset of environmental variables. Variation in palm community similarity was most strongly correlated with inorganic nitrogen availability and cation concentration. A subset of soil variables had a stronger relationship with floristic similarity when geographic distance was controlled for than did geographic distance when differences in soils were controlled for. Main conclusions Both dispersal and niche processes affect palm species distribution patterns. Although spatially limited dispersal may influence species distribution patterns, soil-based habitat associations, particularly with respect to soil nitrogen, cation availability and aluminium concentrations, remain important factors influencing palm community composition at the mesoscale level in this tropical montane forest. C1 [Andersen, Kelly M.] Univ Illinois, Program Ecol & Evolutionary Biol, Urbana, IL 61801 USA. [Turner, Benjamin L.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Dalling, James W.] Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA. RP Andersen, KM (reprint author), Univ Illinois, Program Ecol & Evolutionary Biol, Urbana, IL 61801 USA. EM kanderse@life.uiuc.edu RI Turner, Benjamin/E-5940-2011; OI Turner, Benjamin/0000-0002-6585-0722; Andersen, Kelly/0000-0002-1460-9904 FU NSF [DEB 06-08198]; Smithsonian Institute FX We thank the Smithsonian Tropical Research Institute and Enel Fortuna for logistical support. This research was supported by a Dissertation Completion Grant (NSF DEB 06-08198) and a Smithsonian Institute Predoctoral Fellowship to K. M. A. We thank Edevelio 'Bady' Garcia and Arturo Morris for technical assistance and Milton Solano for constructing a map of our sites. Kyle Harms and an anonymous revferee provided valuable comments on the manuscript. NR 77 TC 33 Z9 37 U1 0 U2 26 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0305-0270 J9 J BIOGEOGR JI J. Biogeogr. PD FEB PY 2010 VL 37 IS 2 BP 278 EP 292 DI 10.1111/j.1365-2699.2009.02192.x PG 15 WC Ecology; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA 545XU UT WOS:000273771100008 ER PT J AU Baugh, AT Ryan, MJ AF Baugh, Alexander T. Ryan, Michael J. TI The Development of Sexual Behavior in Tungara Frogs (Physalaemus pustulosus) SO JOURNAL OF COMPARATIVE PSYCHOLOGY LA English DT Article DE acoustic communication; locomotor; ontogeny; phonotaxis; sexual behavior ID FEMALE MATE CHOICE; BULLFROG RANA-CATESBEIANA; WHITE-CROWNED SPARROWS; MATING CALL PHONOTAXIS; ARGININE VASOTOCIN; ACOUSTIC COMMUNICATION; CONSPECIFIC ATTRACTION; AUDITORY-SENSITIVITY; SPECIES-DIFFERENCES; INNATE RECOGNITION AB We examined the emergence of a critical component of sex, response to sexual signals-phonotaxis-in male and female tungara frogs (Physalaemus pustulosus). We determined the ontogenetic trajectories of phonotactic responses as animals developed from metamorphic froglets to reproductive adults. The results demonstrated that species-typical phonotaxis emerges quite early during postmetamorphic development, well before sexual maturity, suggesting that a developmentally early bias in the auditory system for species-typical signals might be a more general phenomenon than previously thought, and that the neural circuits responsible for processing and responding to conspecific advertisement signals in a species-typical manner might develop long before the coordinated behavior is demanded of the organism. C1 [Baugh, Alexander T.; Ryan, Michael J.] Univ Texas Austin, Sect Integrat Biol, Austin, TX 78712 USA. [Baugh, Alexander T.] Univ Texas Austin, Inst Neurosci, Austin, TX 78712 USA. [Ryan, Michael J.] Smithsonian Trop Res Inst, Balboa Ancon, Panama. RP Baugh, AT (reprint author), Univ Texas Austin, Sect Integrat Biol, 1 Univ Stn C0930, Austin, TX 78712 USA. EM alex.baugh@gmail.com RI Baugh, Alexander/E-4777-2010; OI Baugh, Alexander/0000-0003-2032-892X NR 82 TC 11 Z9 11 U1 0 U2 8 PU AMER PSYCHOLOGICAL ASSOC PI WASHINGTON PA 750 FIRST ST NE, WASHINGTON, DC 20002-4242 USA SN 0735-7036 J9 J COMP PSYCHOL JI J. Comp. Psychol. PD FEB PY 2010 VL 124 IS 1 BP 66 EP 80 DI 10.1037/a0017227 PG 15 WC Behavioral Sciences; Psychology; Psychology, Multidisciplinary; Zoology SC Behavioral Sciences; Psychology; Zoology GA 566QY UT WOS:000275389300007 PM 20175598 ER PT J AU Peretti, AV Eberhard, WG AF Peretti, A. V. Eberhard, W. G. TI Cryptic female choice via sperm dumping favours male copulatory courtship in a spider SO JOURNAL OF EVOLUTIONARY BIOLOGY LA English DT Article DE copulatory courtship; cryptic female choice; paternity; sexual selection; sperm usage; spiders ID MATING-BEHAVIOR; GENITAL MORPHOLOGY; PATERNITY SUCCESS; DRYOMYZA-ANILIS; WATER STRIDERS; D. SERRATA; INSECTS; DROSOPHILA; STORAGE; ARANEAE AB Males of many animals perform `copulatory courtship' during copulation, but the possible reproductive significance of this behaviour has seldom been investigated. In some animals, including the spider Physocyclus globosus (Pholcidae), the female discards sperm during or immediately following some copulations. In this study, we determined which of several variables associated with copulation correlated with paternity success in P. globosus when two males mate with a single female. Then, by determining which of these variables also correlated with sperm dumping, we inferred which variables may affect paternity via the mechanism of sperm dumping. Male abdomen vibration (a copulatory courtship behaviour) and male genitalic squeezing both correlated with both paternity and sperm dumping; so, these traits may be favoured by biased sperm dumping. Biased sperm dumping may also be the mechanism by which possible cryptic female choice favours another male trait that was the subject of a previous study, responsiveness to female stridulation. C1 [Peretti, A. V.] Natl Univ Cordoba, Dept Ecol & Divers, Lab Reprod Biol & Evolut, CONICET,Catedra Anim Divers 1, RA-5000 Cordoba, Argentina. [Eberhard, W. G.] Univ Costa Rica, Smithsonian Trop Res Inst, San Jose, Costa Rica. [Eberhard, W. G.] Univ Costa Rica, Escuela Biol, San Jose, Costa Rica. RP Peretti, AV (reprint author), Natl Univ Cordoba, Dept Ecol & Divers, Lab Reprod Biol & Evolut, CONICET,Catedra Anim Divers 1, Velez Sarsfield 299, RA-5000 Cordoba, Argentina. EM aperetti@com.uncor.edu FU Consejo Nacional de Investigaciones Cientificas y Tecnicas; SECYT UNC; FONCYT of Argentina; PROMEP; Universidad Autonoma del Estado de Hidalgo, Mexico; Smithsonian Tropical Research Institute; Vicerrectoria de Investigacion of the Universidad de Costa Rica FX We thank Gilbert Barrantes, Bernhard Huber, Gabriele Uhl, Anita Aisenberg and Mary Jane West-Eberhard for helpful comments on the manuscript and statistical advice, Bernhard Huber for identifying spiders and sending the sections, Hernan Camacho (UCR) and Dario Mendez (ININ, Mexico) for irradiating males, and Mario Segura-Almaraz for technical assistance with video recordings. Two anonymous referees gave helpful critical comments on a previous version of the manuscript. Financial support was provided by the Consejo Nacional de Investigaciones Cientificas y Tecnicas, SECYT UNC, and FONCYT of Argentina, PROMEP and the Universidad Autonoma del Estado de Hidalgo, Mexico to A.V.P., and by the Smithsonian Tropical Research Institute and the Vicerrectoria de Investigacion of the Universidad de Costa Rica to W.G.E. NR 45 TC 17 Z9 17 U1 2 U2 38 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1010-061X J9 J EVOLUTION BIOL JI J. Evol. Biol. PD FEB PY 2010 VL 23 IS 2 BP 271 EP 281 DI 10.1111/j.1420-9101.2009.01900.x PG 11 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 544DN UT WOS:000273632800004 PM 20487130 ER PT J AU Buchwald, R Dudley, R AF Buchwald, R. Dudley, R. TI Limits to vertical force and power production in bumblebees (Hymenoptera: Bombus impatiens) SO JOURNAL OF EXPERIMENTAL BIOLOGY LA English DT Article DE allometry; Bombus; bumblebee; flight; hindwing; hovering; power ID HOVERING INSECT FLIGHT; ORCHID BEES APIDAE; WING WEAR; AERODYNAMICS; KINEMATICS; PERFORMANCE; EUGLOSSINI; ENERGETICS; ALLOMETRY AB Maximum vertical forces produced by flying animals can be difficult to identify unequivocally, but potentially indicate general limits to aerodynamic force and muscle power output. We used two methods (i.e. incremental addition of supplemental mass and asymptotic load lifting) to determine both the intraspecific allometry of and methodological differences in estimates of maximum flight performance for the bumblebee Bombus impatiens. We found that incremental mass addition underestimated maximum lifting capacity by approximately 18% relative to values obtained by asymptotically increasing the applied load during a lifting bout. In asymptotic loading, bumblebees lifted on average 53% of their body weight, and demonstrated a significantly negative allometry of maximum aerodynamic force production relative to thoracic muscle mass. Estimates of maximum body mass-specific mechanical power output increased intraspecifically with body mass to the 0.38-0.50 power, depending on values assumed for the profile drag coefficient. We also found a significant reduction in vertical force production when both hindwings were removed. Limits to load-lifting capacity ultimately co-occur with an upper bound on stroke amplitude (similar to 145 deg.). Although thoracic muscle mass showed positive allometry, overall load-lifting performance exhibited significant size-dependent degradation. C1 [Buchwald, R.; Dudley, R.] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. [Dudley, R.] Smithsonian Trop Res Inst, Balboa, Panama. RP Buchwald, R (reprint author), Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. EM rbuchwald@gmail.com FU NSF [DBI-0610265, DEB-0543556] FX We thank Koppert Biological for assistance with bumblebee colonies, and the NSF (DBI-0610265 and DEB-0543556) for research support. Michael Dillon and multiple anonymous reviewers provided invaluable comments on the manuscript. NR 19 TC 25 Z9 25 U1 1 U2 23 PU COMPANY OF BIOLOGISTS LTD PI CAMBRIDGE PA BIDDER BUILDING CAMBRIDGE COMMERCIAL PARK COWLEY RD, CAMBRIDGE CB4 4DL, CAMBS, ENGLAND SN 0022-0949 J9 J EXP BIOL JI J. Exp. Biol. PD FEB 1 PY 2010 VL 213 IS 3 BP 426 EP 432 DI 10.1242/jeb.033563 PG 7 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 545GO UT WOS:000273720700013 PM 20086127 ER PT J AU Jung, K Kalko, EKV AF Jung, Kirsten Kalko, Elisabeth K. V. TI Where forest meets urbanization: foraging plasticity of aerial insectivorous bats in an anthropogenically altered environment SO JOURNAL OF MAMMALOGY LA English DT Article DE acoustic monitoring; anthropogenie influence; artificial light; bat activity; chiroptera; habitat plasticity; moon ID FREE-TAILED BATS; ACTIVITY PATTERNS; TROPICAL FOREST; PREDATION RISK; ECHOLOCATION; CHIROPTERA; MOLOSSIDAE; ABUNDANCE; INSECTS; IDENTIFICATION AB Given worldwide rapid human population growth resulting in degradation or loss of habitats. it is important to understand how antrhopogenic Factors affect species presence and activity. and consequently, how well species tolerate or adapt to anthropogenically altered environments This Study, conducted in Panama, focuses on aerial insectivorous hats, a highly mobile and ecologically important. bill largely understudied group Acoustic monitoring Was used to Investigate habitat use in a tropical forest-town interface and microhabitat use around streetlights differing, in wavelength (type of light) and accessibility (distance to vegetation). Plasticity in microhabitat use also was examined in relation to season and moonlight We recorded it total of 25 aerial insectivorous bat species in the Study area and found it subset of 20 species in town of which 18 frequently foraged around streetlights Bat activity (passes/min) was lowest at the forest site. highest at streetlights,. and Intermediate in the dark areas of town General bat activity at streetlights was concentrated at blush-white lights compared to vellow-white and orange lights However, bats revealed species-specit'ic inicrohabitats with regard to light type. distance to vegetation, and relative light intensity Season and moon phase affected microhabitat use around streetlights leading to microhabitat plasticity of individual species. Thus, in the forest-town interface most, but not all, aerial insectivorous bats were present in town and regularly foraged around streetlights, suggesting a species-specific tolerance for habitat alteration. Bats foraging at streetlights used microhabitats, and some species even changed microhabitats, according to season or moon phase. The indicates species-specific requirements for microhabitats and the importance of preserving habitat heterogeneity DOI.10.1644/08-MAMM-A-313R.1 C1 [Jung, Kirsten] Univ Ulm, Inst Expt Ecol, D-89069 Ulm, Germany. [Kalko, Elisabeth K. V.] Smithsonian Trop Res Inst, Balboa, Panama. RP Jung, K (reprint author), Univ Ulm, Inst Expt Ecol, Albert Einstein Allee 11, D-89069 Ulm, Germany. NR 50 TC 32 Z9 33 U1 6 U2 64 PU ALLIANCE COMMUNICATIONS GROUP DIVISION ALLEN PRESS PI LAWRENCE PA 810 EAST 10TH STREET, LAWRENCE, KS 66044 USA SN 0022-2372 J9 J MAMMAL JI J. Mammal. PD FEB PY 2010 VL 91 IS 1 BP 144 EP 153 DI 10.1644/08-MAMM-A-313R.1. PG 10 WC Zoology SC Zoology GA 560UR UT WOS:000274929300016 ER PT J AU Cardona, A Chew, D Valencia, VA Bayona, G Miskovic, A Ibanez-Mejia, M AF Cardona, A. Chew, D. Valencia, V. A. Bayona, G. Miskovic, A. Ibanez-Mejia, M. TI Grenvillian remnants in the Northern Andes: Rodinian and Phanerozoic paleogeographic perspectives SO JOURNAL OF SOUTH AMERICAN EARTH SCIENCES LA English DT Article DE Grenville; Northern Andes; Terrane dispersion; Paleogeography ID U-PB GEOCHRONOLOGY; SOUTHERN MEXICO; OAXACAN COMPLEX; COLOMBIAN ANDES; TECTONIC IMPLICATIONS; ZIRCON GEOCHRONOLOGY; AMAZON CRATON; RB-SR; GUICHICOVI COMPLEX; PALEOZOIC ROCKS AB Grenvillian crust is encountered in several basement inliers in the northern Andes of Colombia, Ecuador and Peru and is also represented as a major detrital or inherited component within Neoproterozoic to Paleozoic sedimentary and magmatic rocks. This review of the tectonic and geochronological record of the Grenvillian belt in the northern Andes suggests that these crustal segments probably formed on an active continental margin in which associated arc and back-arc magmatism evolved from ca. 1.25 to 1.16 Ga, possibly extending to as young as 1.08 Ga. The lithostratigraphic and tectonic history of the Grenvillian belt in the northern Andes differs from that of the Sunsas belt on the southwest Amazonian Craton and from the Grenvillian belt of Eastern Laurentia. It is considered that this belt, along with similar terranes of Grenvillian age in Middle America and Mexico define a separate composite orogen which formed on the northwestern margin of the Amazonian Craton. Microcontinent accretion and interaction with the Sveconorwegian province on Baltica is a feasible tectonic scenario, in line with recent paleogeographic reconstructions of the Rodinian supercontinent. Although Phanerozoic tectonics may have redistributed some of these terranes, they are still viewed as para-autocthonous domains that remained in proximity to the margin of Amazonia. Paleogeographic data derived from Phanerozoic rocks suggest that some of the Colombian Grenvillian fragments were connected to northernmost Peru and Ecuador until the Mesozoic, whereas the Mexican terranes where attached to the Colombian margin until Pangea fragmentation in Late Triassic times. (C) 2009 Elsevier Ltd. All rights reserved. C1 [Cardona, A.] Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archeol, Balboa, Ancon, Panama. [Chew, D.] Univ Dublin Trinity Coll, Dept Geol, Dublin 2, Ireland. [Valencia, V. A.; Ibanez-Mejia, M.] Univ Arizona, Dept Geosci, Tucson, AZ 85721 USA. [Bayona, G.] Corp Geol Ares, Bogota, Colombia. [Miskovic, A.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. RP Cardona, A (reprint author), Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archeol, Balboa, Ancon, Panama. EM CardonaA@si.edu RI Chew, David/B-7828-2008; OI Chew, David/0000-0002-6940-1035; Ibanez-Mejia, Mauricio/0000-0002-7839-2425 NR 102 TC 32 Z9 33 U1 0 U2 2 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 FEB PY 2010 VL 29 IS 1 SI SI BP 92 EP 104 DI 10.1016/j.jsames.2009.07.011 PG 13 WC Geosciences, Multidisciplinary SC Geology GA 559QF UT WOS:000274840300008 ER PT J AU Pisera, A Rutzler, K Kaz'mierczak, J Kempe, S AF Pisera, Andrzej Ruetzler, Klaus Kaz'mierczak, Jozef Kempe, Stephan TI Sponges in an extreme environment: suberitids from the quasi-marine Satonda Island crater lake (Sumbawa, Indonesia) SO JOURNAL OF THE MARINE BIOLOGICAL ASSOCIATION OF THE UNITED KINGDOM LA English DT Article DE suberitid sponges; extreme environment; gemmules; Satonda Island; Indonesia ID MICROBIALITE FORMATION; INCREASED ALKALINITY; SEAWATER; SEA AB Sponges are rare in extreme environments, and very little is known about their adaptations to such settings. Evidence from two species in a marine-derived midwater stratified crater lake on Satonda Island (Sumbawa, Indonesia) suggests their production of gemmules (resting bodies), a rare trait in marine sponges but common in freshwater forms, may be a survival mechanism in the lake's harsh environment. With its epilimnion hydrochemistry-characterized by changing alkalinity, salinity, and O(2) levels over the region's wet and dry seasons-the lake sustains only a few marine macroscopic organisms, among them the suberitid sponges Protosuberites lacustris comb. nov. and Suberites sp. (Hadromerida: Suberitida). Both species belong to the same group as sponges reported from other marine-derived lakes with strongly varying and extreme environmental (especially chemical) parameters. The morphological characters, taxonomic position, ecological adaptations, environmental conditions, and biota associated with the sponges in this ecologically unique site are presented here. C1 [Pisera, Andrzej; Kaz'mierczak, Jozef] Polish Acad Sci, Inst Paleobiol, PL-00818 Warsaw, Poland. [Ruetzler, Klaus] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA. [Kempe, Stephan] Tech Univ Darmstadt, Inst Appl Geosci, D-64287 Darmstadt, Germany. RP Pisera, A (reprint author), Polish Acad Sci, Inst Paleobiol, Twarda 51-55, PL-00818 Warsaw, Poland. EM apis@twarda.pan.pl RI Kempe, Stephan/A-8450-2008; Pisera, Andrzej/F-4429-2011 FU Deutsche Forschungsgemeinschaft (DFG) [Ke 287 9/1-4]; Polish Academy of Sciences and the Committee for Scientific Research (KBN) [6 6209 92 03] FX We are indebted to G. Landmann, A. Lipp, A. Reimer, J. Reimer, T. Strecker and G. Worheide for their assistance in the field and in the laboratory. Field research was funded by the Deutsche Forschungsgemeinschaft (DFG) (Grant Ke 287 9/1-4, Satonda). Financial support by the Polish Academy of Sciences and the Committee for Scientific Research (KBN) (Grant 6 6209 92 03) is gratefully acknowledged. SYNTH ESYS grants (EU) to A. Pisera are also greatly appreciated. NR 32 TC 2 Z9 2 U1 1 U2 7 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0025-3154 J9 J MAR BIOL ASSOC UK JI J. Mar. Biol. Assoc. U.K. PD FEB PY 2010 VL 90 IS 1 BP 203 EP 212 DI 10.1017/S0025315409990968 PG 10 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 582NU UT WOS:000276605500014 ER PT J AU Aiello, A AF Aiello, Annette TI Insectopedia SO LIBRARY JOURNAL LA English DT Book Review C1 [Aiello, Annette] Smithsonian Trop Res Inst, Ancon, Panama. RP Aiello, A (reprint author), Smithsonian Trop Res Inst, Ancon, Panama. 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 FEB 1 PY 2010 VL 135 IS 2 BP 89 EP 89 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 549ZN UT WOS:000274094800196 ER PT J AU Guz, SS AF Guz, Savannah Schroll TI Almanac of the Infamous, the Incredible, and the Ignored 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 FEB 1 PY 2010 VL 135 IS 2 BP 96 EP 96 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 549ZN UT WOS:000274094800213 ER PT J AU Vargas, S Breedy, O Siles, F Guzman, HM AF Vargas, Sergio Breedy, Odalisca Siles, Francisco Guzman, Hector M. TI How many kinds of sclerite? Towards a morphometric classification of gorgoniid microskeletal components SO MICRON LA English DT Review DE Gorgoniidae; Octocorallia; Octocoral systematics; Pacifigorgia; Sclerite morphometrics ID GENUS PACIFIGORGIA COELENTERATA; EASTERN PACIFIC; OCTOCORALLIA; REVISION AB Gorgoniid octocorals constitute a diverse group of organisms that inhabit a wide range of marine environments. The group is currently defined by the presence of calcareous sclerites that are less than 0.3 mm in length with regularly arranged warts. Generic and specific classification schemes are based on the presence/absence of different sclerite classes in the sampled specimen as well as the frequency in which each class occurs in the sample. Sclerite classification typically has been difficult because a continuum of sclerite forms is found within and between species. Thus, the use of sclerites for phylogenetic inference and classification is problematic. Herein, we present a methodology to obtain quantitative measurements of large numbers of sclerites and used finite mixture modeling to assess the number of statistically different sclerite classes present in the eastern Pacific octocoral genus Pacifigorgia. We also test the ability of simple neural classifiers (perceptrons) to sort sclerites into the classes traditionally used in octocoral taxonomy. This methodology can be used for other gorgoniids and can be further extended to include shape quantifiers for groups other than those studied here. (c) 2009 Elsevier Ltd. All rights reserved. C1 [Vargas, Sergio] Univ Costa Rica, Escuela Biol, Museum Zool, San Jose, Costa Rica. [Breedy, Odalisca; Guzman, Hector M.] 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 Estructuras Microscop, San Jose, Costa Rica. [Siles, Francisco] Univ Costa Rica, Fac Ingn, Escuela Ingn Elect, San Jose, Costa Rica. RP Vargas, S (reprint author), Dept Geo & Environm Sci Palaeontol & Geobiol, Mol Geo & Palaeobiol Lab, Richard Wagner Str 10, D-80333 Munich, Germany. EM s.vargas@lrz.uni-muenchen.de RI Vargas, Sergio/A-5678-2011 OI Vargas, Sergio/0000-0001-8704-1339 NR 28 TC 4 Z9 4 U1 0 U2 5 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0968-4328 J9 MICRON JI Micron PD FEB PY 2010 VL 41 IS 2 BP 158 EP 164 DI 10.1016/j.micron.2009.08.009 PG 7 WC Microscopy SC Microscopy GA 539FJ UT WOS:000273238700010 PM 19889548 ER PT J AU Calderon, I Ventura, CRR Turon, X Lessios, HA AF Calderon, I. Ventura, C. R. R. Turon, X. Lessios, H. A. TI Genetic divergence and assortative mating between colour morphs of the sea urchin Paracentrotus gaimardi SO MOLECULAR ECOLOGY LA English DT Article DE assortative mating; bindin; colour polymorphism; histone; mitochondrial ATPase; Paracentrotus ID AMINO-ACID SITES; AMPHIPHOLIS-SQUAMATA ECHINODERMATA; GAMETE RECOGNITION; POSITIVE SELECTION; GENUS ECHINOMETRA; PHENOTYPIC PLASTICITY; EVOLUTION; SPECIATION; POPULATION; PHYLOGEOGRAPHY AB Some species of sea urchins feature large variation in pigmentation. This variability may be the result of phenotypic plasticity or it may be associated with genetic divergence between morphs. Paracentrotus gaimardi exhibits five colour morphs (pink, brown, green, grey and black), which often occur side by side on the same rock. We studied genetic divergence between these morphs in three populations on the coast of Brazil. A fragment of the region encoding the mitochondrial ATPase 8 and 6 mitochondrial genes, a fragment of the intron of a nuclear histone and the entire nuclear gene coding for the sperm protein bindin were analysed. Mitochondrial DNA was differentiated between the pink and all other morphs, but the histone intron was similar in all colour morphs. In bindin, nine codons were found to be under positive selection and significant differences of allelic frequencies were observed in almost all pairwise comparisons between colour morphs. Although the molecular differentiation in bindin is not large enough to suggest reproductive isolation, some degree of assortative mating within morphs seems to be occurring in this species. C1 [Lessios, H. A.] Smithsonian Trop Res Inst, Balboa, Panama. [Calderon, I.] Univ Barcelona, Fac Biol, Dept Anim Biol, E-08028 Barcelona, Spain. [Ventura, C. R. R.] Museu Nacl UFRJ, Dept Invertebrados, Lab Echinodermata, Rio De Janeiro, Brazil. [Turon, X.] CSIC, CEAB, Ctr Adv Studies Blanes, Blanes 17300, Girona, Spain. RP Lessios, HA (reprint author), Smithsonian Trop Res Inst, Balboa, Panama. EM lessiosh@si.edu RI Turon, Xavier/J-9211-2012; Ventura, Carlos Renato/C-5723-2015 OI Turon, Xavier/0000-0002-9229-5541; Ventura, Carlos Renato/0000-0002-1005-1333 FU Spanish Government [CTM2007-66635]; STRI; Brazilian Council of Research (CNPq) FX We thank Ligia and Axel Calderon for their invaluable help with lab work. We are grateful to Laura Geyer for her help in obtaining permissions for sample importation. We are also grateful to Elinia M Lopes, Fernanda S. Viana and Mariana Contins for their help in the field and laboratory work in Brazil. This study was funded by project CTM2007-66635 of the Spanish Government, by General Research Funds from STRI and by the Brazilian Council of Research (CNPq). NR 76 TC 15 Z9 15 U1 0 U2 18 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 FEB PY 2010 VL 19 IS 3 BP 484 EP 493 DI 10.1111/j.1365-294X.2009.04506.x PG 10 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 545KS UT WOS:000273731600007 PM 20070515 ER PT J AU Javonillo, R Malabarba, LR Weitzman, SH Burns, JR AF Javonillo, Robert Malabarba, Luiz R. Weitzman, Stanley H. Burns, John R. TI Relationships among major lineages of characid fishes (Teleostei: Ostariophysi: Characiformes), based on molecular sequence data SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Otophysi; Phylogeny; Bayesian inference; Characidae; Tetragonopterinae; Glandulocaudinae; Acestrorhynchus; Gasteropelecidae; Pseudotympanum; Neotropical fauna ID MITOCHONDRIAL-DNA; AMPLIFICATION; SUBSTITUTION; BIOGEOGRAPHY; PHYLOGENY; MODELTEST; INFERENCE; PRIMERS; MRBAYES; TREES AB The family Characidae is a group of freshwater bony fishes that exhibits high species-level diversity and whose members inhabit parts of Texas, Mexico, and Central and South America. Thus far, morphological data have been of limited use in discerning relationships among subfamilies and incertae sedis genera of the family Characidae. In this study, DNA sequence data from GenBank were combined with new sequences for analyses under Bayesian and parsimony schemes. Sequences fell into four gene partitions, with three genes in the mitochondrial subset (125, 165, COI genes) and one gene in the nuclear subset (RAG2 gene). Inferred Bayesian and parsimony-based phylogenies reject the monophyly of certain groups (e.g., Astyanax, Hyphessobrycon, and Bryconamericus), do not reject the monophyly of others (e.g., Cheirodontinae and "clade A" of previous authors), and present new sister-group hypotheses (e.g., Brittanichthys sister to Paracheirodon). Sister to clade A is a lineage referred to herein as "clade B" which includes Exodon and exemplars from Cheirodontinae (the most basal lineage within clade B), Aphyocharacinae, Tetragonopterinae, and Characinae (excluding Gnathocharax). "Clade C" is sister to A + B and contains representatives of large incertae sedis genera (e.g., Hyphessobrycon, Hemigrammus), as well as members of Stethaprioninae. Unless certain other subfamilial names are to be disregarded, the use of Tetragonopterinae should continue to be restricted to species of Tetragonopterus because other genera previously referred to this subfamily grouped in clades A or C, quite distant from Tetragonopterus. (C) 2009 Elsevier Inc. All rights reserved C1 [Javonillo, Robert; Burns, John R.] George Washington Univ, Dept Biol Sci, Washington, DC 20052 USA. [Malabarba, Luiz R.] Univ Fed Rio Grande do Sul, Dept Zool, BR-91501970 Porto Alegre, RS, Brazil. [Weitzman, Stanley H.] Smithsonian Inst, Natl Museum Nat Hist, Divis Fishes, Dept Vertebrate Zool, Washington, DC 20560 USA. RP Javonillo, R (reprint author), George Washington Univ, Dept Biol Sci, Lisner Hall 340,2023 G St NW, Washington, DC 20052 USA. EM rjavonil@gwmail.gwu.edu RI Malabarba, Luiz/I-3225-2012 FU CNPq [478002/2006-8, 479412/2008-1] FX The authors would like to thank the following individuals for help in handling tissues, use of equipment or consumables, and advice in data collection: Jeff Clayton (Smithsonian Institution, National Museum of Natural History), Carlos Lucena (PUCKS, Museu de Ciencias a Tecnologia), Sandro Bonatto (PUCKS), Andrea Thomaz (UFRGS). For funding, we thank the following organizations: Sigma Xi (Grants-in-Aid of Research Program), The Willi Hennig Society (for making TNT freely available), DeepFin Research Coordination Network, GWU, and CNPq (Brazil). In particular, CNPq processes 478002/2006-8 and 479412/2008-1 to LRM were of major assistance to this project, whereby the former contributed to work at PUCKS and the latter funded a new facility at UFRGS for DNA extraction and amplification. Sheri Church (GWU) kindly provided access to Sequencher software. The manuscript was substantially improved with the help of the reviewer's comments. Special thanks are due to Peter and Martin Hoffmann (Salzgitter and Hannover, Germany, respectively), who supplied a specimen of Brittanichthys axelrodi. NR 49 TC 84 Z9 87 U1 5 U2 33 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 FEB PY 2010 VL 54 IS 2 BP 498 EP 511 DI 10.1016/j.ympev.2009.08.026 PG 14 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 545SX UT WOS:000273758200017 PM 19720150 ER PT J AU Wardlow, JL Smail, I Wilson, GW Yun, MS Coppin, KEK Cybulski, R Geach, JE Ivison, RJ Aretxaga, I Austermann, JE Edge, AC Fazio, GG Huang, J Hughes, DH Kodama, T Kang, Y Kim, S Mauskopf, PD Perera, TA Scott, KS AF Wardlow, J. L. Smail, Ian Wilson, G. W. Yun, M. S. Coppin, K. E. K. Cybulski, R. Geach, J. E. Ivison, R. J. Aretxaga, I. Austermann, J. E. Edge, A. C. Fazio, G. G. Huang, J. Hughes, D. H. Kodama, T. Kang, Y. Kim, S. Mauskopf, P. D. Perera, T. A. Scott, K. S. TI An AzTEC 1.1-mm survey for ULIRGs in the field of the Galaxy Cluster MS 0451.6-0305 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: clusters: individual: MS 0451-03; submillimetre ID STAR-FORMING GALAXIES; SCUBA SUPER-MAP; ULTRALUMINOUS INFRARED GALAXIES; REDSHIFT SUBMILLIMETER GALAXIES; SPECTRAL ENERGY-DISTRIBUTIONS; DEGREE EXTRAGALACTIC SURVEY; DUSTY STARBURST GALAXIES; GOODS-N FIELD; PHOTOMETRIC REDSHIFTS; MAGNITUDE RELATION AB We have undertaken a deep (sigma similar to 1.1 mJy) 1.1-mm survey of the z = 0.54 cluster MS 0451.6-0305 using the AzTEC camera on the James Clerk Maxwell Telescope. We detect 36 sources with signal-to-noise ratio (S/N) >= 3.5 in the central 0.10 deg(2) and present the AzTEC map, catalogue and number counts. We identify counterparts to 18 sources (50 per cent) using radio, mid-infrared, Spitzer InfraRed Array Camera (IRAC) and Submillimetre Array data. Optical, near- and mid-infrared spectral energy distributions are compiled for the 14 of these galaxies with detectable counterparts, which are expected to contain all likely cluster members. We then use photometric redshifts and colour selection to separate background galaxies from potential cluster members and test the reliability of this technique using archival observations of submillimetre galaxies. We find two potential MS 0451-03 members, which, if they are both cluster galaxies, have a total star formation rate (SFR) of similar to 100 M-circle dot yr(-1) - a significant fraction of the combined SFR of all the other galaxies in MS 0451-03. We also examine the stacked rest-frame mid-infrared, millimetre and radio emission of cluster members below our AzTEC detection limit, and find that the SFRs of mid-IR-selected galaxies in the cluster and redshift-matched field populations are comparable. In contrast, the average SFR of the morphologically classified late-type cluster population is nearly three times less than the corresponding redshift-matched field galaxies. This suggests that these galaxies may be in the process of being transformed on the red sequence by the cluster environment. Our survey demonstrates that although the environment of MS 0451-03 appears to suppress star formation in late-type galaxies, it can support active, dust-obscured mid-IR galaxies and potentially millimetre-detected LIRGs. C1 [Wardlow, J. L.; Geach, J. E.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Ivison, R. J.] Univ Edinburgh, Scottish Univ Phys Alliance, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Ivison, R. J.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Aretxaga, I.; Hughes, D. H.] Inst Nacl Astrofis Opt & Electr, Puebla, Mexico. [Austermann, J. E.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Fazio, G. G.; Huang, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kodama, T.] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Kang, Y.; Kim, S.] Sejong Univ, Dept Astron & Space Sci, Seoul, South Korea. [Mauskopf, P. D.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Perera, T. A.] Illinois Wesleyan Univ, Bloomington, IL 61702 USA. [Scott, K. S.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Smail, Ian; Coppin, K. E. K.; Edge, A. C.] Univ Durham, Inst Computat Cosmol, Durham DH1 3LE, England. [Wilson, G. W.; Yun, M. S.; Cybulski, R.; Scott, K. S.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. RP Wardlow, JL (reprint author), Univ Durham, Dept Phys, South Rd, Durham DH1 3LE, England. EM j.l.wardlow@durham.ac.uk RI Smail, Ian/M-5161-2013; Wardlow, Julie/C-9903-2015; Ivison, R./G-4450-2011; OI Smail, Ian/0000-0003-3037-257X; Wardlow, Julie/0000-0003-2376-8971; Ivison, R./0000-0001-5118-1313; Cybulski, Ryan/0000-0002-4997-2308; Edge, Alastair/0000-0002-3398-6916; /0000-0002-0729-2988 FU Science and Technology Facilities Council (STFC); STFC; NASA GSFC Cooperative Agreement [NNG04G155A]; NSF [AST 05-40852]; Korea Science & Engineering Foundation (KOSEF); Astrophysical Research Center of the Structure and Evolution of the Cosmos (ARCSEC); NASA FX We thank an anonymous referee for helpful comments which greatly improved the clarity of this paper. We would also like to thank C. J. Ma and Harald Ebeling for providing us with reduced CFHT U-band images, Richard Ellis for supplying reduced HST WFPC2 images and Sean Moran for the usage of spectroscopic catalogues and attributed information. JLW, IRS and JEG acknowledge support from the Science and Technology Facilities Council (STFC), and KEKC acknowledges support from an STFC Fellowship. KSS was supported in part through the NASA GSFC Cooperative Agreement NNG04G155A. Support for this work was provided in part by the NSF grant AST 05-40852 and the grant from the Korea Science & Engineering Foundation (KOSEF) under a cooperative agreement with the Astrophysical Research Center of the Structure and Evolution of the Cosmos (ARCSEC). Additional support for this work was provided by NASA through an award issued by JPL/Caltech. The JCMT 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. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. This work also made use of the Spitzer Archive, which is operated by the Spitzer Science Center. Based in part on data collected at Subaru Telescope, which is operated by the National Astronomical Observatory of Japan. Based on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA, at 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. The William Herschel Telescope and its service programme 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 79 TC 16 Z9 16 U1 0 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB 1 PY 2010 VL 401 IS 4 BP 2299 EP 2317 DI 10.1111/j.1365-2966.2009.15847.x PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 544VQ UT WOS:000273687800012 ER PT J AU Lampeitl, H Nichol, RC Seo, HJ Giannantonio, T Shapiro, C Bassett, B Percival, WJ Davis, TM Dilday, B Frieman, J Garnavich, P Sako, M Smith, M Sollerman, J Becker, AC Cinabro, D Filippenko, AV Foley, RJ Hogan, CJ Holtzman, JA Jha, SW Konishi, K Marriner, J Richmond, MW Riess, AG Schneider, DP Stritzinger, M van der Heyden, KJ VanderPlas, JT Wheeler, JC Zheng, C AF Lampeitl, H. Nichol, R. C. Seo, H. -J. Giannantonio, T. Shapiro, C. Bassett, B. Percival, W. J. Davis, T. M. Dilday, B. Frieman, J. Garnavich, P. Sako, M. Smith, M. Sollerman, J. Becker, A. C. Cinabro, D. Filippenko, A. V. Foley, R. J. Hogan, C. J. Holtzman, J. A. Jha, S. W. Konishi, K. Marriner, J. Richmond, M. W. Riess, A. G. Schneider, D. P. Stritzinger, M. van der Heyden, K. J. VanderPlas, J. T. Wheeler, J. C. Zheng, C. TI First-year Sloan Digital Sky Survey-II supernova results: consistency and constraints with other intermediate-redshift data sets SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Review DE supernovae: general; cosmology: observations; distance scale; cosmological parameters; large-scale structure of Universe ID LUMINOUS RED GALAXIES; ANISOTROPY-PROBE OBSERVATIONS; HUBBLE-SPACE-TELESCOPE; INTEGRATED SACHS-WOLFE; IA LIGHT CURVES; SPECTROSCOPIC TARGET SELECTION; LARGE-SCALE STRUCTURE; SURVEY IMAGING DATA; DARK ENERGY; POWER-SPECTRUM AB We present an analysis of the luminosity distances of Type Ia Supernovae (SNe) from the Sloan Digital Sky Survey-II (SDSS-II) SN Survey in conjunction with other intermediate-redshift (z < 0.4) cosmological measurements including redshift-space distortions from the Two-Degree Field Galaxy Redshift Survey (2dFGRS), the integrated Sachs-Wolfe (ISW) effect seen by the SDSS and the latest baryon acoustic oscillation (BAO) distance scale from both the SDSS and 2dFGRS. We have analysed the SDSS-II SN data alone using a variety of 'model-independent' methods and find evidence for an accelerating Universe at a > 97 per cent level from this single data set. We find good agreement between the SN and BAO distance measurements, both consistent with a Lambda-dominated cold dark matter cosmology, as demonstrated through an analysis of the distance duality relationship between the luminosity (d(L)) and angular diameter (d(A)) distance measures. We then use these data to estimate omega within this restricted redshift range (z < 0.4). Our most stringent result comes from the combination of all our intermediate-redshift data (SDSS-II SNe, BAO, ISW and redshift-space distortions), giving omega = -0.81(-0.18)(+0.16) (stat) +/- 0.15 (sys) and Omega(M) = 0.22(-0.08)(+0.09) assuming a flat universe. This value of w and associated errors only change slightly if curvature is allowed to vary, consistent with constraints from the cosmic microwave background. We also consider more limited combinations of the geometrical (SN, BAO) and dynamical (ISW, redshift-space distortions) probes. C1 [Lampeitl, H.; Nichol, R. C.; Giannantonio, T.; Shapiro, C.; Percival, W. J.; Smith, M.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. [Seo, H. -J.; Frieman, J.; Hogan, C. J.; Marriner, J.] Fermilab Natl Accelerator Lab, Ctr Particle Astrophys, Batavia, IL 60510 USA. [Giannantonio, T.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany. [Bassett, B.; Smith, M.] Univ Cape Town, Dept Math & Appl Math, ZA-7701 Rondebosch, South Africa. [Bassett, B.] S African Astron Observ, ZA-7935 Cape Town, South Africa. [Davis, T. M.] Univ Queensland, Sch Math & Phys, Brisbane, Qld 4072, Australia. [Davis, T. M.; Sollerman, J.; Stritzinger, M.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. [Dilday, B.; Jha, S. W.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Frieman, J.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Garnavich, P.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Sako, M.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19096 USA. [Sollerman, J.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden. [Becker, A. C.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Cinabro, D.] Wayne State Univ, Dept Phys & Astron, Detroit, MI 48202 USA. [Filippenko, A. V.; Foley, R. J.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Foley, R. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Holtzman, J. A.] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA. [Konishi, K.] Univ Tokyo, Inst Cosm Ray Res, Kashiwa, Chiba 2778582, Japan. [Konishi, K.] Univ Tokyo, Grad Sch Sci, Dept Phys, Bunkyo Ku, Tokyo 1130033, Japan. [Richmond, M. W.] Rochester Inst Technol, Dept Phys, Rochester, NY 14623 USA. [Riess, A. G.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Riess, A. G.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Schneider, D. P.] Penn State Univ, Davey Lab 525, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Stritzinger, M.] Carnegie Observ, Las Campanas Observ, La Serena, Chile. [van der Heyden, K. J.] Univ Cape Town, Dept Astron, ZA-7701 Rondebosch, South Africa. [Wheeler, J. C.] Univ Texas Austin, McDonald Observ, Dept Astron, Austin, TX 78712 USA. [Zheng, C.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. RP Lampeitl, H (reprint author), Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. EM Hubert.Lampeitl@port.ac.uk RI Davis, Tamara/A-4280-2008; OI Davis, Tamara/0000-0002-4213-8783; Sollerman, Jesper/0000-0003-1546-6615 FU Science and Technology Facilities Council (STFC) [ST/F002335/1, ST/H002774/1]; D.O.E at Fermilab; US NSF [AST-0607485]; 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, Cambridge University; 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 (MPA); Max-Planck-Institute for Astrophysics (MPiA); New Mexico State University; Ohio State University; University of Pittsburgh; University of Portsmouth; Princeton University; United States Naval Observatory; University of Washington; California Institute of Technology; University of California; W. M. Keck Foundation FX We thank an anonymous referee for helpful comments on this paper which greatly improved the content of the paper. RCN on behalf of the authors would like to thank Mike Turner for helpful discussions on the q0 fit and Eric Aubourg for useful discussions on the distance duality relation. We also thank Rick Kessler and Mark Sullivan for extensive discussions about their work and papers. TG thanks Jussi Valiviita for helpful suggestions. HL, CS and RCN are grateful to the Science and Technology Facilities Council (STFC) for funding this research with rolling grants ST/F002335/1 and ST/H002774/1. H-JS is supported by the D.O.E at Fermilab. AVF is grateful for the support of US NSF grant AST-0607485.; Funding for the creation and distribution of 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, Cambridge University, 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 (MPA), the Max-Planck-Institute for Astrophysics (MPiA), 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.; This work is based in part on observations made at the following telescopes. The Hobby-Eberly Telescope (HET) is a joint project of the University of Texas at Austin, the Pennsylvania State University, Stanford University, Ludwig-Maximillians-Universitat Munchen and Georg-August-Universitat Gottingen. The HET is named in honour of its principal benefactors, William P. Hobby and Robert E. Eberly. The Marcario Low-Resolution Spectrograph is named for Mike Marcario of High Lonesome Optics, who fabricated several optical elements for the instrument but died before its completion; it is a joint project of the HET partnership and the Instituto de Astronomia de la Universidad Nacional Autonoma de Mexico. The Apache Point Observatory 3.5 m telescope is owned and operated by the Astrophysical Research Consortium. We thank the observatory director, Suzanne Hawley, and site manager, Bruce Gillespie, for their support of this project. The Subaru Telescope is operated by the National Astronomical Observatory of Japan. The William Herschel Telescope is operated by the Isaac Newton Group on the island of La Palma in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. The W. M. Keck Observatory is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration; the observatory was made possible by the generous financial support of the W. M. Keck Foundation. NR 106 TC 61 Z9 61 U1 1 U2 6 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 FEB 1 PY 2010 VL 401 IS 4 BP 2331 EP 2342 DI 10.1111/j.1365-2966.2009.15851.x PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 544VQ UT WOS:000273687800014 ER PT J AU Dijkstra, M Westra, E AF Dijkstra, Mark Westra, Eduard TI Star formation indicators and line equivalent width in Ly alpha galaxies SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: high redshift ID HIGH-REDSHIFT GALAXIES; LYMAN BREAK GALAXIES; SUBARU DEEP FIELD; SIMILAR-TO 3; STARBURST GALAXIES; FORMING GALAXIES; SPECTROSCOPIC PROPERTIES; RADIATIVE-TRANSFER; POPULATION III; RADIO GALAXY AB The equivalent width (EW) of the Ly alpha line is directly related to the ratio of star formation rates (SFR) determined from Ly alpha flux and UV flux density [SFR(Ly alpha)/SFR(UV)]. We use published data - in the literature EW and SFR(Ly alpha)/SFR(UV) are treated as independent quantities - to show that the predicted relation holds for the vast majority of observed Ly alpha-emitting galaxies (LAEs). We show that the relation between EW and SFR(Ly alpha)/SFR(UV) applies irrespective of a galaxy's 'true' underlying SFR, and that its only source of scatter is the variation in the spectral slope of the UV continuum between individual galaxies. The derived relation, when combined with the observed EW distribution, implies that the ratio SFR(UV)/SFR(Ly alpha) is described well by a lognormal distribution with a standard deviation of similar to 0.3-0.35. This result is useful when modelling the statistical properties of LAEs. We further discuss why the relation between EW and SFR(Ly alpha)/SFR(UV) may help in identifying galaxies with unusual stellar populations. C1 [Dijkstra, Mark] Harvard Univ, Dept Astron, Cambridge, MA 02138 USA. [Westra, Eduard] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Dijkstra, M (reprint author), Harvard Univ, Dept Astron, 60 Garden St, Cambridge, MA 02138 USA. EM mdijkstr@cfa.harvard.edu FU Harvard University funds; Smithsonian Institution FX MD is supported by Harvard University funds. EW acknowledges the Smithsonian Institution for the support of his post-doctoral fellowship. We thank an anonymous referee for helpful, constructive comments that significantly improved the content of this paper. NR 42 TC 13 Z9 13 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 FEB 1 PY 2010 VL 401 IS 4 BP 2343 EP 2348 DI 10.1111/j.1365-2966.2009.15859.x PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 544VQ UT WOS:000273687800015 ER PT J AU Aird, J Nandra, K Laird, ES Georgakakis, A Ashby, MLN Barmby, P Coil, AL Huang, JS Koekemoer, AM Steidel, CC Willmer, CNA AF Aird, J. Nandra, K. Laird, E. S. Georgakakis, A. Ashby, M. L. N. Barmby, P. Coil, A. L. Huang, J. -S. Koekemoer, A. M. Steidel, C. C. Willmer, C. N. A. TI The evolution of the hard X-ray luminosity function of AGN SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; galaxies: evolution; galaxies: luminosity function, mass function; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; DEEP FIELD-SOUTH; SUPERMASSIVE BLACK-HOLES; STAR-FORMING GALAXIES; EXTENDED GROTH STRIP; MEDIUM SENSITIVITY SURVEY; LYMAN-BREAK GALAXIES; LARGE SKY SURVEY; HIGH-REDSHIFT; PHOTOMETRIC REDSHIFTS AB We present new observational determinations of the evolution of the 2-10 keV X-ray luminosity function (XLF) of active galactic nuclei (AGN). We utilize data from a number of surveys including both the 2 Ms Chandra Deep Fields and the AEGIS-X 200 ks survey, enabling accurate measurements of the evolution of the faint end of the XLF. We combine direct, hard X-ray selection and spectroscopic follow-up or photometric redshift estimates at z < 1.2 with a rest-frame UV colour pre-selection approach at higher redshifts to avoid biases associated with catastrophic failure of the photometric redshifts. Only robust optical counterparts to X-ray sources are considered using a likelihood ratio matching technique. A Bayesian methodology is developed that considers redshift probability distributions, incorporates selection functions for our high-redshift samples and allows robust comparison of different evolutionary models. We statistically account for X-ray sources without optical counterparts to correct for incompleteness in our samples. We also account for Poissonian effects on the X-ray flux estimates and sensitivities and thus correct for the Eddington bias. We find that the XLF retains the same shape at all redshifts, but undergoes strong luminosity evolution out to z similar to 1, and an overall negative density evolution with increasing redshift, which thus dominates the evolution at earlier times. We do not find evidence that a luminosity-dependent density evolution, and the associated flattening of the faint-end slope, is required to describe the evolution of the XLF. We find significantly higher space densities of low-luminosity, high-redshift AGN than in prior studies, and a smaller shift in the peak of the number density to lower redshifts with decreasing luminosity. The total luminosity density of AGN peaks at z = 1.2 +/- 0.1, but there is a mild decline to higher redshifts. We find that > 50 per cent of black hole growth takes place at z > 1, with around half in L-X < 10(44) erg s(-1) AGN. C1 [Aird, J.; Nandra, K.; Laird, E. S.] Univ London Imperial Coll Sci Technol & Med, Astrophys Grp, Blackett Lab, London SW7 2AZ, England. [Georgakakis, A.] Inst Astron, Natl Observ Athens, Athens 15236, Greece. [Ashby, M. L. N.; Huang, J. -S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Barmby, P.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [Aird, J.; Coil, A. L.] Univ Calif San Diego, Dept Phys, CASS, La Jolla, CA 92093 USA. [Koekemoer, A. M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Steidel, C. C.] CALTECH, Pasadena, CA 91125 USA. [Willmer, C. N. A.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Aird, J (reprint author), Univ Calif San Diego, Dept Phys, CASS, La Jolla, CA 92093 USA. EM jaird@ucsd.edu RI Georgakakis, Antonis/K-4457-2013; Barmby, Pauline/I-7194-2016; OI Barmby, Pauline/0000-0003-2767-0090; Koekemoer, Anton/0000-0002-6610-2048; Georgakakis, Antonis/0000-0002-3514-2442 FU STFC; CFHT; CEA/DAPNIA; National Research Council (NRC) of Canada; Institut National des Sciences de l'Univers of the Centre National de la Recherche Scientifique (CNRS) of France; University of Hawaii; Canadian Astronomy Data Centre FX We acknowledge financial support from STFC (JA, ESL). Some observations reported here were obtained at the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona. Also based in part on observations obtained with MegaPrime/MegaCam, a joint project of 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 CFHTLS, a collaborative project of NRC and CNRS. NR 95 TC 183 Z9 183 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 FEB 1 PY 2010 VL 401 IS 4 BP 2531 EP 2551 DI 10.1111/j.1365-2966.2009.15829.x PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 544VQ UT WOS:000273687800031 ER PT J AU Pal, A Bakos, GA Torres, G Noyes, RW Fischer, DA Johnson, JA Henry, GW Butler, RP Marcy, GW Howard, AW Sipocz, B Latham, DW Esquerdo, GA AF Pal, Andras Bakos, Gaspar A. Torres, Guillermo Noyes, Robert W. Fischer, Debra A. Johnson, John A. Henry, Gregory W. Butler, R. Paul Marcy, Geoffrey W. Howard, Andrew W. Sipocz, Brigitta Latham, David W. Esquerdo, Gilbert A. TI Refined stellar, orbital and planetary parameters of the eccentric HAT-P-2 planetary system SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE techniques: spectroscopic; stars: fundamental parameters; stars: individual: HD 147506, HAT-P-2; planetary systems ID LIMB-DARKENING LAW; EXTRASOLAR PLANET; MASSIVE PLANET; LIGHT CURVES; BRIGHT STAR; SPIN-ORBIT; EXOPLANET HAT-P-1B; TRANSITING PLANET; SURFACE GRAVITIES; ATMOSPHERE MODELS AB We present refined parameters for the extrasolar planetary system HAT-P-2 (also known as HD 147506), based on new radial velocity and photometric data. HAT-P-2b is a transiting extrasolar planet that exhibits an eccentric orbit. We present a detailed analysis of the planetary and stellar parameters, yielding consistent results for the mass and radius of the star, better constraints on the orbital eccentricity and refined planetary parameters. The improved parameters for the host star are M(star) = 1.36 +/- 0.04 M(circle dot) and R(star) = 1.64 +/- 0.08 R(circle dot), while the planet has a mass of M(p) = 9.09 +/- 0.24 M(Jup) and radius of R(p) = 1.16 +/- 0.08 R(Jup). The refined transit epoch and period for the planet are E = 245 4387.49375 +/- 0.00074 (BJD) and P = 5.6334729 +/- 0.0000061 (d), and the orbital eccentricity and argument of periastron are e = 0.5171 +/- 0.0033 and omega = 185.degrees 22 +/- 0.degrees 95. These orbital elements allow us to predict the timings of secondary eclipses with a reasonable accuracy of similar to 15 min. We also discuss the effects of this significant eccentricity including the characterization of the asymmetry in the transit light curve. Simple formulae are presented for the above, and these, in turn, can be used to constrain the orbital eccentricity using purely photometric data. These will be particularly useful for very high precision, space-borne observations of transiting planets. C1 [Pal, Andras; Bakos, Gaspar A.; Torres, Guillermo; Noyes, Robert W.; Sipocz, Brigitta; Latham, David W.; Esquerdo, Gilbert A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Pal, Andras] Hungarian Acad Sci, Konkoly Observ, H-1121 Budapest, Hungary. [Pal, Andras; Sipocz, Brigitta] Eotvos Lorand Univ, Dept Astron, H-1117 Budapest, Hungary. [Fischer, Debra A.] San Francisco State Univ, Dept Phys & Astron, San Francisco, CA 94132 USA. [Johnson, John A.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Henry, Gregory W.] Tennessee State Univ, Ctr Excellence Informat Syst, Nashville, TN 37209 USA. [Butler, R. Paul] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA. [Marcy, Geoffrey W.; Howard, Andrew W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Pal, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM apal@szofi.net RI Butler, Robert/B-1125-2009; Howard, Andrew/D-4148-2015; OI Howard, Andrew/0000-0001-8638-0320; Fischer, Debra/0000-0003-2221-0861 FU HATNet; ESA [PECS 98073]; NASA [NNG04GN74G, NNX08AF23G, NNX09AF59G, NCC2-1390]; SAO IRD; NSF Astronomy and Astrophysics [AST-0702843, AST-0702821]; NOAO; State of Tennessee through its Centers of Excellence FX The work by AP was supported by the HATNet project and in part by ESA grant PECS 98073. HATNet operations have been funded by NASA grants NNG04GN74G, NNX08AF23G and SAO IR&D grants. Work of GAB and JAJ were supported by the Post-doctoral Fellowship of the NSF Astronomy and Astrophysics Program (AST-0702843 and AST-0702821, respectively). GT received partial support from NASA Origins grant NNX09AF59G. We acknowledge partial support also from the Kepler Mission under NASA Cooperative Agreement NCC2-1390 (DWL, PI). This research has made use of Keck telescope time granted through NOAO and NASA. We thank the UCO/Lick technical staff for supporting the remote-observing capability of the Nickel Telescope, allowing the photometry to be carried out from UC Berkeley. Automated Astronomy at Tennessee State University has been supported long term by NASA and NSF as well as Tennessee State University and the State of Tennessee through its Centers of Excellence program. We are grateful for the comments and suggestions by the referee, Frederic Pont. We acknowledge the use of the VizieR service (Ochsenbein, Bauer & Marcout 2000) operated at CDS, Strasbourg, France, of NASA's Astrophysics Data System Abstract Service, and of the 2MASS Catalogue. NR 53 TC 46 Z9 46 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 FEB 1 PY 2010 VL 401 IS 4 BP 2665 EP 2674 DI 10.1111/j.1365-2966.2009.15849.x PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 544VQ UT WOS:000273687800041 ER PT J AU Popov, SB Pons, JA Miralles, JA Boldin, PA Posselt, B AF Popov, S. B. Pons, J. A. Miralles, J. A. Boldin, P. A. Posselt, B. TI Population synthesis studies of isolated neutron stars with magnetic field decay SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: neutron; pulsars: general ID ROSAT ALL-SKY; X-RAY PULSARS; ISOLATED RADIO PULSARS; TEMPERATURE DISTRIBUTION; 3EG J1835+5918; MASSIVE STARS; GOULD BELT; EMISSION; EVOLUTION; ROTATION AB We perform population synthesis studies of different types of neutron stars (NSs) (thermally emitting isolated NSs, normal radio pulsars, magnetars) taking into account the magnetic field decay and using results from the most recent advances in NS cooling theory. For the first time, we confront our results with observations using simultaneously the log N-log S distribution for nearby isolated NSs, the log N-log L distribution for magnetars, and the distribution of radio pulsars in the P-(P) over dot diagram. For this purpose, we fix a baseline NS model (all microphysics input), and other relevant parameters to standard values (velocity distribution, mass spectrum, birth rates, etc.), allowing us to vary the initial magnetic field strength. We find that our theoretical model is consistent with all sets of data if the initial magnetic field distribution function follows a lognormal law with < log (B-0/G)> similar to 13.25 and sigma(logB0) similar to 0.6 . The typical scenario includes about 10 per cent of NSs born as magnetars, significant magnetic field decay during the first million years of a NS life (only about a factor of 2 for low-field NSs but more than an order of magnitude for magnetars), and a mass distribution function dominated by low-mass objects. This model explains satisfactorily all known populations. Evolutionary links between different subclasses may exist, although robust conclusions are not yet possible. C1 [Popov, S. B.] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Moscow 119991, Russia. [Pons, J. A.; Miralles, J. A.] Univ Alacant, Dept Fis Aplicada, Alacant 03080, Spain. [Boldin, P. A.] Moscow MV Lomonosov State Univ, Moscow Engn Phys Inst, Moscow 115409, Russia. [Posselt, B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Popov, SB (reprint author), Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Univ Ski Pr 13, Moscow 119991, Russia. EM polar@sai.msu.ru; jose.pons@ua.es RI Popov, Sergei/B-6368-2008; PONS, JOSE/D-4687-2012; OI Popov, Sergei/0000-0002-4292-8638; PONS, JOSE/0000-0003-1018-8126; Posselt, Bettina/0000-0003-2317-9747 FU MEC [AYA 2007-67626-C03-02]; ESF; Russian Foundation for Basic research [07-02-00961, 09-02-00032]; Deutsche Akademie der Naturforscher Leopoldina (Halle, Germany) [BMBF-LPD 9901/8-170] FX We thank D. N. Aguilera and R. Turolla for interesting discussions. We thank the referee for critical remarks. This research has been supported by the Spanish MEC grant AYA 2007-67626-C03-02, the Research Network Program Compstar funded by the ESF and the Russian Foundation for Basic research (grants 07-02-00961 and 09-02-00032). SBP thanks the Universities of Alicante and Padova for hospitality. BP acknowledges support by the Deutsche Akademie der Naturforscher Leopoldina (Halle, Germany) under grant BMBF-LPD 9901/8-170. NR 74 TC 54 Z9 55 U1 0 U2 4 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 FEB 1 PY 2010 VL 401 IS 4 BP 2675 EP 2686 DI 10.1111/j.1365-2966.2009.15850.x PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 544VQ UT WOS:000273687800042 ER PT J AU Hardcastle, MJ Massaro, F Harris, DE AF Hardcastle, M. J. Massaro, F. Harris, D. E. TI X-ray emission from the extended emission-line region of the powerful radio galaxy 3C 171 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: individual: 3C 171; galaxies: ISM; galaxies: jets; X-rays: galaxies ID JET-CLOUD INTERACTIONS; STATISTICAL PROPERTIES; HOT-GAS; LOBES; NUCLEI; SHOCKS; OUTFLOWS; PROJECT; CHANDRA; 3C-171 AB We present Chandra X-ray observations of the powerful radio galaxy 3C 171, which reveal an extended region of X-ray emission spatially associated with the well-known 10-kpc scale optical emission-line region around the radio jets. We argue that the X-ray emission comes from collisionally ionized material, originally cold gas that has been shock heated by the passage of the radio jet, rather than being photoionized by nuclear radiation. This hot plasma is also responsible for the depolarization at low frequencies of the radio emission from the jet and hotspots, which allows us to estimate the magnetic field strength in the external medium. We show that it is likely that both the cold emission-line gas and the hot plasma in which it is embedded are being driven out of the host galaxy of 3C 171 at supersonic speeds. A significant fraction of the total energy budget of the central active galactic nuclei must have been expended in driving this massive outflow. We argue that 3C 171, with its unusual radio morphology and the strong relation between the jet and large amounts of outflowing material, is a member of a class of radio galaxies in which there is strong interaction between the radio jets and cold material in the host galaxy; such objects may have been very much more common in the early Universe. C1 [Hardcastle, M. J.] Univ Hertfordshire, Sch Phys Astron & Math, Hatfield AL10 9AB, Herts, England. [Massaro, F.; Harris, D. E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Hardcastle, MJ (reprint author), Univ Hertfordshire, Sch Phys Astron & Math, Coll Lane, Hatfield AL10 9AB, Herts, England. EM m.j.hardcastle@herts.ac.uk RI Hardcastle, Martin/E-2264-2012; Massaro, Francesco/L-9102-2016 OI Hardcastle, Martin/0000-0003-4223-1117; Massaro, Francesco/0000-0002-1704-9850 FU Royal Society; Foundation BLANCEFLOR Boncompagni-Ludovisi; NASA [NASA grant GO9-0110X] FX We thank Judith Croston for helpful discussions of the central density in poor groups, Clive Tadhunter for providing emission-line images and Avanti Tilak for help with the [O III] luminosity of 3C 171. MJH thanks the Royal Society for a research fellowship. FM acknowledges the Foundation BLANCEFLOR Boncompagni-Ludovisi, nee Bildt, for the grant awarded him in 2009 to support his research. Work at SAO was supported by NASA grant GO9-0110X. NR 40 TC 8 Z9 8 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 FEB 1 PY 2010 VL 401 IS 4 BP 2697 EP 2705 DI 10.1111/j.1365-2966.2009.15855.x PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 544VQ UT WOS:000273687800044 ER PT J AU Katsova, MM Livshits, MA Soon, W Baliunas, SL Sokoloff, DD AF Katsova, M. M. Livshits, M. A. Soon, W. Baliunas, S. L. Sokoloff, D. D. TI Differential rotation of some HK-Project stars and the butterfly diagrams SO NEW ASTRONOMY LA English DT Article DE Stellar rotation; Late-type stars; Solar activity ID CYCLES; SUN AB We analyze the long-term variability of the chromospheric radiation of 20 stars monitored in the course of the HK-Project at the Mount Wilson Observatory. We apply the modified wavelet algorithm for this set of gapped time series. Besides the mean rotational periods for all these stars, we find reliable changes of the rotational periods from year to year for a few stars. Epochs of slower rotation occur when the activity level of the star is high, and the relationship repeats again during the next maximum of an activity cycle. Such an effect is traced in two stars with activity cycles that are not perfectly regular (but labeled "Good" under the classification in [Baliunas, S.L., Donahue, R.A., Soon, W.H., Horne, J.H., Frazer, J.. Woodard-Eklund, L., Bradford, M., Rao, L.M., Wilson, O.C., Zhang, Q. et al., 1995. ApJ 438,269.]) but the two stars have mean activity levels exceed that of the Sun. The averaged rotational period of HD 115404 is 18.5 days but sometimes the period increases up to 21.5 days. The sign of the differential rotation is the same as the Sun's, and the value Delta Omega/(Omega) = -0.14. For the star HD 149661, this ratio is -0.074. Characteristic changes of rotational periods occur over around three years when the amplitude of the rotational modulation is large. These changes can be transformed into latitude-time butterfly diagrams with minimal a priori assumptions. We compare these results with those for the Sun as a star and conclude that epochs when surface inhomogeneities rotate slower are synchronous with the reversal of the global magnetic dipole. (C) 2009 Elsevier B.V. All rights reserved. C1 [Sokoloff, D. D.] Moscow MV Lomonosov State Univ, Dept Phys, Moscow, Russia. [Katsova, M. M.] Moscow MV Lomonosov State Univ, Sternberg State Astron Inst, Moscow, Russia. [Livshits, M. A.] Russian Acad Sci, Pushkov Inst Terr Magnetism Ionosphere & Radio Wa, Troitsk, Moscow Region, Russia. [Soon, W.; Baliunas, S. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Sokoloff, DD (reprint author), Moscow MV Lomonosov State Univ, Dept Phys, Moscow, Russia. EM maria@sai.msu.ru; d_sokoloff@hotmail.com FU RFBR [09-02-01010]; ISTC [3726]; [1685.2008.2]; [4573.2008.2] FX The work by MK and ML is supported financially by the Grants 09-02-01010 (RFBR) and 1685.2008.2 and 4573.2008.2. DS is grateful to ISTC for financial support under Grant 3726. NR 11 TC 15 Z9 15 U1 0 U2 1 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1384-1076 J9 NEW ASTRON JI New Astron. PD FEB PY 2010 VL 15 IS 2 BP 274 EP 281 DI 10.1016/j.newast.2009.08.003 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 518YK UT WOS:000271732000010 ER PT J AU Cernusak, LA Winter, K Turner, BL AF Cernusak, Lucas A. Winter, Klaus Turner, Benjamin L. TI Leaf nitrogen to phosphorus ratios of tropical trees: experimental assessment of physiological and environmental controls SO NEW PHYTOLOGIST LA English DT Article DE leaf nitrogen concentration; leaf nitrogen to phosphorus ratio; leaf phosphorus concentration; relative growth rate; water-use efficiency ID WATER-USE EFFICIENCY; N-P STOICHIOMETRY; PLANT-GROWTH; NUTRIENT AVAILABILITY; ISOTOPE COMPOSITION; SOIL FERTILITY; LIMITATION; TRANSPIRATION; DELTA-O-18; DELTA-C-13 AB We investigated the variation in leaf nitrogen to phosphorus ratios of tropical tree and liana seedlings as a function of the relative growth rate, whole-plant water-use efficiency, soil water content and fertilizer addition. First, seedlings of 13 tree and liana species were grown individually in 38-l pots prepared with a homogeneous soil mixture. Second, seedlings of three tree species were grown in 19-l pots at high or low soil water content, and with or without added fertilizer containing nitrogen, phosphorus and potassium. For plants grown under common soil conditions, leaf nitrogen to phosphorus ratios showed a unimodal, or hump-shaped, relationship with the relative growth rate. The leaf nitrogen to phosphorus ratio increased in response to low soil water content in three species, and increased in response to fertilizer addition in two of the three species. Across all species and treatments, the leaf nitrogen to phosphorus ratio was positively correlated with the water-use efficiency. The results suggest that the within-site variation among tropical tree species in the leaf nitrogen to phosphorus ratio may be caused by associations between this ratio and the relative growth rate. Modification of the soil environment changed the leaf nitrogen to phosphorus ratio, but underlying associations between this ratio and the relative growth rate were generally maintained. The observed correlation between the leaf nitrogen to phosphorus ratio and water-use efficiency has implications for linking nutrient stoichiometry with plant transpiration. C1 [Cernusak, Lucas A.; 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 Smithsonian Tropical Research Institute; Australian Research Council FX We thank Jorge Aranda, Milton Garcia, Aurelio Virgo, Lisa Petheram, Carlos Martinez, Tania Romero and Aneth Sarmiento for technical assistance in carrying out the experiments. Lucas A. Cernusak was supported by a Tupper Postdoctoral Fellowship from the Smithsonian Tropical Research Institute and by an Australian Postdoctoral Fellowship from the Australian Research Council. NR 40 TC 39 Z9 41 U1 5 U2 52 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0028-646X J9 NEW PHYTOL JI New Phytol. PD FEB PY 2010 VL 185 IS 3 BP 770 EP 779 DI 10.1111/j.1469-8137.2009.03106.x PG 10 WC Plant Sciences SC Plant Sciences GA 544VR UT WOS:000273687900018 PM 19968799 ER PT J AU Baxter, SW Nadeau, NJ Maroja, LS Wilkinson, P Counterman, BA Dawson, A Beltran, M Perez-Espona, S Chamberlain, N Ferguson, L Clark, R Davidson, C Glithero, R Mallet, J McMillan, WO Kronforst, M Joron, M Ffrench-Constant, RH Jiggins, CD AF Baxter, Simon W. Nadeau, Nicola J. Maroja, Luana S. Wilkinson, Paul Counterman, Brian A. Dawson, Anna Beltran, Margarita Perez-Espona, Silvia Chamberlain, Nicola Ferguson, Laura Clark, Richard Davidson, Claire Glithero, Rebecca Mallet, James McMillan, W. Owen Kronforst, Marcus Joron, Mathieu Ffrench-Constant, Richard H. Jiggins, Chris D. TI Genomic Hotspots for Adaptation: The Population Genetics of Mullerian Mimicry in the Heliconius melpomene Clade SO PLOS GENETICS LA English DT Article ID HYBRID ZONE; COLOR PATTERN; LINKAGE DISEQUILIBRIUM; REPRODUCTIVE ISOLATION; DNA POLYMORPHISM; WARNING-COLOR; BUTTERFLIES; EVOLUTION; DROSOPHILA; DIVERSITY AB Wing patterning in Heliconius butterflies is a longstanding example of both Mullerian mimicry and phenotypic radiation under strong natural selection. The loci controlling such patterns are "hotspots" for adaptive evolution with great allelic diversity across different species in the genus. We characterise nucleotide variation, genotype-by-phenotype associations, linkage disequilibrium, and candidate gene expression at two loci and across multiple hybrid zones in Heliconius melpomene and relatives. Alleles at HmB control the presence or absence of the red forewing band, while alleles at HmYb control the yellow hindwing bar. Across HmYb two regions, separated by similar to 100 kb, show significant genotype-by-phenotype associations that are replicated across independent hybrid zones. In contrast, at HmB a single peak of association indicates the likely position of functional sites at three genes, encoding a kinesin, a G-protein coupled receptor, and an mRNA splicing factor. At both HmYb and HmB there is evidence for enhanced linkage disequilibrium (LD) between associated sites separated by up to 14 kb, suggesting that multiple sites are under selection. However, there was no evidence for reduced variation or deviations from neutrality that might indicate a recent selective sweep, consistent with these alleles being relatively old. Of the three genes showing an association with the HmB locus, the kinesin shows differences in wing disc expression between races that are replicated in the co-mimic, Heliconius erato, providing striking evidence for parallel changes in gene expression between Mullerian co-mimics. Wing patterning loci in Heliconius melpomene therefore show a haplotype structure maintained by selection, but no evidence for a recent selective sweep. The complex genetic pattern contrasts with the simple genetic basis of many adaptive traits studied previously, but may provide a better model for most adaptation in natural populations that has arisen over millions rather than tens of years. C1 [Baxter, Simon W.; Nadeau, Nicola J.; Maroja, Luana S.; Dawson, Anna; Beltran, Margarita; Ferguson, Laura; Jiggins, Chris D.] Univ Cambridge, Dept Zool, Cambridge, England. [Maroja, Luana S.] Smithsonian Trop Res Inst, Balboa, Panama. [Wilkinson, Paul; Ffrench-Constant, Richard H.] Univ Exeter Cornwall, Sch Biosci, Penryn, England. [Counterman, Brian A.; McMillan, W. Owen] N Carolina State Univ, Dept Genet, Raleigh, NC 27695 USA. [Perez-Espona, Silvia] Univ Bristol, Sch Biol Sci, Bristol, Avon, England. [Chamberlain, Nicola; Kronforst, Marcus] Harvard Univ, Harvard FAS Ctr Syst Biol, Cambridge, MA 02138 USA. [Clark, Richard; Davidson, Claire; Glithero, Rebecca] Wellcome Trust Sanger Inst, Cambridge, England. [Mallet, James] UCL, Galton Lab, London, England. [Joron, Mathieu] Museum Natl Hist Nat, Dept Systemat & Evolut, F-75231 Paris, France. RP Baxter, SW (reprint author), Univ Cambridge, Dept Zool, Cambridge, England. EM c.jiggins@zoo.cam.ac.uk RI Joron, Mathieu/C-9178-2009; mallet, james/B-5114-2008; Perez-Espona, Silvia/G-2294-2010; Nadeau, Nicola/E-1149-2011; Jiggins, Chris/B-9960-2008 OI Joron, Mathieu/0000-0003-1043-4147; ffrench-Constant, Richard/0000-0001-5385-9888; Davidson, Claire/0000-0002-4910-8202; Perez-Espona, Silvia/0000-0001-7098-4904; Nadeau, Nicola/0000-0002-9319-921X; Jiggins, Chris/0000-0002-7809-062X FU BBSRC [011845]; Leverhulme Trust [F/09364/E]; NERC [D00114/2]; Royal Society Fellowship; National Science Foundation [DEB-0715096, IBN-0344705] FX This work was principally funded by a BBSRC grant (011845) to CDJ and RHf- C, and also supported by a Leverhulme Trust award (F/09364/E), a NERC grant (D00114/2), and a Royal Society Fellowship to CDJ. Funding for the H. erato BAC sequencing was provided by National Science Foundation grants to WOM (DEB-0715096 and IBN-0344705). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 65 TC 41 Z9 42 U1 1 U2 24 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 FEB PY 2010 VL 6 IS 2 AR e1000794 DI 10.1371/journal.pgen.1000794 PG 12 WC Genetics & Heredity SC Genetics & Heredity GA 565BG UT WOS:000275262700027 PM 20140188 ER PT J AU Mahon, AR Thornhill, DJ Norenburg, JL Halanych, KM AF Mahon, Andrew R. Thornhill, Daniel J. Norenburg, Jon L. Halanych, Kenneth M. TI DNA uncovers Antarctic nemertean biodiversity and exposes a decades-old cold case of asymmetric inventory SO POLAR BIOLOGY LA English DT Article DE Antarctica; Biodiversity; Cryptic species; 16S; Larvae ID PHYLUM NEMERTEA; OCEAN BARRIERS; POLAR FRONT; SEA; PHYLOGENY; TEMPERATURE; DIVERSITY; LARVAE; RECORD; HETERONEMERTEA AB With threats to biodiversity posed by anthropogenic impacts and global climate change, characterization of existing flora and fauna is increasingly important, but continues to focus predominantly on easily studied taxa. In the Southern Ocean, levels of species richness remain relatively unexplored due to remoteness and difficulties of sampling the region. Nemerteans (proboscis worms; ribbon worms) are unusually abundant and occasionally conspicuous in the Antarctic region. Despite being routinely collected, difficulties in preserving voucher material, morphological limitations, and shortage of taxonomic expertise have hindered our understanding of nemertean diversity. To assess patterns of diversity, we examined a fragment of the mitochondrial 16S rRNA gene from larval and adult nemerteans (n = 192) from 53 sites along the western Antarctic Peninsula. We found 20 distinct lineages having an uncorrected genetic distance (p) greater than 5% to the nearest sister taxon or group, 19 of which have not been genetically characterized in previous studies. Additionally, the putatively dominant adult species in the region, Parborlasia corrugatus, was found to comprise only 4.3% of larvae sampled (n = 3 out of 69 samples from 12 locations). Of 47 nemertean species recorded from Antarctic waters, 20 are heteronemerteans and therefore could have a pelagic pilidium larval phase. These results suggest that Antarctic biodiversity is underestimated, and that unknown species of nemerteans await description from Southern Ocean waters. C1 [Mahon, Andrew R.; Thornhill, Daniel J.; Halanych, Kenneth M.] Auburn Univ, Dept Biol Sci, Auburn, AL 36849 USA. [Mahon, Andrew R.] Univ Notre Dame, Dept Biol Sci, Ctr Aquat Conservat, Notre Dame, IN 46617 USA. [Thornhill, Daniel J.] Bowdoin Coll, Dept Biol, Brunswick, ME 04011 USA. [Norenburg, Jon L.] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20013 USA. RP Mahon, AR (reprint author), Univ Notre Dame, Dept Biol Sci, Ctr Aquat Conservat, Galvin Hall, Notre Dame, IN 46556 USA. EM amahon@nd.edu; thornhill.dan@gmail.com; norenburgj@si.edu; ken@auburn.edu RI Thornhill, Daniel/A-7730-2009; Halanych, Ken/A-9480-2009; Norenburg, Jon/K-3481-2015 OI Halanych, Ken/0000-0002-8658-9674; Norenburg, Jon/0000-0001-7776-1527 FU ASRV Laurence M. Gould [LMG 04-14, LMG 06-05]; National Science Foundation [OPP-9910164, OPP-0338087, OPP-0338218, OPP-0132032] FX We would like to thank R. S. Scheltema for his assistance in this work. Additionally, we thank H. W. Deitrich, S. J. Lockhart for sharing samples for this investigation and also to S. Santos for insightful discussions leading to this work. The Edison-Chouest Offshore crew, Raytheon personnel, and scientific participants of the ASRV Laurence M. Gould in the 2004 and 2006 Antarctic cruises (LMG 04-14 and LMG 06-05, respectively) are gratefully acknowledged for their help and logistical support. This work was supported by a National Science Foundation grants to R. S. Scheltema and K. M. Halanych (OPP-9910164, OPP-0338087, OPP-0338218), and to H. W. Detrich (OPP-0132032). This work is AU Marine Biology Program contribution number 56. NR 57 TC 21 Z9 22 U1 0 U2 11 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0722-4060 J9 POLAR BIOL JI Polar Biol. PD FEB PY 2010 VL 33 IS 2 BP 193 EP 202 DI 10.1007/s00300-009-0696-0 PG 10 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 543QW UT WOS:000273594300006 ER PT J AU Clough, GW AF Clough, G. Wayne TI SI in the City 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 FEB PY 2010 VL 40 IS 11 BP 24 EP 24 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 546SE UT WOS:000273830500013 ER PT J AU Sayer, EJ Tanner, EVJ AF Sayer, E. J. Tanner, E. V. J. TI A new approach to trenching experiments for measuring root-rhizosphere respiration in a lowland tropical forest SO SOIL BIOLOGY & BIOCHEMISTRY LA English DT Article DE Rhizosphere; Soil respiration partitioning; Trenching experiments; Litter addition; Litter removal; Soil CO(2) efflux; Soil temperature; Soil water availability ID ELEVATED ATMOSPHERIC CO-2; SOIL CO2 EFFLUX; INCREASED LITTERFALL; CARBON ALLOCATION; TROPOSPHERIC O-3; RAIN-FOREST; LEAF-LITTER; BIOMASS; ECOSYSTEMS; DYNAMICS AB Soil respiration in tropical forests is a major source of atmospheric CO(2). The ability to partition soil respiration into its individual components is becoming increasingly important to predict the effects of disturbance on CO(2) efflux from the soil as the responses of heterotrophic and autotrophic respiration to change are likely to differ. However, current field methods to partition respiration suffer from various methodological artefacts; root-rhizosphere respiration is particularly difficult to estimate. We used trenched subplots to estimate root-rhizosphere respiration in large-scale litter addition (L+), litter removal (L-) and control (CT) plots in a lowland tropical semi-evergreen forest in Panama. We took a new approach to trenching by making measurements immediately before-and-after trenching and comparing them to biweekly measurements made over one year. Root-rhizosphere respiration was estimated to be 38%, 17% and 27% in the Cr, L+, and L- plots, respectively, from the measurements taken immediately before and one day after trenching in May-June 2007. Biweekly measurements over the following year provided no estimates of root-rhizosphere respiration for the first seven months due to decomposition of decaying roots. We were also unable to estimate root-rhizosphere respiration during the dry season due to differences in soil water content between trenched and untrenched soil. However, biweekly measurements taken during the early rainy season one year after trenching (May-June 2008) provided estimates of root-rhizosphere respiration of 39%, 24% and 36% in the CT, L+, and L- plots, respectively, which are very similar to those obtained during the first day after trenching. We suggest that measurements taken immediately before and one day after root excision are a viable method for a rapid estimation of root-rhizosphere respiration without the methodological artefacts usually associated with trenching experiments. (C) 2009 Elsevier Ltd. All rights reserved. C1 [Sayer, E. J.; Tanner, E. V. J.] Univ Cambridge, Dept Plant Sci, Cambridge CB2 3EA, England. [Sayer, E. J.] Smithsonian Trop Res Inst, Panama City, 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 European Union Marie-Curie Outgoing Fellowship [MOIF-CT-2005-21728]; Smithsonian Tropical Research Institute, Panama; Mellon Fund, Gonville; Caius College, Cambridge; Department of Plant Sciences, Cambridge FX We thank Francisco Valdez, Didimo Urena, Arturo Worrell Jr., Seferino Valdez, Simon Valdez, and Oliver Gonzalez for help in the field. We also thank Andrew Nottingham and two anonymous reviewers for constructive comments on earlier versions of the manuscript. EJS was funded by a European Union Marie-Curie Outgoing Fellowship MOIF-CT-2005-21728, and the Smithsonian Tropical Research Institute, Panama; EVT was funded by the Mellon Fund, 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 to whom we are very grateful. NR 39 TC 18 Z9 22 U1 5 U2 43 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0038-0717 J9 SOIL BIOL BIOCHEM JI Soil Biol. Biochem. PD FEB PY 2010 VL 42 IS 2 BP 347 EP 352 DI 10.1016/j.soilbio.2009.11.014 PG 6 WC Soil Science SC Agriculture GA 548FW UT WOS:000273946300027 ER PT J AU Liu, AZ Kress, WJ Li, DZ AF Liu, Ai-Zhong Kress, W. John Li, De-Zhu TI Phylogenetic analyses of the banana family (Musaceae) based on nuclear ribosomal (ITS) and chloroplast (trnL-F) evidence SO TAXON LA English DT Article DE biogeography; ITS; molecular phylogeny; Musaceae; trnL-F ID SEQUENCE DATA; MOLECULAR EVIDENCE; WILD BANANAS; SP-NOV; CHINA; POLLINATION; GENUS; DNA; YUNNAN; TREES AB The banana family (Musaceae s.str.; Zingiberales), an economically important tropical group of plant, includes three genera, Musa, Ensete and Musella, and possible 41 species. We performed phylogenetic analyses of a total of 39 accessions covering 28 species in the Musaceae and five outgroup species using nuclear ribosomal ITS and chloroplast trnL-F sequences. Outgroups were chosen from the closely related families Lowiaceae. Strelitziaceae, and Heliconiaceae. Our results suggest that Musaceae s.str. is monophyletic. Three main internal clades are well-supported within the fmaily. The genus Musa is comprised of two of these clades, and Musella plus Ensete make-up the third clade. The sectional classification system of Musa based on chromosome numbers is not supported by DNA sequence evidence. Both inflorescence orientation (erect or pendent) and chromosomal number in Musa, which were characters traditionally though to be diagnostic in sectional classification, are homoplasious traits in the family. The disjunct distribution of living members of the genus Ensete in tropical Asia and Africa with a fossil species described from the Ecocene of Oregon in North America may be an example of the distributional retreat of the Boreal Tropics. The phylogenetic position of the monospecific Musella as sister to the African clade of Ensete suggests that the single species in this lineage is a highly specialized member not warranting generic status. Evidence from the molecular phylogenetic investigations highlights the evolutionary diversification and biogeographic context of this plant group, and suggests additional taxonomic investigations of both Musa and Ensete are in order. C1 [Liu, Ai-Zhong; Kress, W. John] Chinese Acad Sci, Xishuangbanna Trop Bot Garden, Kunming 650223, Yunnan, Peoples R China. [Liu, Ai-Zhong; Li, De-Zhu] Chinese Acad Sci, Kunming Inst Bot, Key Lab Biodivers & Biogeog, Kunming 650204, Yunnan, Peoples R China. [Kress, W. John] Natl Museum Nat Hist, Dept Bot, Smithsonian Inst, MRC 166, Washington, DC 20013 USA. RP Liu, AZ (reprint author), Chinese Acad Sci, Xishuangbanna Trop Bot Garden, 88 Xuefu Rd, Kunming 650223, Yunnan, Peoples R China. EM liuaizhong@xtbg.ac.cn RI Liu, aizhong/F-1770-2010 FU National Basic Research Program of China [2007CB411601]; Natural Science Foundation of China [30871548]; National Museum of Natural History Biotic Services; National Geographic Society FX We thank Dr. Linda prince, Ms. Ida Lopez, and Mr. Lee Weigt for their laboratory assistance, Dr. Elizabeth Zimmer for her critical comments oil in earlier draft, Mr. Mike Bordelon for his assistance with living plants and Mr. Markku Hakkinen (Helsinki University Botanic Garden. Finland) for providing samples. This research was jointly supported by National Basic Research Program of China (973 Program: 2007CB411601 to DC-ZhU Li), Natural Science Foundation of China (30871548). and Smithsonian's Scholarly Studies, Program. the National Museum of Natural History Biotic Services and Inventories Program, and the National Geographic Society. NR 83 TC 16 Z9 20 U1 1 U2 12 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 FEB PY 2010 VL 59 IS 1 BP 20 EP 28 PG 9 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA 555AE UT WOS:000274478100003 ER PT J AU Chen, JH Sun, H Wen, J Yang, YP AF Chen, Jia-Hui Sun, Hang Wen, Jun Yang, Yong-Ping TI Molecular phylogeny of Salix L. (Salicaceae) inferred from three chloroplast datasets and its systematic implications SO TAXON LA English DT Article DE atpB-rbcL; chloroplast markers; molecular phylogeny; rbcL; Salicaceae; Salix; systematics; trnD-T ID RIBULOSE 1,5-BISPHOSPHATE CARBOXYLASE; NORTHERN-HEMISPHERE; UNIVERSAL PRIMERS; LARGE SUBUNIT; EASTERN ASIA; DNA; TERTIARY; BIOGEOGRAPHY; AMPLIFICATION; EVOLUTION AB Salix is a taxonomically difficult genus and its generic limits and infrageneric division are still highly controversial. We employed sequences of the chloroplast rbcL gene, trnD-T spacer and atpB-rbcL spacer for phylogenetic analyses of Salix. The results strongly support that Salix. Toisusu and Chosenia form a monophyletic group, confirming the merge of Toisusu and Chosenia with Salix. Within Salix s.l., two major clades are recognizable; one contains species of subgenus Salix (excluding sections Triandrae and Urbanianae), with the New World and the Old World species forming strongly supported clades, respectively; and the other includes sections Triandrae, Urbanianae, Chosenia and all species of subgenera Chamaetia and Vetrix, with the latter two subgenera forming a robustly supported subclade but with low resolution. A new infrageneric classification of Salix is herein proposed. The previously recognized subgenus Salix is split into three subgenera: Salix, Chosenia and Triandrae, and subgenera Chamaetia and Vetrix are combined as subgenus Vetrix. C1 [Chen, Jia-Hui; Sun, Hang; Wen, Jun; Yang, Yong-Ping] Chinese Acad Sci, Kunming Inst Bot, Key Lab Biodivers & Biogeog, Kunming 650204, Yunnan, Peoples R China. [Chen, Jia-Hui; Yang, Yong-Ping] Chinese Acad Sci, Inst Tibet Plateau Res Kunming, Kunming 650204, Yunnan, Peoples R China. [Wen, Jun] Natl Museum Nat Hist, Dept Bot, Smithsonian Inst, Washington, DC 20013 USA. [Wen, Jun] Chinese Acad Sci, Inst Bot, Lab Systemat & Evolutionary Bot, Beijing 100093, Peoples R China. RP Yang, YP (reprint author), Chinese Acad Sci, Kunming Inst Bot, Key Lab Biodivers & Biogeog, Kunming 650204, Yunnan, Peoples R China. EM yangyp@mail.kib.ac.cn FU National Natural Science Foundation of china [NSFC 30900085, 40930209, 30625004, 40771073]; Chinese Academy of Scienc; Yunnan Natural Science Foundation [2008CC013]; U.S. National Science Foundation [DEB-0321846] FX We thank the Botanical Garden of Tohoku University, Kazumi Fujikawa, George W. Argus (Canadian Museum of Nature), the Harvard University Herbaria (HUH), and the Herbarium of Kunming Institute of Botany (KUN) For providing experimental materials and George W. Argus, Zelong Nie and two anonymous reviewers for providing valuable comments of the manuscript. This study was suppported by grants from the National Natural Science Foundation of china (NSFC 30900085 to J.H. Chen and 40930209, 30625004 40771073 to H. Sun), the Xibuzhiguang (Light in western China) project of the Chinese Academy of Science (to Chen), Yunnan Natural Science Foundation (2008CC013 to H. Sun). and U.S. National Science Foundation (DEB-0321846 to David. E. Boufford). NR 71 TC 20 Z9 26 U1 3 U2 30 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 FEB PY 2010 VL 59 IS 1 BP 29 EP 37 PG 9 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA 555AE UT WOS:000274478100004 ER PT J AU Borges, A Bermingham, E Herrera, N Alfonzo, MJ Sanjur, OI AF Borges, Adolfo Bermingham, Eldredge Herrera, Nimiadina Alfonzo, Marcelo J. Sanjur, Oris I. TI Molecular systematics of the neotropical scorpion genus Tityus (Buthidae): The historical biogeography and venom antigenic diversity of toxic Venezuelan species SO TOXICON LA English DT Review DE Tityus; Scorpion; Mitochondrial DNA; 16S rRNA; Cytochrome oxidase I; Historical biogeography; Molecular clocks; Venom antigenicity ID PHYLOGENETIC INFERENCE; BRAZILIAN AMAZONIA; PROTEOMIC ANALYSIS; DIVERGENCE TIME; NORTHERN ANDES; DNA-SEQUENCES; MANAUS REGION; FAUNA; DISCREPANS; EVOLUTION AB We provide a mitochondrial DNA-based phylogenetic hypothesis for 21 Tityus species collected in Venezuela, Trinidad, Brazil and Panama, including 12 taxa known to be toxic to humans. Our phylogenetic reconstruction is based on 850 nucleotides of the combined cytochrome oxidase subunit I and 16S rRNA genes for most species, and centered on Venezuelan scorpions owing to the detailed taxonomic and biogeographic information available for Tityus in this region. The principal phylogenetic result was the strong support for mtDNA clades representing geographical groupings associated with the Perija mountain range, the Merida Andes, or the central and eastern coastal ranges in Venezuela, suggesting that vicariance has been a potent force in the diversification of local scorpions. Venezuelan Tityus species have been organized by Gonzalez-Sponga into three artificial morphological groups, "androcottoides", "discrepans", and "nematochirus", based on the array of ventral carinae in metasomal segments II-IV. We also incorporated a fourth morphological group ("Tityus clathratus"), recently documented in Venezuela. Our results do not support the clustering of the species in the "androcottoides" and "discrepans" morphological groups, which include the majority of taxa of medical importance, but provided support for the "nematochirus" species group. T clathratus was found to cluster with the Brazilian T serrulatus and T bahiensis. Divergence times of most clades are consistent with major events in the geological history of northern Venezuela and suggest that many Venezuelan Tityus species formed in the late Miocene and the Pliocene. In turn, we used the Tityus mtDNA phylogeny to determine the potential utility of phylogenetic systematics to predict Tityus venom antigenic reactivity by testing the recognition of T norotientalis, T discrepans, T zulianus, T perijanensis, and T clathratus venoms by anti-T discrepans horse antibodies. Cross-reactivity was significantly higher for the closely related eastern (T nororientalis) and central coastal (T discrepans) species in comparison to the distantly related Andean (T zulianus) and Perija (T perijanensis) species. Reactivity of T clathratus low mol. mass toxic components towards anti-T serrulatus and anti-T. discrepans antivenoms was low, suggesting that venom components produced by the subgenus Archaeotityus (which encompass "clathratus" species) diverge antigenically from other Tityus scorpions. (C) 2009 Elsevier Ltd. All rights reserved. C1 [Borges, Adolfo] Cent Univ Venezuela, Fac Med, Inst Expt Med, Lab Biol Mol Toxinas & Receptores, Caracas 1051, Venezuela. [Bermingham, Eldredge; Herrera, Nimiadina; Sanjur, Oris I.] Smithsonian Trop Res Inst, Panama City, Panama. RP Borges, A (reprint author), Cent Univ Venezuela, Fac Med, Inst Expt Med, Lab Biol Mol Toxinas & Receptores, Box 50587, Caracas 1051, Venezuela. EM borges.adolfo@gmail.com FU Fondo Nacional de Ciencia; Tecnologia e Innovacion [S1-2001000674, PI-2004000385] FX We are very indebted to the numerous people who assisted our collections. We are extremely grateful to the late Professor Manuel A. Gonzalez-Sponga, Institute of Tropical Zoology, Central University of Venezuela, for his advice in the identification of Venezuelan specimens and for his encouragement. We are also thankful to Dr. Sylvia Lucas, Butantan Institute, sao Paulo, Brasil, for the kind gift of T serrulatus and T bahiensis specimens. We are most grateful to Dr. Leonardo De Sousa, Laboratorio de Toxinologia, Nucleo de Anzoategui, Universidad de Oriente, Venezuela, for kindly donating specimens of T gonzalespongai and T quirogae, for his advice in many matters, and for the wonderful "scorpion" conversations. We are indebted to Fernando Rojas-Runjaic, who was instrumental in sampling T perijanensis from Zulia State and for his critical reading of the manuscript. Jesus Manzanilla, Michael Jowers and their co-workers from the University of Glasgow provided us with a home-away-from-home during our stay in Trinidad and outstanding help in the field and with logistics. We are grateful to the Wildlife Section, Forestry Division, Ministry of Agriculture, Land and Marine Resources, Republic of Trinidad and Tobago, for issuing the necessary collection and export permits. Dr. Carmen Garcia, Instituto de Medicina Experimental, assisted with DNA extractions and many difficult PCR assays. Maribel Gonzalez (Smithsonian Tropical Research Institute, Naos Laboratories) is gratefully acknowledged for her skillful technical their help with phylogenetic analyses. Thanks are conveyed to Jose Faks for his assistance with protein electrophoresis. Financial support was provided by Fondo Nacional de Ciencia, Tecnologia e Innovacion (FONACIT-Venezuela), Grants S1-2001000674 and PI-2004000385 (to A.B.), and the Smithsonian Institution for a Short-term Visiting Fellowship to A.B. during a visit to E.B.'s laboratory. NR 128 TC 16 Z9 16 U1 1 U2 11 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 FEB-MAR PY 2010 VL 55 IS 2-3 BP 436 EP 454 DI 10.1016/j.toxicon.2009.09.011 PG 19 WC Pharmacology & Pharmacy; Toxicology SC Pharmacology & Pharmacy; Toxicology GA 556GU UT WOS:000274579100034 PM 19799925 ER PT J AU McCormick, MK Kettenring, KM Baron, HM Whigham, DF AF McCormick, Melissa K. Kettenring, Karin M. Baron, Heather M. Whigham, Dennis F. TI Extent and Reproductive Mechanisms of Phragmites australis Spread in Brackish Wetlands in Chesapeake Bay, Maryland (USA) SO WETLANDS LA English DT Article DE Clonal propagation; Genetic diversity; Invasive species; Non-native genotype; Rhode River; Seeds ID COMMON REED; GENETIC DIVERSITY; POPULATION-GENETICS; CHROMOSOME-NUMBERS; CLONAL STRUCTURE; SALT MARSHES; INVASION; DISPERSAL; STATISTICS; MANAGEMENT AB The number of patches of non-native Phragmites australis in brackish tidal wetlands in the Rhode River subestuary increased from 5 in 1971-72 to 212 in 2007, and the area covered by the patches increased more than 25 times during the same time interval. Genetic analysis of the patches showed that the expansion has primarily been from seed, and genetic similarities between patches indicate that most cross-pollination occurs within a distance of 50 m. Comparison of patches in different parts of the subestuary indicate that the expansion of Phragmites australis has occurred at the scale of the entire subestuary and not the scale of subsections of the subestuary dominated by differing upland land-uses. C1 [McCormick, Melissa K.; Kettenring, Karin M.; Baron, Heather M.; Whigham, Dennis F.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP McCormick, MK (reprint author), Smithsonian Environm Res Ctr, Box 28, Edgewater, MD 21037 USA. EM mccormickm@si.edu OI Whigham, Dennis/0000-0003-1488-820X FU Pennsylvania State University on an EPA [692105] FX This research was supported through a subcontract with Pennsylvania State University on an EPA STAR grant (692105), Denice Wardrop, Principal Investigator, a Smithsonian Postdoctoral Fellowship to KMK, and a Smithsonian Work-learn internship to HMB. Mark Brinson and two anonymous reviewers provided valuable comments on earlier drafts of the manuscript. NR 40 TC 45 Z9 46 U1 4 U2 21 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0277-5212 J9 WETLANDS JI Wetlands PD FEB PY 2010 VL 30 IS 1 BP 67 EP 74 DI 10.1007/s13157-009-0007-0 PG 8 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA 569ZX UT WOS:000275642500006 ER PT J AU Fitzgerald, EMG AF Fitzgerald, Erich M. G. TI The morphology and systematics of Mammalodon colliveri (Cetacea: Mysticeti), a toothed mysticete from the Oligocene of Australia SO ZOOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Review DE evolution; Mammalodontidae; phylogeny; whale ID WHALE PHYLOGENY; NEW-ZEALAND; SOUTHEASTERN AUSTRALIA; EARLY MIOCENE; BALEEN WHALE; LATE EOCENE; INNER-EAR; EVOLUTION; WATER; ODONTOCETI AB Mammalodon colliveri is an unusual toothed archaic mysticete (Cetacea) from the Upper Oligocene Jan Juc Formation of south-east Australia. The morphology of the holotype skull and postcrania are described in detail. Superimposed on the generally plesiomorphic archaeocete-like morphology of Mammalodon are subtle mysticete synapomorphies. Derived features of Mammalodon include a short and bluntly rounded rostrum, reduced premaxillae, and anterodorsally directed orbits. Within Mysticeti, this suite of features is unique. The aberrant rostral morphology of Mammalodon suggests specialization for suction feeding. Janjucetus hunderi is placed in an expanded family Mammalodontidae. Phylogenetic analysis corroborates the monophyly of Basilosauridae, Neoceti, Odontoceti, and Mysticeti, and yields a novel hypothesis of toothed mysticete relationships: a basal clade of undescribed toothed mysticetes from South Carolina, a Llanocetidae + Mammalodontidae clade, and monophyletic Aetiocetidae are posited as successive sister taxa to edentulous baleen whales (Chaeomysticeti). Toothed archaic mysticetes clearly employed diverse prey capture strategies, with exaptations for filter feeding evolving sequentially in stem group Mysticeti. A stratigraphically calibrated phylogeny implies that the initial diversification of Mysticeti occurred during the Late Eocene. (C) 2009 The Linnean Society of London, Zoological Journal of the Linnean Society, 2010, 158, 367-476. doi: 10.1111/j.1096-3642.2009.00572.x C1 [Fitzgerald, Erich M. G.] Monash Univ, Sch Geosci, Clayton, Vic 3800, Australia. [Fitzgerald, Erich M. G.] Museum Victoria, Melbourne, Vic 3001, Australia. [Fitzgerald, Erich M. G.] Smithsonian Inst, Natl Museum Nat Hist, Div Mammals, NHB MRC 108, Washington, DC 20013 USA. RP Fitzgerald, EMG (reprint author), Monash Univ, Sch Geosci, Clayton, Vic 3800, Australia. EM efitzgerald@museum.vic.gov.au FU Australian Postgraduate Award; South Australian Museum FX I wish to dedicate this article to the late George Baxter Pritchard and Frederick Stanley Colliver in acknowledgement of their efforts in the collection, study, and long-term preservation of the holotype of Ma. colliveri. Ewan Fordyce is thanked for preparing the holotype of Ma. colliveri. I thank Peter Hayward for his editorial comments, and Ewan Fordyce and an anonymous referee for their constructive reviews of the manuscript. My fellow graduate students at Monash University and Museum Victoria are thanked for their discussion of ideas articulated in this article. Thomas Darragh and Stephen Gallagher are thanked for providing invaluable discussion on the stratigraphy and sedimentology of the Torquay Group. For their contemplation of Mammalodon, I wish to thank Larry Barnes, Brian Beatty, David Bohaska, Ewan Fordyce, John Long, James Mead, Nicholas Pyenson, Karen Roberts, and Anne Warren, although these individuals do not necessarily agree with all the conclusions reached in this article. I am especially grateful to Frank C. Whitmore Jr, for his hospitality and generosity in discussing fossil Cetacea. Jonathan Geisler and Mark Uhen produced constructive criticisms on an early draft of the periotic description presented herein. Tom Rich and Pat Vickers-Rich read a draft of the manuscript. Philip Gingerich and the University of Michigan Museum of Paleontology kindly produced casts of basilosaurid periotics used in this study. In addition, Mark Uhen produced a cast of the periotic of Z. kochii. Ewan Fordyce, with the University of Otago Department of Geology, donated casts of New Zealand fossil Cetacea. Larry Barnes, Howell Thomas, and Samuel McLeod (Natural History Museum of Los Angeles County), David Bohaska, James Mead, and Charley Potter (National Museum of Natural History, Smithsonian Institution), Ewan Fordyce (Department of Geology, University of Otago), Neville Pledge (South Australian Museum), and Albert E. Sanders (Charleston Museum), all provided access to specimens in their care as well as research and photographic facilities. This research could not have been initiated, conducted, and concluded without the consistent support from Museum Victoria and the Smithsonian Institution. Rodney Start (Museum Victoria) is thanked for producing many of the superb photographs used in this article. I thank Brian Choo for his artwork depicting Ma. colliveri. Financial support for this research was primarily through an Australian Postgraduate Award along with travel funds provided by Monash University, Museum Victoria, and the South Australian Museum. This article stems from my PhD research at Monash University and Museum Victoria. NR 293 TC 47 Z9 48 U1 2 U2 28 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 FEB PY 2010 VL 158 IS 2 BP 367 EP 476 DI 10.1111/j.1096-3642.2009.00572.x PG 110 WC Zoology SC Zoology GA 548IA UT WOS:000273952600006 ER PT J AU Cottrell, E Walter, MJ Walker, D AF Cottrell, Elizabeth Walter, Michael J. Walker, David TI Erratum to Metal-silicate partitioning of tungsten at high pressure and temperature: Implications for equilibrium core formation in Earth (vol 281, pg 275, 2009) SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Correction C1 [Cottrell, Elizabeth] Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. [Walter, Michael J.] Univ Bristol, Dept Earth Sci, Bristol BS8 1RJ, Avon, England. [Walker, David] Columbia Univ, Lamont Doherty Earth Observ, Dept Earth & Environm Sci, Palisades, NY 10964 USA. RP Cottrell, E (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, 10th & Constitut Ave, Washington, DC 20560 USA. EM CottrellE@si.edu NR 1 TC 12 Z9 12 U1 0 U2 7 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0012-821X J9 EARTH PLANET SC LETT JI Earth Planet. Sci. Lett. PD JAN 31 PY 2010 VL 289 IS 3-4 BP 631 EP 634 PG 4 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 553FH UT WOS:000274351000031 ER PT J AU Li, XY Weller, DE Jordan, TE AF Li, Xuyong Weller, Donald E. Jordan, Thomas E. TI Watershed model calibration using multi-objective optimization and multi-site averaging SO JOURNAL OF HYDROLOGY LA English DT Article DE Multi-site averaging; Multi-objective optimization; Watershed model calibration; Parameter estimation; GWLF watershed model; Chesapeake Bay ID RAINFALL-RUNOFF MODELS; CHESAPEAKE BAY; AUTOMATIC CALIBRATION; PARAMETER-ESTIMATION; HYDROLOGIC-MODELS; MULTIPLE OBJECTIVES; GLOBAL OPTIMIZATION; LOADING FUNCTIONS; CLIMATE-CHANGE; STREAM-FLOW AB Recent advances in optimizing watershed model calibration have focused mainly on incorporating multiple objective measures of model performance and improving optimization algorithms. However, some parameters vary widely among different calibration locations. We present a watershed model calibration method that combines multi-objective optimization with averaging across multiple calibration sites. Model parameters were first estimated by multi-objective optimization at each calibration site, and then finalized by weighted averaging the parameter values across sites. The weight for each site was calculated from the prediction error at that site. The calibration framework was applied to estimate 16 hydrological and nutrient parameters of the General Watershed Loading Function (GWLF) watershed model at the Rhode River basin, in Maryland, United States of America. When calibrated to a single watershed, GWLF gave reasonable predictions for monthly streamflow (r(2) = 0.71-0.78), monthly total nitrogen (TN) loads (r(2) = 0.55-0.65), annual streamflow (r(2) = 0.80-0.91), and annual TN loads (r(2) = 0.67-0.86); but success for total phosphorus (TP) loads varied among watersheds (r(2) = 0.41-0.68 for monthly TP loads and r(2) = 0.47-0.79 for annual TP loads). In comparison to the single-site calibrations, the multi-site weighted average approach combined with multi-objective optimization reduced the relative cumulative error of predictions in validation watersheds by 3.5-7.4% for monthly streamflow, 3.2-6.3% for monthly TN loads, and 4.3-5.9% for monthly TP loads, respectively. (C) 2009 Elsevier B.V. All rights reserved. C1 [Li, Xuyong] Chinese Acad Sci, State Key Lab Urban & Reg Ecol, Ecoenvironm Sci Res Ctr, Beijing 100085, Peoples R China. [Li, Xuyong; Weller, Donald E.; Jordan, Thomas E.] Smithsonian Environm Res Ctr, Edgewater, MD 20137 USA. RP Li, XY (reprint author), Chinese Acad Sci, State Key Lab Urban & Reg Ecol, Ecoenvironm Sci Res Ctr, Shuangqing Rd 18, Beijing 100085, Peoples R China. EM lix@si.edu OI Weller, Donald/0000-0002-7629-5437 FU US EPA Science [RD83087801]; Basic Research of China [2009CB421104]; Urban and Regional Ecology Laboratory of Research Center for Eco-Environmental Sciences, Chinese Academy of Sciences [SKLURE2008-1-05] FX This work was initially supported by an award from the US EPA Science To Achieve Results (STAR) Program on Regional-Scale Modeling of Multiple Stressors to Aquatic Ecosystems (Grant No. RD83087801). Additional fund to support the first author was provided by State Key Development Program of Basic Research of China (Grant No. 2009CB421104) and State Key Laboratory Program (Grant No. SKLURE2008-1-05) of Urban and Regional Ecology Laboratory of Research Center for Eco-Environmental Sciences, Chinese Academy of Sciences. NR 51 TC 25 Z9 31 U1 7 U2 36 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-1694 J9 J HYDROL JI J. Hydrol. PD JAN 30 PY 2010 VL 380 IS 3-4 BP 277 EP 288 DI 10.1016/j.jhydrol.2009.11.003 PG 12 WC Engineering, Civil; Geosciences, Multidisciplinary; Water Resources SC Engineering; Geology; Water Resources GA 555GO UT WOS:000274497100004 ER PT J AU Pohl, T Demler, E Lukin, MD AF Pohl, T. Demler, E. Lukin, M. D. TI Dynamical Crystallization in the Dipole Blockade of Ultracold Atoms SO PHYSICAL REVIEW LETTERS LA English DT Article ID RYDBERG BLOCKADE AB We describe a method for controlling many-body states in extended ensembles of Rydberg atoms, forming crystalline structures during laser excitation of a frozen atomic gas. Specifically, we predict the existence of an excitation-number staircase in laser excitation of atomic ensembles into Rydberg states. It is shown that such ordered states can be selectively excited by chirped laser pulses, and, via quantum state transfer from atoms to light, be used to create crystalline photonic states. C1 [Pohl, T.] Max Planck Inst Phys Komplexer Syst, D-01187 Dresden, Germany. [Pohl, T.; Demler, E.; Lukin, M. D.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. [Demler, E.; Lukin, M. D.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. RP Pohl, T (reprint author), Max Planck Inst Phys Komplexer Syst, D-01187 Dresden, Germany. RI Pohl, Thomas/B-5133-2013 FU NSF; Harvard-MIT CUA; DARPA; AFOSR; MURI; Packard Foundation FX This work was supported by NSF, through a grant to ITAMP, by Harvard-MIT CUA, DARPA, NSF, AFOSR, MURI, and the Packard Foundation. NR 24 TC 165 Z9 165 U1 1 U2 9 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 JAN 29 PY 2010 VL 104 IS 4 AR 043002 DI 10.1103/PhysRevLett.104.043002 PG 4 WC Physics, Multidisciplinary SC Physics GA 553AK UT WOS:000274336600016 PM 20366704 ER PT J AU Toledo, M Spangler, PJ Balke, M AF Toledo, Mario Spangler, Paul J. Balke, Michael TI Taxonomic revision of the Neotropical diving beetles genus Laccodytes Regimbart, 1895 (Coleoptera: Dytiscidae) SO ZOOTAXA LA English DT Article DE Coleoptera; Dytiscidae; Laccodytes; running water; strictly lotic; new species ID LACCOPHILINAE COLEOPTERA; PHYLOGENETIC-RELATIONSHIPS; WATER BEETLE; LEACH; MORPHOLOGY AB The Neotropical Laccophilinae genus Laccodytes Regimbart, 1895 is redefined and revised. We recognize ten species, six of which are described as new. We define two species groups: the Laccodytes apalodes-group (L. apalodes Guignot, 1955, L. rondonia sp.n.), and the L. phalacroides-group (L. americanus Peschet, 1919, L. obscuratus sp.n., L. bassignanii sp.n., L. neblinae sp.n., L. olibroides Regimbart, 1895, L. phalacroides Regimbart, 1895, L. takutuanus sp.n., L. androginus sp.n.). Laccophilus pumilio LeConte, 1878, assigned to Laccodytes by Young (1954), belongs to an undescribed genus. Laccodytes species are lotic and most of them inhabit the north-eastern part of South America, apparently with Venezuela and Guyana as centre of diversity. Descriptions, illustrations and SEM photos of habitus, genitals and other diagnostic features are provided for each species, together with habitat notes, when known. We provide a key for species identification. C1 [Toledo, Mario] Univ Parma, Dipartimento Biol Evolutiva & Funz, Museo Storia Nat, I-43100 Parma, Italy. [Spangler, Paul J.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. [Balke, Michael] Nat Hist Museum, Dept Entomol, London SW7 5BD, England. [Balke, Michael] Zool Staatssammlung, D-81247 Munich, Germany. RP Toledo, M (reprint author), Univ Parma, Dipartimento Biol Evolutiva & Funz, Museo Storia Nat, Via Farini 90, I-43100 Parma, Italy. EM mariotoledo@hotmail.it; michael_balke@yahoo.de FU German Science Foundation [BA2152/3-1, BA2152/3-2, BA2152/4-1]; EU union [ES-TAF-193, ES-TAF-2197] FX We wish to thank the Smithsonian Institution for a generous visitor grant to Michael Balke which supported this research in 2000. Thanks to Warren Steiner and the entire staff of the USNM Coleoptera Section for their kind support. Thanks to Manfred Jach and the staff of the NMW Coleoptera Section. Thanks to Lars Hendrich for his help. Thanks to W. Zelenka (Vienna) for the habitus illustration of L. rondonia. Financial support was granted by German Science Foundation DFG BA2152/3-1, 3-2, and 4-1, as well as EU union SYNTHESYS grants ES-TAF-193 and ES-TAF-2197. NR 28 TC 3 Z9 3 U1 1 U2 4 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD JAN 29 PY 2010 IS 2347 BP 37 EP 58 PG 22 WC Zoology SC Zoology GA 550KU UT WOS:000274127500002 ER PT J AU Soderberg, AM Chakraborti, S Pignata, G Chevalier, RA Chandra, P Ray, A Wieringa, MH Copete, A Chaplin, V Connaughton, V Barthelmy, SD Bietenholz, MF Chugai, N Stritzinger, MD Hamuy, M Fransson, C Fox, O Levesque, EM Grindlay, JE Challis, P Foley, RJ Kirshner, RP Milne, PA Torres, MAP AF Soderberg, A. M. Chakraborti, S. Pignata, G. Chevalier, R. A. Chandra, P. Ray, A. Wieringa, M. H. Copete, A. Chaplin, V. Connaughton, V. Barthelmy, S. D. Bietenholz, M. F. Chugai, N. Stritzinger, M. D. Hamuy, M. Fransson, C. Fox, O. Levesque, E. M. Grindlay, J. E. Challis, P. Foley, R. J. Kirshner, R. P. Milne, P. A. Torres, M. A. P. TI A relativistic type Ibc supernova without a detected gamma-ray burst SO NATURE LA English DT Article ID IC SUPERNOVAE; BLAST WAVES; GRB 980425; EMISSION; 1998BW; RATES; ARRAY AB Long duration gamma-ray bursts (GRBs) mark(1) the explosive death of some massive stars and are a rare sub-class of type Ibc supernovae. They are distinguished by the production of an energetic and collimated relativistic outflow powered(2) by a central engine (an accreting black hole or neutron star). Observationally, this outflow is manifested(3) in the pulse of gamma-rays and a long-lived radio afterglow. Until now, central-engine driven supernovae have been discovered exclusively through their gamma-ray emission, yet it is expected(4) that a larger population goes undetected because of limited satellite sensitivity or beaming of the collimated emission away from our line of sight. In this framework, the recovery of undetected GRBs may be possible through radio searches(5,6) for type Ibc supernovae with relativistic outflows. Here we report the discovery of luminous radio emission from the seemingly ordinary type Ibc SN 2009bb, which requires a substantial relativistic outflow powered by a central engine. A comparison with our radio survey of type Ibc supernovae reveals that the fraction harbouring central engines is low, about one per cent, measured independently from, but consistent with, the inferred(7) rate of nearby GRBs. Independently, a second mildly relativistic supernova has been reported(8). C1 [Soderberg, A. M.; Copete, A.; Levesque, E. M.; Grindlay, J. E.; Challis, P.; Foley, R. J.; Kirshner, R. P.; Torres, M. A. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Chakraborti, S.; Ray, A.] Tata Inst Fundamental Res, Mumbai 400005, Maharashtra, India. [Pignata, G.; Hamuy, M.] Univ Chile, Dept Astron, Santiago, Chile. [Chevalier, R. A.; Fox, O.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Chandra, P.] Royal Mil Coll Canada, Kingston, ON K7K 7B4, Canada. [Wieringa, M. H.] CSIRO, Australia Telescope Natl Facil, Epping, NSW 2121, Australia. [Chaplin, V.; Connaughton, V.] Univ Alabama, Huntsville, AL 35899 USA. [Barthelmy, S. D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Bietenholz, M. F.] York Univ, Dept Phys & Astron, Toronto, ON M3J 1P3, Canada. [Bietenholz, M. F.] Hartebeestehoek Radio Observ, ZA-1740 Krugersdorp, South Africa. [Chugai, N.] RAS, Inst Astron, Moscow 119017, Russia. [Stritzinger, M. D.] Carnegie Observ, Las Campanas Observ, La Serena, Chile. [Stritzinger, M. D.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen O, Denmark. [Fransson, C.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden. [Levesque, E. M.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Milne, P. A.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Soderberg, AM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-51, Cambridge, MA 02138 USA. EM asoderberg@cfa.harvard.edu RI Barthelmy, Scott/D-2943-2012; Hamuy, Mario/G-7541-2016 FU NASA; Ford Foundation; NSF; FONDECYT; Iniciativa Cientifica Milenio; FONDAP; CONICYT; 11th Five Year Plan Project FX The VLA is operated by the NRAO, a facility of the NSF operated under cooperative agreement by Associated Universities, Inc. GMRT is run by the National Centre for Radio Astrophysics of the Tata Institute of Fundamental Research. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. A. M. S. and O. F. acknowledge support by NASA through Hubble and GSRP grants, respectively. E. M. L. is funded through a Ford Foundation Predoctoral Fellowship. R. J. F. is a Clay fellow. R. A. C. and R. P. K. acknowledge support through NASA and NSF grants. G. P. and M. H. acknowledge support from FONDECYT, Iniciativa Cientifica Milenio, FONDAP and CONICYT. A. R. and S. C. are funded by an 11th Five Year Plan Project. NR 28 TC 157 Z9 157 U1 0 U2 6 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD JAN 28 PY 2010 VL 463 IS 7280 BP 513 EP 515 DI 10.1038/nature08714 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 548QK UT WOS:000273981100044 PM 20110995 ER PT J AU Lavilla, EO Langone, JA Caramaschi, U Heyer, WR De Sa, RO AF Lavilla, Esteban O. Langone, Jose A. Caramaschi, Ulisses Heyer, W. Ronald De Sa, Rafael O. TI The identification of Rana ocellata Linnaeus, 1758. Nomenclatural impact on the species currently known as Leptodactylus ocellatus (Leptodactylidae) and Osteopilus brunneus (Gosse, 1851) (Hylidae) SO ZOOTAXA LA English DT Review DE Nomenclature; Leptodactylus; Rana; Osteopilus; neotypes ID ANURA AB The usage of the name Rana ocellata Linnaeus, 1758, is plagued by misidentifications and misinterpretations. After an exhaustive bibliographic review, we conclude that the Linnaeus 1758 name refers to Osteopilus brunneus (Gosse, 1851) from Jamaica, while the taxon currently known as Leptodactylus ocellatus corresponds to Rana latrans Steffen, 1815. Herein, we designate and provide descriptions of the neotypes of Leptodactylus latrans ( Steffen, 1815), revalidated, new combination, and Osteopilus ocellatus ( Linnaeus, 1758), new combination, as a senior synonym of Osteopilus brunneus ( Gosse, 1851). C1 [De Sa, Rafael O.] Univ Richmond, Dept Biol, Richmond, VA 23173 USA. [Lavilla, Esteban O.] Fdn Miguel Lillo, RA-4000 San Miguel De Tucuman, Argentina. [Langone, Jose A.] Museo Nacl Hist Nat, Dept Herpetol, Montevideo 11000, Uruguay. [Caramaschi, Ulisses] Univ Fed Rio de Janeiro, Museu Nacl, Dept Vertebrados, Setor Herpetol, BR-20940040 Rio De Janeiro, Brazil. [Heyer, W. Ronald] Smithsonian Inst, Washington, DC 20013 USA. RP De Sa, RO (reprint author), Univ Richmond, Dept Biol, Richmond, VA 23173 USA. EM eolavilla@gmail.com; pplangone@fcien.edu.uy; ulisses@acd.ufrj.br; heyerr@si.edu; rdesa@richmond.edu RI Caramaschi, Ulisses/N-5189-2016 OI Caramaschi, Ulisses/0000-0003-1534-1038 FU Sistema Nacional de Investigadores, Agencia Nacional de Investigacion e Innovacion (ANII), Uruguay; Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq), Brazil; National Science Foundation, USA [0342918] FX We thank Darrel Frost and Alain Dubois for their useful comments on a previous version of this manuscript. Many papers related to Rana ocellata were published in the second half of the 18th Century. EOL thanks the colleagues of AnimalBase Project Group, Gottingen University, and Gallica ( National Library of France) who digitized several of those old books and generously made them available through their respective websites. Kraig Adler (Cornell University, USA), Dione Seripieri (Museu de Zoologia, Universidade de Sao Paulo, SP, Brazil), and Santiago Castroviejo-Fischer and Jose M. Padial (both from Evolutionary Biology Centre, Uppsala University, Sweden) also served as resources of valuable references. Sonia Ziert-Kretzschmar (Fundacion Miguel Lillo, Tucuman, Argentina) translated papers written in gothic German. James R. Poindexter II, Biological Resources Division, United States Geological Service, provided the photos of the neotype of Rana ocellata Linnaeus, 1758. JAL acknowledges financial support from the Sistema Nacional de Investigadores, Agencia Nacional de Investigacion e Innovacion (ANII), Uruguay. UC acknowledges Helianne de Niemeyer and Decio F. de Moraes Jr. for their assistance in fieldwork, Paulo R. Nascimento for the line drawings of the neotype of L. latrans, and the Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq), Brazil, for financial support. RdS and WRH acknowledge support provided by the National Science Foundation (NSF award 0342918.), USA. NR 104 TC 20 Z9 22 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 JAN 28 PY 2010 IS 2346 BP 1 EP 16 PG 16 WC Zoology SC Zoology GA 548SN UT WOS:000273986700001 ER PT J AU Hershler, R Liu, HP AF Hershler, Robert Liu, Hsiu-Ping TI Two new, possibly threatened species of Pyrgulopsis (Gastropoda: Hydrobiidae) from southwestern California SO ZOOTAXA LA English DT Article DE Santa Clara River; Tule River; springsnails; mitochondrial DNA; conservation ID AMERICAN NYMPHOPHILINE GASTROPODS; MITOCHONDRIAL-DNA SEQUENCES; RIVER-BASIN; SPRINGSNAILS GASTROPODA; GENUS PYRGULOPSIS; ASH MEADOWS; SNAILS; RISSOOIDEA; NEVADA; SYSTEM AB Here we describe (for conservation purposes) two new species of Pyrgulopsis from southwestern California based on morphologic and molecular (mtCOI) evidence. Pyrgulopsis castaicensis n. sp. is endemic to a single spring in the upper portion of the Santa Clara River basin and may be threatened by the proposed development of a master-planned community (Newhall Ranch) near Santa Clarita Valley. This snail differs from two morphologically similar regional congeners (P. micrococcus [Pilsbry in Stearns, 1893], P. stearnsiana [Pilsbry, 1899]) by its larger terminal gland, simple oviduct coil and mtCOI sequences (6.1-9.3% for P. micrococcus, 3.5-8.2% for P. stearnsiana). Pyrgulopsis milleri n. sp. is distributed in spring-fed waters along a short reach of upper Tule River drainage and threatened by surface water diversion and its close proximity to a major road (CA 190). Pyrgulopsis milleri differs from closely similar and geographically proximal P. stearnsiana in its broader central cusps on the central radular teeth, shorter pallial section of the albumen gland, greater overlap of the bursa copulatrix by the albumen gland, simple anterior vas deferens, usual absence of a terminal gland and mtCOI sequences (2.8-8.4%). C1 [Hershler, Robert] Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20013 USA. [Liu, Hsiu-Ping] Metropolitan State Coll, Dept Biol, Denver, CO 80217 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; liu.hsiuping@gmail.com FU Smithsonian Institution FX The first author thanks Matt Carpenter (Newhall Land) for permission to sample Middle Canyon Spring and for assistance in the field. Additional collections from this site were provided by Douglas Threloff. We thank Erich Hochberg and Paul Scott for the loan of SBMNH material that was used in this study. Yolanda Villacampa measured shells and prepared scanning electron micrographs. Karolyn Darrow inked the anatomical drawings. The first author's fieldwork was supported, in part, by an award from the Smithsonian Institution's Research Opportunity Fund. This manuscript was improved by comments and corrections provided by Matt Carpenter and two anonymous reviewers. NR 43 TC 5 Z9 6 U1 0 U2 2 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD JAN 25 PY 2010 IS 2343 BP 1 EP 17 PG 17 WC Zoology SC Zoology GA 547IP UT WOS:000273880900001 ER PT J AU Magdis, GE Rigopoulou, D Huang, JS Fazio, GG AF Magdis, G. E. Rigopoulou, D. Huang, J. -S. Fazio, G. G. TI On the stellar masses of IRAC detected Lyman Break Galaxies at z similar to 3 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE Catalogues; galaxies: high-redshift; early Universe ID HUBBLE-DEEP-FIELD; HIGH-REDSHIFT GALAXIES; STAR-FORMING GALAXIES; MASSIVE GALAXIES; SUBMILLIMETER GALAXIES; LUMINOSITY FUNCTION; RED GALAXIES; MIDINFRARED OBSERVATIONS; PHOTOMETRIC PROPERTIES; SPITZER OBSERVATIONS AB We present results of a large survey of the mid-infrared (mid-IR) properties of 248 Lyman Break Galaxies (LBGs) with confirmed spectroscopic redshift using deep Spitzer/Infrared Array Camera (IRAC) observations in six cosmological fields. By combining the new mid-IR photometry with optical and near-infrared observations, we model the spectral energy distributions (SEDs) employing a revised version of the Bruzual and Charlot synthesis population code that incorporates a new treatment of the thermal-pulsating asymptotic giant branch phase (CB07). Our primary aim is to investigate the impact of the AGB phase in the stellar masses of the LBGs, and compare our new results with previous stellar mass estimates. We investigate the stellar mass of the LBG population as a whole and assess the benefits of adding longer wavelengths to estimates of stellar masses for high-redshift galaxies. Based on the new CB07 code, we find that the stellar masses of LBGs are smaller on an average by a factor of similar to 1.4 compared to previous estimates. LBGs with 8 and/or 24 mu m detections show higher masses (M(*) similar to 10(11)M(circle dot)) than LBGs faint in the IRAC bands (M(*) similar to 10(9)M(circle dot)) . The ages of these massive LBGs are considerably higher than the rest of the population, indicating that they have been star forming for at least similar to 1 Gyr. We also show how the addition of the IRAC bands improves the accuracy of the estimated stellar masses and reduced the scatter on the derived mass-to-light ratios. In particular, we present a tight correlation between the 8 mu m IRAC band (rest-frame K for galaxies at z similar to 3) and the stellar mass. We calculate the number density of massive (M(*) > 10(11)M(circle dot)) LBGs and find it to be Phi = (1.12 +/- 0.4) x 10(-5) Mpc(-3), similar to 1.5 times lower than that found by previous studies. Finally, based on ultraviolet-corrected star formation rates (SFRs), we investigate the SFR-stellar mass correlation at z similar to 3, find it similar to the one observed at other redshifts and show that our data place the peak of the evolution of the specific SFR at z similar to 3. C1 [Magdis, G. E.; Rigopoulou, D.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Magdis, G. E.] CEA Saclay, Serv Astrophys, CNRS, F-91191 Gif Sur Yvette, France. [Rigopoulou, D.] Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England. [Huang, J. -S.; Fazio, G. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Magdis, GE (reprint author), Univ Oxford, Dept Phys, Keble Rd, Oxford OX1 3RH, England. EM georgios.magdis@cea.fr RI Magdis, Georgios/C-7295-2014 OI Magdis, Georgios/0000-0002-4872-2294 FU NASA 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. GEM would like to thank S. Charlot for providing the new CB07 code as well as D. Elbaz, H. Aussel and E. Daddi for useful discussions. NR 91 TC 79 Z9 79 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 JAN 21 PY 2010 VL 401 IS 3 BP 1521 EP 1531 DI 10.1111/j.1365-2966.2009.15779.x PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 543DM UT WOS:000273550500010 ER PT J AU Narayanan, D Hayward, CC Cox, TJ Hernquist, L Jonsson, P Younger, JD Groves, B AF Narayanan, Desika Hayward, Christopher C. Cox, Thomas J. Hernquist, Lars Jonsson, Patrik Younger, Joshua D. Groves, Brent TI The formation of high-redshift submillimetre galaxies SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: formation; galaxies: high-redshift; galaxies: interactions; galaxies: ISM; galaxies: starburst; cosmology: theory ID SUPERMASSIVE BLACK-HOLES; PARTICLE HYDRODYNAMICS SIMULATIONS; LUMINOUS INFRARED GALAXIES; INITIAL MASS FUNCTION; DEEP-FIELD-NORTH; STAR-FORMATION; ELLIPTIC GALAXIES; EXTRA LIGHT; COSMOLOGICAL FRAMEWORK; HIERARCHICAL-MODELS AB We describe a model for the formation of z similar to 2 submillimetre galaxies (SMGs) which simultaneously accounts for both average and bright SMGs while providing a reasonable match to their mean observed spectral energy distributions (SEDs). By coupling hydrodynamic simulations of galaxy mergers with the high-resolution 3D polychromatic radiative transfer code SUNRISE, we find that a mass sequence of merger models which use observational constraints as physical input naturally yield objects which exhibit black hole, bulge and H(2) gas masses similar to those observed in SMGs. The dominant drivers behind the 850 mu m flux are the masses of the merging galaxies and the stellar birth cloud covering fraction. The most luminous (S(850) greater than or similar to 15 mJy) sources are recovered by similar to 10(13) M(circle dot) 1:1 major mergers with a birth cloud covering fraction close to unity, whereas more average SMGs (S(850) similar to 5-7 mJy) may be formed in lower mass haloes (similar to 5 x 10(12) M(circle dot)). These models demonstrate the need for high spatial resolution hydrodynamic and radiative transfer simulations in matching both the most luminous sources as well as the full SEDs of SMGs. While these models suggest a natural formation mechanism for SMGs, they do not attempt to match cosmological statistics of galaxy populations; future efforts along this line will help ascertain the robustness of these models. C1 [Hayward, Christopher C.; Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Jonsson, Patrik] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Groves, Brent] Sterrewacht Leiden, NL-2333 CA Leiden, Netherlands. EM dnarayanan@cfa.harvard.edu RI Hayward, Christopher/I-4756-2012 OI Hayward, Christopher/0000-0003-4073-3236 FU W.M. Keck Foundation; National Science Foundation; NASA [HF-51266.01, NAS 5-26555, HST-AR-10678, 10958]; Space Telescope Science Institute; Jet Propulsion Laboratory [30183] FX The authors thank Laura Hainline, Dusan Keres and Mark Swinbank for helpful comments. We thank Laura Hainline for kindly providing Spitzer photometry of SMGs in advance of publication. The simulations in this paper were run on the Odyssey cluster supported by the Harvard FAS Research Computing Group. This project was funded in part by a grant from the W.M. Keck Foundation (TC) and by a Graduate Research Fellowship from the National Science Foundation (CH). JDY acknowledges support provided by 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. PJ was supported by programs HST-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. NR 69 TC 97 Z9 97 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 JAN 21 PY 2010 VL 401 IS 3 BP 1613 EP 1619 DI 10.1111/j.1365-2966.2009.15790.x PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 543DM UT WOS:000273550500018 ER PT J AU Spaandonk, L Steeghs, D Marsh, TR Torres, MAP AF van Spaandonk, L. Steeghs, D. Marsh, T. R. Torres, M. A. P. TI Time-resolved spectroscopy of the pulsating CV GW Lib SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE binaries: spectroscopic; stars: individual: GW Lib; novae, cataclysmic variables ID CATACLYSMIC VARIABLES; WHITE-DWARF; WZ-SAGITTAE; TELESCOPE; BINARIES; SUPEROUTBURST; SPECTROGRAPH; EVOLUTION; MINIMUM; SPECTRA AB We present time-resolved optical spectroscopy of the dwarf nova GW Librae during its rare 2007 April superoutburst and compare these with quiescent epochs. The data provide the first opportunity to track the evolution of the principal spectral features. In the early stages of the outburst, the optically thick disc dominates the optical and the line components show clear orbital radial velocity excursions. In the course of several weeks, optically thin regions become more prominent as strong emission lines replace the broad disc absorption. Post-outburst spectroscopy covering the I band illustrates the advantages of Ca II relative to the commonly used Balmer lines when attempting to constrain binary parameters. Due to the lower ionization energy combined with smaller thermal and shear broadening of these lines, a sharp emission component is seen to be moving in between the accretion disc peaks in the Ca II line. No such component is visible in the Balmer lines. We interpret this as an emission component originating on the hitherto unseen mass donor star. This emission component has a mean velocity of similar to -15 +/- 5 km s(-1) which is associated with the systemic velocity., and a velocity semi-amplitude of K(em) = 82.2 +/- 4.9 km s(-1). Doppler tomography reveals an asymmetric accretion disc, with the S-wave mapping to a sharp spot in the tomogram with a velocity consistent to what is obtained with line profile fitting. A centre of symmetry analysis of the disc component suggests a very small value for the WD orbital velocity K(1) as is also inferred from double Gaussian fits to the spectral lines. While our conservative dynamical limits place a hard upper limit on the binary mass ratio of q < 0.23, we favour a significantly lower value near q similar to 0.06. Pulsation modelling suggests a white dwarf mass similar to 1 M(circle dot). This, paired with a low-mass donor, near the empirical sequence of an evolved cataclysmic variable close to the period bounce, appears to be consistent with all the observational constraints to date. C1 [van Spaandonk, L.; Steeghs, D.; Marsh, T. R.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Steeghs, D.; Torres, M. A. P.] Harvard Smithsonian Astrophys, Cambridge, MA 02138 USA. RP Spaandonk, L (reprint author), Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. EM L.van-Spaandonk@warwick.ac.uk RI Steeghs, Danny/C-5468-2009 OI Steeghs, Danny/0000-0003-0771-4746 FU STFC FX We acknowledge with thanks the variable star observations from the AAVSO International Data base contributed by observers worldwide and used in this research. DS acknowledges a STFC Advanced Fellowship. We thank Perry Berlind and Mike Calkins for their assistance with obtaining the FWLO/FAST target of opportunity spectroscopy. The WHT is operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. This paper includes data gathered with the 6.5-m Magellan Telescopes located at Las Campanas Observatory, Chile operated by the Carnegie Institution of Washington and the 1.6-m TT located at the Fred Lawrence Whipple Observatory operated by the Smithsonian Astrophysical Observatory. NR 41 TC 11 Z9 11 U1 0 U2 5 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 JAN 21 PY 2010 VL 401 IS 3 BP 1857 EP 1868 DI 10.1111/j.1365-2966.2009.15762.x PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 543DM UT WOS:000273550500036 ER PT J AU Leauthaud, A Finoguenov, A Kneib, JP Taylor, JE Massey, R Rhodes, J Ilbert, O Bundy, K Tinker, J George, MR Capak, P Koekemoer, AM Johnston, DE Zhang, YY Cappelluti, N Ellis, RS Elvis, M Giodini, S Heymans, C Le Fevre, O Lilly, S McCracken, HJ Mellier, Y Refregier, A Salvato, M Scoville, N Smoot, G Tanaka, M Van Waerbeke, L Wolk, M AF Leauthaud, Alexie Finoguenov, Alexis Kneib, Jean-Paul Taylor, James E. Massey, Richard Rhodes, Jason Ilbert, Olivier Bundy, Kevin Tinker, Jeremy George, Matthew R. Capak, Peter Koekemoer, Anton M. Johnston, David E. Zhang, Yu-Ying Cappelluti, Nico Ellis, Richard S. Elvis, Martin Giodini, Stefania Heymans, Catherine Le Fevre, Oliver Lilly, Simon McCracken, Henry J. Mellier, Yannick Refregier, Alexandre Salvato, Mara Scoville, Nick Smoot, George Tanaka, Masayuki Van Waerbeke, Ludovic Wolk, Melody TI A WEAK LENSING STUDY OF X-RAY GROUPS IN THE COSMOS SURVEY: FORM AND EVOLUTION OF THE MASS-LUMINOSITY RELATION SO ASTROPHYSICAL JOURNAL LA English DT Review DE cosmology: observations; gravitational lensing; large-scale structure of universe ID HUBBLE-SPACE-TELESCOPE; GALAXY CLUSTER SURVEY; DIGITAL SKY SURVEY; DARK-MATTER HALOS; WIDE-FIELD SURVEY; SCALING RELATIONS; COSMOLOGICAL PARAMETERS; PHOTOMETRIC REDSHIFTS; ADVANCED CAMERA; SOURCE CATALOG AB Measurements of X-ray scaling laws are critical for improving cosmological constraints derived with the halo mass function and for understanding the physical processes that govern the heating and cooling of the intracluster medium. In this paper, we use a sample of 206 X-ray-selected galaxy groups to investigate the scaling relation between X-ray luminosity (L(X)) and halo mass (M(200)) where M(200) is derived via stacked weak gravitational lensing. This work draws upon a broad array of multi-wavelength COSMOS observations including 1.64 degrees(2) of contiguous imaging with the Advanced Camera for Surveys to a limiting magnitude of I(F814W) = 26.5 and deep XMM-Newton/Chandra imaging to a limiting flux of 1.0 x 10(-15) erg cm(-2) s(-1) in the 0.5-2 keV band. The combined depth of these two data sets allows us to probe the lensing signals of X-ray-detected structures at both higher redshifts and lower masses than previously explored. Weak lensing profiles and halo masses are derived for nine sub-samples, narrowly binned in luminosity and redshift. The COSMOS data alone are well fit by a power law, M(200) alpha (L(X))(alpha), with a slope of alpha = 0.66 +/- 0.14. These results significantly extend the dynamic range for which the halo masses of X-ray-selected structures have been measured with weak gravitational lensing. As a result, tight constraints are obtained for the slope of the M-L(X) relation. The combination of our group data with previously published cluster data demonstrates that the M-L(X) relation is well described by a single power law, a = 0.64 +/- 0.03, over two decades in mass, M(200) similar to 10(13.5)-10(15.5) h(72)(-1) M(circle dot). These results are inconsistent at the 3.7 sigma level with the self-similar prediction of alpha = 0.75. We examine the redshift dependence of the M-L(X) relation and find little evidence for evolution beyond the rate predicted by self-similarity from z similar to 0.25 to z similar to 0.8. C1 [Leauthaud, Alexie] Univ Calif Berkeley, Lawrence Berkeley Lab, Berkeley, CA 94720 USA. [Leauthaud, Alexie; Tinker, Jeremy; Smoot, George] Univ Calif Berkeley, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA. [Finoguenov, Alexis; Cappelluti, Nico; Giodini, Stefania] Max Planck Inst Extraterr Phys, D-85748 Munich, Germany. [Finoguenov, Alexis] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA. [Kneib, Jean-Paul; Ilbert, Olivier; Le Fevre, Oliver] Univ Aix Marseille, CNRS, LAM, F-13013 Marseille, France. [Taylor, James E.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [Massey, Richard; Heymans, Catherine] Astron Inst, Edinburgh EH9 3HJ, Midlothian, Scotland. [Rhodes, Jason] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Rhodes, Jason; Ellis, Richard S.; Salvato, Mara; Scoville, Nick] CALTECH, Pasadena, CA 91125 USA. [Bundy, Kevin; George, Matthew R.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Capak, Peter] Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Koekemoer, Anton M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Johnston, David E.] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. [Zhang, Yu-Ying] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany. [Elvis, Martin] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lilly, Simon] ETH, Inst Astron, Dept Phys, CH-8093 Zurich, Switzerland. [McCracken, Henry J.; Mellier, Yannick] Inst Astrophys, UMR 7095, F-75014 Paris, France. [Refregier, Alexandre] CEA Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France. [Salvato, Mara] IPP Max Planck Inst Plasma Phys, D-85748 Garching, Germany. [Tanaka, Masayuki] European So Observ, D-85748 Garching, Germany. [Van Waerbeke, Ludovic] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Wolk, Melody] Ecole Normale Super, F-94235 Cachan, France. RP Leauthaud, A (reprint author), Univ Calif Berkeley, Lawrence Berkeley Lab, 1 Cyclotron Rd, Berkeley, CA 94720 USA. EM asleauthaud@lbl.gov RI Le Fevre, Olivier/G-7389-2011; Kneib, Jean-Paul/A-7919-2015; OI Kneib, Jean-Paul/0000-0002-4616-4989; Cappelluti, Nico/0000-0002-1697-186X; Koekemoer, Anton/0000-0002-6610-2048 FU NASA [NAS 5-26555]; ESA Member States; European Southern Observatory [175.A-0839]; Association of Universities forResearch in Astronomy, Inc. (AURA); National Science Foundation; National Radio Astronomy Observatory; Associated Universities, Inc; CEA/DAPNIA; National Research Council of Canada; Canadian Astronomy Data Centre; Centre National de la Recherche Scientifique de France; TERAPIX; University of Hawaii 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; Kitt Peak National Observatory, Cerro Tololo Inter-American Observatory, and the National Optical Astronomy Observatory, which are operated by the Association of Universities forResearch in Astronomy, Inc. (AURA) under cooperative agreement with the National Science Foundation; the National Radio Astronomy Observatory which is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc; and the Canada-France-Hawaii Telescope with MegaPrime/MegaCam operated as a joint project by the Canada-France-Hawaii-Telescope 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. NR 112 TC 149 Z9 151 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 JAN 20 PY 2010 VL 709 IS 1 BP 97 EP 114 DI 10.1088/0004-637X/709/1/97 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 539TY UT WOS:000273282500010 ER PT J AU Marengo, M Evans, NR Barmby, P Bono, G Welch, DL Romaniello, M AF Marengo, M. Evans, N. R. Barmby, P. Bono, G. Welch, D. L. Romaniello, M. TI GALACTIC CEPHEIDS WITH SPITZER. I. LEAVITT LAW AND COLORS SO ASTROPHYSICAL JOURNAL LA English DT Article DE distance scale; infrared: stars; stars: mass-loss; stars: variables: Cepheids ID PERIOD-LUMINOSITY RELATION; HUBBLE-SPACE-TELESCOPE; LARGE-MAGELLANIC-CLOUD; INFRARED ARRAY CAMERA; MULTIBAND IMAGING PHOTOMETER; BAADE-WESSELINK METHOD; CLASSICAL CEPHEIDS; MASS-LOSS; EXTENDED ENVELOPES; HORIZONTAL-BRANCH AB Classical Cepheid variable stars have been important indicators of extragalactic distance and Galactic evolution for over a century. The Spitzer Space Telescope has opened the possibility of extending the study of Cepheids into the mid- and far-infrared, where interstellar extinction is reduced. We have obtained photometry from images of a sample of Galactic Cepheids with the Infrared Array Camera (IRAC) and Multiband Infrared Photometer for Spitzer instruments on Spitzer. Here we present the first mid- infrared period-luminosity relations for Classical Cepheids in the Galaxy, and the first ever Cepheid period-luminosity relations at 24 and 70 mu m. We compare these relations with theoretical predictions, and with period-luminosity relations obtained in recent studies of the Large Magellanic Cloud. We find a significant period-color relation for the [3.6] - [8.0] IRAC color. Other mid- infrared colors for both Cepheids and non-variable supergiants are strongly affected by variable molecular spectral features, in particular deep CO absorption bands. We do not find strong evidence for mid-infrared excess caused by warm (similar to 500 K) circumstellar dust. We discuss the possibility that recent detections with near-infrared interferometers of circumstellar shells around delta Cep, l Car, Polaris, Y Oph, and RS Pup may be a signature of shocked gas emission in a dust-poor wind associated with pulsation-driven mass loss. C1 [Marengo, M.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Marengo, M.; Evans, N. R.; Barmby, P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Barmby, P.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [Bono, G.] Univ Roma Tor Vergata, Dept Phys, I-00133 Rome, Italy. [Bono, G.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy. [Welch, D. L.] McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1, Canada. [Romaniello, M.] European So Observ, D-85748 Garching, Germany. RP Marengo, M (reprint author), Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. RI Barmby, Pauline/I-7194-2016 OI Barmby, Pauline/0000-0003-2767-0090 FU NASA [1407]; Natural Sciences and Engineering Research Council of Canada; Chandra X-Ray Center [NAS8-03060] 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 NASA contract 1407. P. B. and D. W. both acknowledge research support through Discovery Grants from the Natural Sciences and Engineering Research Council of Canada. N. R. E. acknowledges support from the Chandra X-Ray Center grant NAS8-03060. We thank Robert Kurucz and Chow-Choong Ngeow for helpful discussions during the preparation of this manuscript. We also acknowledge M. Marconi, P. G. Prada Moroni, and M. Cignoni for sending us the predicted Cepheid PL relations in advance of publication. NR 89 TC 35 Z9 35 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2010 VL 709 IS 1 BP 120 EP 134 DI 10.1088/0004-637X/709/1/120 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 539TY UT WOS:000273282500012 ER PT J AU Knudsen, KK Kneib, JP Richard, J Petitpas, G Egami, E AF Knudsen, Kirsten K. Kneib, Jean-Paul Richard, Johan Petitpas, Glen Egami, Eiichi TI PHYSICAL PROPERTIES AND MORPHOLOGY OF A NEWLY IDENTIFIED COMPACT z=4.04 LENSED SUBMILLIMETER GALAXY IN ABELL 2218 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: high-redshift; galaxies: individual (SMM J163556+661300); submillimeter: galaxies ID SPECTRAL ENERGY-DISTRIBUTIONS; MASSIVE DISK GALAXIES; SIMILAR-TO 2.5; DEEP-FIELD; NUMBER COUNTS; MOLECULAR GAS; HIGH-REDSHIFT; GOODS 850-5; PHOTOMETRIC REDSHIFTS; SOURCE EXTRACTION AB We present the identification of a bright submillimeter (submm) source, SMM J163555.5+661300, detected in the lensing cluster Abell 2218, for which we have accurately determined the position using observations from the Submillimeter Array (SMA). The identified optical counterpart has a spectroscopic redshift of z = 4.044+/-0.001 if we attribute the single emission line detected at lambda = 6140 angstrom to Ly alpha. This redshift identification is in good agreement with the optical/near-infrared photometric redshift as well as the submm flux ratio S(450)/S(850) similar to 1.6, the radio-submm flux ratio S(1.4)/S(850) < 0.004, and the 24 mu m to 850 mu m flux ratio S(24)/S(850) < 0.005. Correcting for the gravitational lensing amplification of similar to 5.5, we find that the source has a far-infrared luminosity of 1.3x10(12) L(circle dot), which implies a star formation rate (SFR) of 230 M(circle dot) yr(-1). This makes it the lowest-luminosity submillimeter galaxy (SMG) known at z > 4 to date. Previous CO(4-3) emission line observations yielded a non-detection, for which we derived an upper limit of the CO line luminosity of L'(CO) = 0.3 x 10(10) K km s(-1) pc(-2), which is not inconsistent with the L'(CO)-L(FIR) relation for starburst galaxies. The best-fit model to the optical and near-infrared photometry give a stellar population with an age of 1.4 Gyr and a stellar mass of 1.6x10(10) M(circle dot). The optical morphology is compact and in the source plane the galaxy has an extent of similar to 6x3 kpc with individual star-forming knots of <500 pc in size. J163556 is not resolved in the SMA data, and we place a strict upper limit on the size of the starburst region of 8 kpc x 3 kpc, which implies a lower limit on the SFR surface density of 12 M(circle dot) yr(-1) kpc(2). The redshift of J163556 extends the redshift distribution of faint, lensed SMGs, and we find no evidence that these have a different redshift distribution than bright SMGs. C1 [Knudsen, Kirsten K.] Argelander Inst Astron, D-53121 Bonn, Germany. [Kneib, Jean-Paul] Univ Aix Marseille, OAMP, Lab Astrophys Marseille, F-13388 Marseille 13, France. [Kneib, Jean-Paul] CNRS, F-13388 Marseille 13, France. [Kneib, Jean-Paul; Richard, Johan] CALTECH, Pasadena, CA 91125 USA. [Richard, Johan] Univ Durham, Dept Phys & Astron, Durham DH3 1LE, England. [Petitpas, Glen] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Egami, Eiichi] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Knudsen, KK (reprint author), Argelander Inst Astron, Hugel 71, D-53121 Bonn, Germany. EM knudsen@astro.uni-bonn.de RI Kneib, Jean-Paul/A-7919-2015; OI Kneib, Jean-Paul/0000-0002-4616-4989; Knudsen, Kirsten Kraiberg/0000-0002-7821-8873 FU NASA [NAS 5-26555]; Smithsonian Institution; Academia Sinica; Deutsche Forschungsgemeinschaft (DFG) [1177]; CNRS; EU FX We thank an anonymous referee for insightful comments, which help improve the manuscript. 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. This program is 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 NAS 5-26555, the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan, the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. We thank Federica Govoni and Marie Machacek for providing the Chandra X-ray upper limit. K. K. acknowledges support from the Deutsche Forschungsgemeinschaft (DFG) Priority Programme 1177. J.P.K. thanks CNRS for support. J.R. acknowledges support from a EU Marie-Curie fellowship. NR 60 TC 34 Z9 34 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 JAN 20 PY 2010 VL 709 IS 1 BP 210 EP 217 DI 10.1088/0004-637X/709/1/210 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 539TY UT WOS:000273282500019 ER PT J AU Bogdanov, S van den Berg, M Heinke, CO Cohn, HN Lugger, PM Grindlay, JE AF Bogdanov, Slavko van den Berg, Maureen Heinke, Craig O. Cohn, Haldan N. Lugger, Phyllis M. Grindlay, Jonathan E. TI A CHANDRA X-RAY OBSERVATORY STUDY OF PSR J1740-5340 AND CANDIDATE MILLISECOND PULSARS IN THE GLOBULAR CLUSTER NGC 6397 SO ASTROPHYSICAL JOURNAL LA English DT Article DE globular clusters: general; globular clusters: individual (NGC 6397); pulsars: general; pulsars: individual (PSR J1740-5340); stars: neutron; X-rays: stars ID COUNTING DETECTOR IMAGES; XMM-NEWTON; GLOBULAR-CLUSTER-47 TUCANAE; DYNAMICAL FORMATION; WAVELET TRANSFORMS; SAX J1808.4-3658; NGC-6397; BINARY; EMISSION; COMPANION AB We present a deep Chandra X-ray Observatory study of the peculiar binary radio millisecond pulsar (MSP) PSR J1740-5340 and candidate millisecond pulsars in the globular cluster NGC 6397. The X-rays from PSR J1740-5340 appear to be non-thermal and exhibit variability at the binary period. These properties suggest the presence of a relativistic intrabinary shock formed due to interaction of a relativistic rotation-powered pulsar wind and outflow from the unusual "red-straggler/sub-subgiant" companion. We find the X-ray source U18 to show similar X-ray and optical properties to those of PSR J1740-5340, making it a strong MSP candidate. It exhibits variability on timescales from hours to years, also consistent with an intrabinary shock origin of its X-ray emission. The unprecedented depth of the X-ray data allows us to conduct a complete census of MSPs in NGC 6397. Based on the properties of the present sample of X-ray-detected MSPs in the Galaxy, we find that NGC6397 probably hosts no more than six MSPs. C1 [Bogdanov, Slavko] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [van den Berg, Maureen; Grindlay, Jonathan E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Heinke, Craig O.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2G7, Canada. [Lugger, Phyllis M.; Grindlay, Jonathan E.] Indiana Univ, Dept Astron, Bloomington, IN 47405 USA. RP Bogdanov, S (reprint author), McGill Univ, Dept Phys, 3600 Univ St, Montreal, PQ H3A 2T8, Canada. EM bogdanov@physics.mcgill.ca OI Bogdanov, Slavko/0000-0002-9870-2742; Heinke, Craig/0000-0003-3944-6109 FU NASA [GO78033A]; Canadian Institute for Advanced Research Junior Fellowship FX This work was funded in part by NASA Chandra grant GO78033A, awarded through the Harvard College Observatory. S. B. is supported in part by a Canadian Institute for Advanced Research Junior Fellowship. The research in this paper has made use of the NASA Astrophysics Data System (ADS). NR 58 TC 29 Z9 29 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 JAN 20 PY 2010 VL 709 IS 1 BP 241 EP 250 DI 10.1088/0004-637X/709/1/241 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 539TY UT WOS:000273282500021 ER PT J AU Berger, E Basri, G Fleming, TA Giampapa, MS Gizis, JE Liebert, J Martin, E Phan-Bao, N Rutledge, RE AF Berger, E. Basri, G. Fleming, T. A. Giampapa, M. S. Gizis, J. E. Liebert, J. Martin, E. Phan-Bao, N. Rutledge, R. E. TI SIMULTANEOUS MULTI-WAVELENGTH OBSERVATIONS OF MAGNETIC ACTIVITY IN ULTRACOOL DWARFS. III. X-RAY, RADIO, AND H alpha ACTIVITY TRENDS IN M AND L DWARFS SO ASTROPHYSICAL JOURNAL LA English DT Article DE brown dwarfs; radio continuum: stars; stars: activity; stars: low-mass; stars: magnetic fields ID LOW-MASS STARS; MAIN-SEQUENCE; BROWN DWARF; SOLAR NEIGHBORHOOD; ROSAT SURVEY; COOL STARS; MID-M; EMISSION; ROTATION; FLARE AB As part of our on-going investigation into the magnetic field properties of ultracool dwarfs, we present simultaneous radio, X-ray, and H alpha observations of three M9.5-L2.5 dwarfs (BRI 0021-0214, LSR 060230.4+391059, and 2MASS J052338.2-140302). We do not detect X-ray or radio emission from any of the three sources, despite previous detections of radio emission from BRI 0021 and 2M0523-14. Steady and variable H alpha emission are detected from 2M0523-14 and BRI 0021, respectively, while no H alpha emission is detected from LSR 0602+39. Overall, our survey of nine M8-L5 dwarfs doubles the number of ultracool dwarfs observed in X-rays, and triples the number of L dwarfs, providing in addition the deepest limits to date, log (L-X/L-bol) less than or similar to -5. With this larger sample we find the first clear evidence for a substantial reduction in X-ray activity, by about two orders of magnitude, from mid-M to mid-L dwarfs. We find that the decline in H alpha roughly follows LH alpha/L-bol proportional to 10(-0.4x(SP-6)) for SP >= 6, where SP = 0 for spectral type M0. In the radio band, however, the luminosity remains relatively unchanged from M0 to L4, leading to a substantial increase in L-rad/L-bol. Our survey also provides the first comprehensive set of simultaneous radio/X-ray/H alpha observations of ultracool dwarfs, and reveals a clear breakdown of the radio/X-ray correlation beyond spectral type M7, evolving smoothly from L-nu,L-rad/L-X approximate to 10(-15.5) to similar to 10(-11.5) Hz(-1) over the narrow spectral-type range M7-M9. This breakdown reflects the substantial reduction in X-ray activity beyond M7, but its physical origin remains unclear since, as evidenced by the uniform radio emission, there is no drop in the field dissipation and particle acceleration efficiency. Based on the results of our survey, we conclude that a further investigation of magnetic activity in ultracool dwarfs will benefit from a two-pronged approach: multi-rotation observations of nearby known active sources and a snapshot survey of a large sample within similar to 50 pc to uncover rare flaring objects. C1 [Berger, E.] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Basri, G.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Fleming, T. A.; Liebert, J.] Univ Arizona, Dept Astron & Steward Observ, Tucson, AZ 85721 USA. [Giampapa, M. S.] Natl Opt Astron Observ, Natl Solar Observ, Tucson, AZ 85726 USA. [Gizis, J. E.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Martin, E.] Inst Astrofis Canarias, Tenerife, Spain. [Martin, E.] Univ Cent Florida, Dept Phys, Orlando, FL 32816 USA. [Phan-Bao, N.] Vietnam Natl Univ, HCMIU, Dept Phys, Ho Chi Minh City, Vietnam. [Rutledge, R. E.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. RP Berger, E (reprint author), Harvard Univ, Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU National Science Foundation (United States); Science and Technology Facilities Council (United Kingdom); National Research Council (Canada); CONICYT (Chile); Australian Research Council (Australia); CNPq (Brazil); CONICET (Argentina); National Aeronautics and Space Administration [G08-9013A]; National Aeronautics Space Administration [NAS8-03060] FX We thank the Chandra, Gemini, and VLA schedulers for their invaluable help in coordinating these observations. We also thank the referee, Dr. Alexander Brown, for helpful suggestions and comments that improved the quality of the manuscript. This work has made use of the SIMBAD database, operated at CDS, Strasbourg, France. It is based in part on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the Science and Technology Facilities Council (United Kingdom), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), CNPq (Brazil) and CONICET (Argentina). Support for this work was provided by the National Aeronautics and Space Administration through Chandra Award Number G08-9013A issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060. NR 51 TC 69 Z9 69 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2010 VL 709 IS 1 BP 332 EP 341 DI 10.1088/0004-637X/709/1/332 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 539TY UT WOS:000273282500030 ER PT J AU Birzan, L McNamara, BR Nulsen, PEJ Carilli, CL Wise, MW AF Birzan, L. McNamara, B. R. Nulsen, P. E. J. Carilli, C. L. Wise, M. W. TI RADIATIVE EFFICIENCY AND CONTENT OF EXTRAGALACTIC RADIO SOURCES: TOWARD A UNIVERSAL SCALING RELATION BETWEEN JET POWER AND RADIO POWER (vol 686, 859, 2008) SO ASTROPHYSICAL JOURNAL LA English DT Correction C1 [Birzan, L.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Birzan, L.] Ohio Univ, Dept Phys & Astron, Clippinger Labs, Athens, OH 45701 USA. [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.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Carilli, C. L.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Wise, M. W.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. RP Birzan, L (reprint author), Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. NR 1 TC 3 Z9 3 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 JAN 20 PY 2010 VL 709 IS 1 BP 546 EP 546 DI 10.1088/0004-637X/709/1/546 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 539TY UT WOS:000273282500050 ER PT J AU Lee, JE Lee, HG Shinn, JH Dunham, MM Kim, IS Kim, CH Bourke, TL Evans, NJ Choi, Y AF Lee, Jeong-Eun Lee, Ho-Gyu Shinn, Jong-Ho Dunham, Michael M. Kim, Il-Suk Kim, Chang Hee Bourke, Tyler L. Evans, Neal J. Choi, Yunhee TI THE SPITZER c2d SURVEY OF NEARBY DENSE CORES: JET AND MOLECULAR OUTFLOW ASSOCIATED WITH A YOUNG STELLAR OBJECT IN CORE A OF L1251 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE ISM: individual objects (L1251); stars: formation ID ARRAY CAMERA IRAC; STAR-FORMATION; SPACE-TELESCOPE; SMALL CLOUDS; LUMINOSITY; H-2; PROTOSTARS; EVOLUTION; HYDROGEN; SHOCKS AB A long infrared jet has been discovered by the Spitzer c2d Legacy Program in core A of L1251. It is associated with a very embedded Class 0 object with an accretion luminosity of about 0.9 L(circle dot) derived by radiative transfer model fitting to the observed spectral energy distribution. Comparing the observed Infrared Array Camera colors along the infrared jet with those calculated from a model of an admixture of gas with a power-law temperature distribution indicates that the jet is possibly created by a paraboloidal bow shock propagating into the ambient medium of n(H(2)) = 10(5) cm(-3). In addition, the variation of the power-law index along the jet suggests that the portion of hot gas decreases with distance from the jet engine. The molecular outflow in this region has been mapped for the first time using CO data. From the calculated outflow momentum flux, a very strong lower limit to the average accretion luminosity is 3.6 sin i/cos(3) i L(circle dot), indicative of a decrease in the accretion rate with time. C1 [Lee, Jeong-Eun; Kim, Il-Suk; Choi, Yunhee] Sejong Univ, Dept Astron & Space Sci, Astrophys Res Ctr Struct & Evolut Cosmos, Seoul 143747, South Korea. [Lee, Ho-Gyu] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Shinn, Jong-Ho] Korea Astron & Space Sci Inst, Taejon 305348, South Korea. [Dunham, Michael M.; Evans, Neal J.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Kim, Chang Hee] Seoul Natl Univ, Dept Phys & Astron, Seoul 151747, South Korea. [Bourke, Tyler L.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Lee, JE (reprint author), Sejong Univ, Dept Astron & Space Sci, Astrophys Res Ctr Struct & Evolut Cosmos, Seoul 143747, South Korea. EM jelee@sejong.ac.kr; tohogyu@gmail.com; mdunham@astro.as.utexas.edu; tbourke@cfa.harvard.edu; nje@astro.as.utexas.edu RI Shinn, Jong-Ho/B-8889-2009; Lee , Jeong-Eun/E-2387-2013 OI Shinn, Jong-Ho/0000-0001-7967-6473; FU Korean government (MEST) [2009-0062865]; NRF [R01-2007-000-20336-0]; NASA [1407, 1224608] FX We acknowledge the support by the National Research Foundation of Korea (NRF) grant funded by the Korean government (MEST) (No. 2009-0062865). This work was also supported in part by a grant (R01-2007-000-20336-0) from the Basic Research Program of the NRF. Support for this work, part of the Spitzer Legacy Science Program, was provided by NASA through contract 1224608 issued by the Jet Propulsion Laboratory, California Institute of Technology, under NASA contract 1407. NR 35 TC 13 Z9 13 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 JAN 20 PY 2010 VL 709 IS 1 BP L74 EP L78 DI 10.1088/2041-8205/709/1/L74 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 540DC UT WOS:000273310000015 ER PT J AU Levesque, EM Soderberg, AM Foley, RJ Berger, E Kewley, LJ Chakraborti, S Ray, A Torres, MAP Challis, P Kirshner, RP Barthelmy, SD Bietenholz, MF Chandra, P Chaplin, V Chevalier, RA Chugai, N Connaughton, V Copete, A Fox, O Fransson, C Grindlay, JE Hamuy, MA Milne, PA Pignata, G Stritzinger, MD Wieringa, MH AF Levesque, E. M. Soderberg, A. M. Foley, R. J. Berger, E. Kewley, L. J. Chakraborti, S. Ray, A. Torres, M. A. P. Challis, P. Kirshner, R. P. Barthelmy, S. D. Bietenholz, M. F. Chandra, P. Chaplin, V. Chevalier, R. A. Chugai, N. Connaughton, V. Copete, A. Fox, O. Fransson, C. Grindlay, J. E. Hamuy, M. A. Milne, P. A. Pignata, G. Stritzinger, M. D. Wieringa, M. H. TI THE HIGH-METALLICITY EXPLOSION ENVIRONMENT OF THE RELATIVISTIC SUPERNOVA 2009bb SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: ISM; gamma rays: bursts: general; supernovae: individual (SN 2009bb) ID GAMMA-RAY BURSTS; STAR-FORMING GALAXIES; MASSIVE STARS; STARBURST GALAXIES; HOST GALAXIES; WOLF-RAYET; EMISSION; RADIO; CLASSIFICATION; PROGENITORS AB We investigate the environment of the nearby (d approximate to 40 Mpc) broad-lined Type Ic supernova (SN) 2009bb. This event was observed to produce a relativistic outflow likely powered by a central accreting compact object. While such a phenomenon was previously observed only in long-duration gamma-ray bursts (LGRBs), no LGRB was detected in association with SN 2009bb. Using an optical spectrum of the SN 2009bb explosion site, we determine a variety of interstellar medium properties for the host environment, including metallicity, young stellar population age, and star formation rate. We compare the SN explosion site properties to observations of LGRB and broad-lined SN Ic host environments on optical emission line ratio diagnostic diagrams. Based on these analyses, we find that the SN 2009bb explosion site has a metallicity between 1.7 Z(circle dot) and 3.5 Z(circle dot), in agreement with other broad-lined SN Ic host environments and at odds with the low-redshift LGRB host environments and recently proposed maximum metallicity limits for relativistic explosions. We consider the implications of these findings and the impact that SN 2009bb's unusual explosive properties and environment have on our understanding of the key physical ingredient that enables some SNe to produce a relativistic outflow. C1 [Levesque, E. M.; Kewley, L. J.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Levesque, E. M.; Soderberg, A. M.; Foley, R. J.; Berger, E.; Torres, M. A. P.; Challis, P.; Kirshner, R. P.; Copete, A.; Grindlay, J. E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Chakraborti, S.; Ray, A.] Tata Inst Fundamental Res, Bombay 400005, Maharashtra, India. [Barthelmy, S. D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Bietenholz, M. F.] York Univ, Dept Phys & Astron, Toronto, ON M3J 1P3, Canada. [Bietenholz, M. F.] Hartebeestehoek Radio Observ, ZA-1740 Krugersdorp, South Africa. [Chandra, P.] Royal Mil Coll Canada, Kingston, ON K7K 784, Canada. [Chaplin, V.; Connaughton, V.] Univ Alabama, Huntsville, AL 35899 USA. [Chevalier, R. A.; Fox, O.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Chugai, N.] RAS, Inst Astron, Moscow 119017, Russia. [Fransson, C.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden. [Hamuy, M. A.; Pignata, G.] Univ Chile, Dept Astron, Santiago, Chile. [Milne, P. A.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Pignata, G.] Univ Andres Bello, Dept Ciencias Fis, Santiago, Chile. [Stritzinger, M. D.] Carnegie Observ, Las Campanas Observ, La Serena, Chile. [Stritzinger, M. D.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. [Wieringa, M. H.] CSIRO, Australia Telescope Natl Facil, Epping, NSW 2121, Australia. RP Levesque, EM (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. EM emsque@ifa.hawaii.edu RI Barthelmy, Scott/D-2943-2012; Hamuy, Mario/G-7541-2016 FU National Aeronautics and Space Administration; National Science Foundation; Ford Foundation; NSF EARLY CAREER AWARD [AST07-48559]; NASA; 11th Five Year Plan [11P-409]; NSF; Millennium Center for Supernova Science [P06-045-F]; Comite Mixto ESO-Gobierno de Chile; Centro de Astrofisica FONDAP [15010003]; Center of Excellence in Astrophysics and Associated Technologies [PFB 06]; Proyectos Fondecyt [1060808, 1109421] FX We gratefully acknowledge the hospitality and assistance of the staff at Las Campanas Observatory in Chile. GMRT is run by the National Centre for Radio Astrophysics of the Tata Institute of Fundamental Research. This work made use of the Central Bureau for Astronomical Telegrams. We also include data from the Two Micron All Sky Survey (2MASS), which is a joint project of the University of Massachusetts and the Infrared Processes and Analysis Center, California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. E.M.L.'s participation was made possible in part by a Ford Foundation Predoctoral Fellowship. L.J.K. and E. M. L. gratefully acknowledge support by NSF EARLY CAREER AWARD AST07-48559. A. M. S. acknowledges support by NASA through a Hubble Fellowship grant. A.R. and S.C.'s research is part of the 11th Five Year Plan Project No. 11P-409 at TIFR. R. A. C. and R. P. K. acknowledge support through NSF grants. G. P. and M. H. acknowledge support from the Millennium Center for Supernova Science (P06-045-F), Comite Mixto ESO-Gobierno de Chile, Centro de Astrofisica FONDAP (15010003), Center of Excellence in Astrophysics and Associated Technologies (PFB 06) and Proyectos Fondecyt 1060808 and 1109421. NR 49 TC 26 Z9 26 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JAN 20 PY 2010 VL 709 IS 1 BP L26 EP L31 DI 10.1088/2041-8205/709/1/L26 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 540DC UT WOS:000273310000005 ER PT J AU Mehdiabadi, NJ Kronforst, MR Queller, DC Strassmann, JE AF Mehdiabadi, Natasha J. Kronforst, Marcus R. Queller, David C. Strassmann, Joan E. TI Phylogeography and sexual macrocyst formation in the social amoeba Dictyostelium giganteum SO BMC EVOLUTIONARY BIOLOGY LA English DT Article ID CELLULAR SLIME-MOLDS; SPECIES RICHNESS; GLOBAL DIVERSITY; MATING TYPES; MATE CHOICE; PHYLOGENY; MICROORGANISMS; BIODIVERSITY; EVOLUTION; BEHAVIOR AB Background: Microorganisms are ubiquitous, yet we are only beginning to understand their diversity and population structure. Social amoebae (Dictyostelia) are a diverse group of unicellular eukaryotic microbes that display a unique social behaviour upon starvation in which cells congregate and then some die to help others survive and disperse. The genetic relationships among co-occurring cells have a major influence on the evolution of social traits and recent population genetic analysis found extensive genetic variation and possible cryptic speciation in one dictyostelid species ( Dictyostelium purpureum). To further characterize the interplay among genetic variation, species boundaries, social behaviour, and reproductive isolation in the Dictyostelia, we conducted phylogenetic analyses and mating experiments with the geographically widespread social amoeba Dictyostelium giganteum. Results: We sequenced approximately 4,000 basepairs of the nuclear ribosomal DNA from 24 isolates collected from Texas, Michigan, Massachusetts, Virginia, and Wisconsin and identified 16 unique haplotypes. Analyses of the sequence data revealed very little genetic differentiation among isolates and no clear evidence of phylogenetic structure, although there was evidence for some genetic differentiation between the Massachusetts and Texas populations. These results suggest that sexual mating ( macrocyst formation) is not likely to correlate with either genetic or geographical distance. To test this prediction, we performed 108 mating experiments and found no association between mating probability and genetic or geographical distance. Conclusions: D. giganteum isolates from across North America display little genetic variation, phylogeographic structure, and genetic differentiation among populations relative to the cryptic species observed within D. purpureum. Furthermore, variation that does exist does not predict the probability of mating among clones. These results have important implications for our understanding of speciation and social evolution in microbes. C1 [Mehdiabadi, Natasha J.; Kronforst, Marcus R.; Queller, David C.; Strassmann, Joan E.] Rice Univ, Dept Ecol & Evolutionary Biol, Houston, TX 77005 USA. [Mehdiabadi, Natasha J.] Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, Washington, DC 20013 USA. [Mehdiabadi, Natasha J.] Smithsonian Inst, Labs Analyt Biol, Natl Museum Nat Hist, Washington, DC 20013 USA. [Kronforst, Marcus R.] Harvard Univ, FAS Ctr Syst Biol, Cambridge, MA 02138 USA. RP Mehdiabadi, NJ (reprint author), Rice Univ, Dept Ecol & Evolutionary Biol, Houston, TX 77005 USA. EM Mehdiabadi@si.edu OI Strassmann, Joan/0000-0003-0638-8440 FU National Science Foundation (NSF) [EF-0626963, DBI-0301415]; National Library of Medicine [5T15 LM07093] FX We thank Jim Cavender for graciously supplying isolate WS589 and members of the Strassmann-Queller lab for help with collecting samples, especially Chandra Jack, Tracy Edwards, William Massie, and Stephen Rodriguez. We also thank Sara Kalla for help and advice with macrocyst experiments, Ted Schultz for help with phylogenetic analyses, Jessica Louton and Scott Solomon for insightful discussions, and the Associate Editor and two anonymous reviewers for comments that helped to improve the manuscript. This material is based on work supported by the National Science Foundation (NSF) Program under Grant EF-0626963. N.J.M. was supported by NSF Postdoctoral Fellowship DBI-0301415 in Microbial Biology and a Keck Postdoctoral Fellowship in Computational Biology (National Library of Medicine Grant 5T15 LM07093). NR 44 TC 5 Z9 5 U1 0 U2 9 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 JAN 20 PY 2010 VL 10 AR 17 DI 10.1186/1471-2148-10-17 PG 8 WC Evolutionary Biology; Genetics & Heredity SC Evolutionary Biology; Genetics & Heredity GA 564XC UT WOS:000275250800002 PM 20089169 ER PT J AU Kime, NM Whitney, TK Ryan, MJ Rand, AS Marler, CA AF Kime, Nicole M. Whitney, Tina K. Ryan, Michael J. Rand, A. Stanley Marler, Catherine A. TI Treatment with arginine vasotocin alters mating calls and decreases call attractiveness in male tungara frogs SO GENERAL AND COMPARATIVE ENDOCRINOLOGY LA English DT Article DE Arginine vasotocin; AVT; Anuran; Frog; Tungara frog; Physalaemus pustulosus; Communication; Sexual selection; Mate choice; Mate preference ID PHYSALAEMUS-PUSTULOSUS; NEOTROPICAL FROG; HYLA-VERSICOLOR; CRICKET FROGS; BEHAVIOR; MECHANISMS; TREEFROG; MANIPULATIONS; PREFERENCES; VASOPRESSIN AB The peptide hormone arginine vasotocin (AVT) and its mammalian homolog arginine vasopressin modulate a variety of social behaviors in vertebrates. In anurans, AVT influences the production of advertisement calls, the acoustic signals that males use to attract females and repel rival males. In this study, we investigate the effects of AVT on call characteristics in the tungara frog (Physalaemus pustulosus). Tungara frogs produce a "whine" that is important for species recognition; they may also produce a second, attractive call component, the "chuck". We used a field playback experiment to determine changes in male calling behavior following treatment with AVT. A previous study showed that AVT alters call rate and the production of chucks; in the current analysis, we focus on changes in the whine. Males produce shorter whines with higher initial frequencies following treatment with AVT. Call changes do not vary with a social stimulus. We also used female phonotaxis experiments to investigate the effects of call changes on female mate choice. Females disfavor the calls produced by males treated with exogenous AVT. We suggest that AVT influences motivation to call and the motor control of call production, but that over-stimulation of the vocal system limited the production of attractive calls in this experimental context. (C) 2009 Elsevier Inc. All rights reserved. C1 [Kime, Nicole M.] Edgewood Coll, Dept Nat Sci, Madison, WI 53711 USA. [Kime, Nicole M.; Whitney, Tina K.; Marler, Catherine A.] Univ Wisconsin, Dept Psychol, Madison, WI 53706 USA. [Ryan, Michael J.] Univ Texas Austin, Sect Integrat Biol, Austin, TX 78712 USA. [Ryan, Michael J.; Rand, A. Stanley] Smithsonian Trop Res Inst, Balboa, Panama. RP Kime, NM (reprint author), Edgewood Coll, Dept Nat Sci, 1000 Edgewood Coll Dr, Madison, WI 53711 USA. EM nkime@edgewood.edu RI Marler, Catherine/D-1285-2011 FU NSF [IBN 0078150] FX We thank Pat Martin for her insight into the design of these experiments and her invaluable assistance as we prepared for field work. We also thank Ximena Bernal for her support and suggestions in Panama, and John Marino for his assistance with call analysis back in Wisconsin. The Smithsonian Tropical Research institute was instrumental in providing space and research support. This project was funded by NSF Grant IBN 0078150. NR 39 TC 13 Z9 14 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 0016-6480 J9 GEN COMP ENDOCR JI Gen. Comp. Endocrinol. PD JAN 15 PY 2010 VL 165 IS 2 BP 221 EP 228 DI 10.1016/j.ygcen.2009.06.023 PG 8 WC Endocrinology & Metabolism SC Endocrinology & Metabolism GA 542TD UT WOS:000273517500006 PM 19576218 ER PT J AU Niven, JE Buckingham, CJ Lumley, S Cuttle, MF Laughlin, SB AF Niven, Jeremy E. Buckingham, Christian J. Lumley, Sheila Cuttle, Matthew F. Laughlin, Simon B. TI Visual Targeting of Forelimbs in Ladder-Walking Locusts SO CURRENT BIOLOGY LA English DT Article ID APPROACH PHASE; LEG MOVEMENTS; PREY-CAPTURE; STICK INSECT; COORDINATION; LOCOMOTION; OBSTACLE; INFORMATION; ENVIRONMENT; COCKROACH AB Accurate limb placement helps animals and robots to walk on substrates that are uneven or contain gaps. Visual information is important in controlling limb placement in walking mammals [1-4] but has received little attention in insects [5-7]. We investigated whether desert locusts walking along a horizontal ladder use vision to control limb placement. High-speed video analysis showed that locusts targeted their front legs to specific rungs in the absence of any previous contact, suggesting that visual information alone is sufficient for targeting single steps. Comparison between the proportions of missed steps before and after monocular occlusion showed that monocular visual information was used to place the ipsilateral but not the contralateral front leg. Accurate placement also depended upon mechanosensory inputs from the antennae and proprioceptive feedback from the ipsilateral but not the contralateral forelimb. Locusts also compensated for the loss of inputs to one eye by altering their stepping pattern. Changing the rung position after initiation of a step showed that targeting of the front leg depends on visual information acquired before but not during a step. The trajectory was only modified after missing the rung. Our data show that locusts walking in environments where footholds are limited use visual and mechanosensory information to place their front legs. C1 [Niven, Jeremy E.; Buckingham, Christian J.; Lumley, Sheila; Laughlin, Simon B.] Univ Cambridge, Dept Zool, Cambridge CB2 3EJ, England. [Niven, Jeremy E.] Smithsonian Trop Res Inst, Panama City, Panama. [Cuttle, Matthew F.] Univ Southampton, Sch Biol Sci, Southampton SO16 7PX, Hants, England. RP Niven, JE (reprint author), Univ Cambridge, Dept Zool, Downing St, Cambridge CB2 3EJ, England. EM jen22@hermes.cam.ac.uk RI Niven, Jeremy/A-5883-2011; OI Lumley, Sheila/0000-0001-6825-9324; Laughlin, Simon/0000-0003-4659-6543 FU Royal Society; Smithsonian Tropical Research Institute Laboratory of Evolutionary Behaviour and Neuroscience; Levinson Family Foundation FX We thank B. Hedwig for comments on the manuscript, B. Sengupta for assistance with analysis, M. Burrows for the loan of high-speed video cameras, and G. Harrison and S. Ellis for ladder design. This study was supported by the Royal Society, the Smithsonian Tropical Research Institute Laboratory of Evolutionary Behaviour and Neuroscience, and the Levinson Family Foundation (J.E.N.). NR 25 TC 21 Z9 21 U1 1 U2 12 PU CELL PRESS PI CAMBRIDGE PA 600 TECHNOLOGY SQUARE, 5TH FLOOR, CAMBRIDGE, MA 02139 USA SN 0960-9822 J9 CURR BIOL JI Curr. Biol. PD JAN 12 PY 2010 VL 20 IS 1 BP 86 EP 91 DI 10.1016/j.cub.2009.10.079 PG 6 WC Biochemistry & Molecular Biology; Cell Biology SC Biochemistry & Molecular Biology; Cell Biology GA 544YM UT WOS:000273697500029 PM 20036539 ER PT J AU Levesque, EM Bloom, JS Butler, NR Perley, DA Cenko, SB Prochaska, JX Kewley, LJ Bunker, A Chen, HW Chornock, R Filippenko, AV Glazebrook, K Lopez, S Masiero, J Modjaz, M Morgan, A Poznanski, D AF Levesque, Emily M. Bloom, Joshua S. Butler, Nathaniel R. Perley, Daniel A. Cenko, S. Bradley Prochaska, J. Xavier Kewley, Lisa J. Bunker, Andrew Chen, Hsiao-Wen Chornock, Ryan Filippenko, Alexei V. Glazebrook, Karl Lopez, Sebastian Masiero, Joseph Modjaz, Maryam Morgan, Adam Poznanski, Dovi TI GRB 090426: the environment of a rest-frame 0.35-s gamma-ray burst at a redshift of 2.609 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: ISM; gamma-rays: bursts ID LARGE-SCALE ENVIRONMENTS; HUBBLE-SPACE-TELESCOPE; HOST GALAXY; STAR-FORMATION; SPECTRAL CATALOG; FORMATION RATES; ALPHA EMISSION; DURATION; PROGENITORS; AFTERGLOW AB We present the discovery of an absorption-line redshift of z = 2.609 for GRB 090426, establishing the first firm lower limit to a redshift for a gamma-ray burst (GRB) with an observed duration of < 2 s. With a rest-frame burst duration of T(90z) = 0.35 s and a detailed examination of the peak energy of the event, we suggest that this is likely (at > 90 per cent confidence) a member of the short/hard phenomenological class of GRBs. From analysis of the optical-afterglow spectrum we find that the burst originated along a very low H i column density sightline, with N(H i) < 3.2 x 1019 cm-2. Our GRB 090426 afterglow spectrum also appears to have weaker low-ionization absorption (Si ii, C ii) than similar to 95 per cent of previous afterglow spectra. Finally, we also report the discovery of a blue, very luminous, star-forming putative host galaxy (similar to 2L(*)) at a small angular offset from the location of the optical afterglow. We consider the implications of this unique GRB in the context of burst duration classification and our understanding of GRB progenitor scenarios. C1 [Levesque, Emily M.; Kewley, Lisa J.; Masiero, Joseph] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Levesque, Emily M.] Smithsonian Astrophys Observ, Cambridge, MA 02139 USA. [Bloom, Joshua S.; Butler, Nathaniel R.; Perley, Daniel A.; Cenko, S. Bradley; Chornock, Ryan; Filippenko, Alexei V.; Modjaz, Maryam; Morgan, Adam; Poznanski, Dovi] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Prochaska, J. Xavier] Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO Lick Observ, Santa Cruz, CA 95064 USA. [Bunker, Andrew] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England. [Chen, Hsiao-Wen] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Glazebrook, Karl] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Lopez, Sebastian] Univ Chile, Dept Astron, Santiago, Chile. RP Levesque, EM (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. EM emsque@ifa.hawaii.edu RI Glazebrook, Karl/N-3488-2015; Lopez, Sebastian /I-5657-2016; OI Glazebrook, Karl/0000-0002-3254-9044; Lopez, Sebastian /0000-0003-0389-0902; Masiero, Joseph/0000-0003-2638-720X FU W. M. Keck Foundation; Ford Foundation; Las Cumbres Observatory Global Telescope Network; NASA [NNG05GF55G, NNG06DO90A, NNX07AE94G, NNG06GI86G]; US Department of Energy (DOE) [DE-FC02-06ER41453]; NSF [AST-0548180]; US NSF [AST-0607485]; TABASGO Foundation; Gary and Cynthia Bengier and the Richard and Rhoda Goldman Fund; Miller Institute for Basic Research in Science; Chilean Centro de Astrofi sica FONDAP [15010003]; FONDECYT [1060823] FX Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and NASA; the observatory was made possible by the generous financial support of the W. M. Keck Foundation. We wish to thank the support staff of the W. M. Keck Observatory, Subaru telescope and Gemini Observatory for their hospitality and assistance. We also thank to Jeff Silverman for his assistance during our observations. This paper made use of data from the Gamma-Ray Burst Coordinates Network (GCN) circulars. EML's participation was made possible in part by a Ford Foundation Predoctoral Fellowship. JSB's group is supported in part by Las Cumbres Observatory Global Telescope Network, and NASA/Swift Guest Investigator grant NNG05GF55G. NRB is partially supported by US Department of Energy (DOE) SciDAC grant DE-FC02-06ER41453 and through the GLAST Fellowship Program (NASA Cooperative Agreement: NNG06DO90A). JXP is partially supported by NASA/Swift grant NNX07AE94G and an NSF CAREER grant (AST-0548180). AVF and his group are grateful for funding from US NSF grant AST-0607485, NASA/Swift grant NNG06GI86G, DOE/SciDAC grant DE-FC02-06ER41453, the TABASGO Foundation, Gary and Cynthia Bengier and the Richard and Rhoda Goldman Fund. MM is supported by a research fellowship from the Miller Institute for Basic Research in Science. SL was partly supported by the Chilean Centro de Astrofi sica FONDAP No. 15010003 and by FONDECYT grant No. 1060823. NR 98 TC 49 Z9 51 U1 0 U2 2 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 JAN 11 PY 2010 VL 401 IS 2 BP 963 EP 972 DI 10.1111/j.1365-2966.2009.15733.x PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 540FS UT WOS:000273317300015 ER PT J AU Hopkins, PF Bundy, K Hernquist, L Wuyts, S Cox, TJ AF Hopkins, Philip F. Bundy, Kevin Hernquist, Lars Wuyts, Stijn Cox, Thomas J. TI Discriminating between the physical processes that drive spheroid size evolution SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Review DE galaxies: active; galaxies: evolution; galaxies: formation; quasars: general; cosmology: theory ID EARLY-TYPE GALAXIES; BLACK-HOLE MASS; HIGH-REDSHIFT GALAXIES; STAR-FORMING GALAXIES; TULLY-FISHER RELATION; SIMILAR-TO 2; DISC MERGER REMNANTS; DIGITAL SKY SURVEY; VELOCITY DISPERSION CORRELATION; INTEGRAL-FIELD SPECTROSCOPY AB Observations have shown that massive galaxies at high redshift have much smaller effective radii than galaxies of similar mass today; however, recent work has shown that they have similar central densities. The primary growth of size, therefore, relates to the apparent relative abundance of low-density material at low redshifts. But various models have been proposed to accomplish this, and the exact contribution of these mechanisms, relative to others that would, for example, lower the density of the system uniformly, or relate to possible observational misestimates of the stellar mass distribution, remain uncertain, as does the degree to which this evolution is driven by processes of initial spheroid formation versus subsequent 'dry' assembly of spheroids. These different possibilities also yield dramatically different constraints on any possible evolution in the M(BH)-Sigma relation. Here, we compile observations of spheroid properties as a function of redshift and use them to test the different proposed models, each of which we have calibrated and studied in a suite of high-resolution hydrodynamic simulations. We show that the evolution in progenitor disc gas fractions with redshift gives rise to the initial formation of smaller spheroids at high redshift. We then consider how these early-forming systems must evolve to be consistent with the larger sizes of old spheroids today. We consider (1) equal-density 'dry' mergers, (2) later major or minor 'dry' mergers with less dense galaxies, (3) adiabatic expansion, after significant gas mass loss, (4) gradients in stellar mass-to-light ratios from young nuclear stellar populations (yielding smaller R(e) at early times, which vanish as the system fades), (5) biases in the stellar mass estimation of high-redshift (young) systems (from e.g. uncertain asymptotic giant branch starlight contributions) and (6) observational effects (possible biases in fitting or missed light from surface brightness dimming, or the effects of different definitions of effective radii). In principle, any of these models could be tuned to explain any observed effective radius evolution. However, the predicted evolution in velocity dispersions, central stellar mass surface densities and profile shape are very distinct. Comparing with observations, only model (2), later or minor 'dry' mergers with less dense systems, is consistent with the constraints as an explanation of the entire effect. Moreover, it is the only model which allows for any evolution in M(BH)-Sigma towards more massive black holes (BHs) at high redshift. Still, the amount of merging needed for this to explain the observed factor of similar to 6 size evolution is larger than that predicted by hierarchical growth and clustering constraints. We, therefore, consider a cosmologically motivated model with high-resolution simulations, in which the initial galaxy forms in a gas rich merger and is observed at an appropriate age under representative conditions, then evolves undergoing a 'typical' level of dry merging and mass loss. We show that this case is consistent with all the observational constraints without tension with cosmological expectations. Effect (2), which builds up an extended, low-density envelope, dominates the evolution (giving factors similar to 2-3 size evolution), but effects (1), (3), (4) and (possibly) (6) each contribute an additional similar to 20 per cent size evolution (net factor of similar to 2), together bringing the natural cosmological predictions into good agreement with the combination of observational constraints. We discuss implications for the evolution in correlations between BH and host bulge properties and show that this naturally predicts some evolution similar to that observed; better observations of BH masses could also constrain host galaxy merger histories. C1 [Hopkins, Philip F.; Bundy, Kevin] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Hernquist, Lars; Wuyts, Stijn; Cox, Thomas J.] 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; W. M. Keck Foundation FX We thank Eliot Quataert, Norm Murray, Pieter van Dokkum and Ignacio Trujillo for a number of very helpful conversations and suggestions throughout the development of this manuscript. Support for PFH was provided by the Miller Institute for Basic Research in Science, University of California Berkeley. SW and TJC gratefully acknowledge support from the W. M. Keck Foundation. NR 173 TC 133 Z9 136 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 JAN 11 PY 2010 VL 401 IS 2 BP 1099 EP 1117 DI 10.1111/j.1365-2966.2009.15699.x PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 540FS UT WOS:000273317300026 ER PT J AU Hopkins, PF Keres, D Ma, CP Quataert, E AF Hopkins, Philip F. Keres, Dusan Ma, Chung-Pei Quataert, Eliot TI When should we treat galaxies as isolated? SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Review DE galaxies: active; galaxies: evolution; galaxies: formation; galaxies: spiral; cosmology: theory ID STAR-FORMING GALAXIES; TULLY-FISHER RELATION; DARK-MATTER HALOES; ECCENTRIC GRAVITATIONAL INSTABILITIES; LAMBDA-CDM COSMOLOGY; BARRED GALAXIES; SPIRAL GALAXIES; DISK GALAXIES; STELLAR BARS; NUMERICAL SIMULATIONS AB Traditionally, secular evolution is defined as evolution of systems where the internal growth of structure and instabilities dominates the growth via external drivers (e.g. accretion and mergers). Most study has focused on 'isolated' galaxies, where seed asymmetries may represent realistic cosmological substructure, but subsequent evolution ignores galaxy growth and interactions. Large-scale modes in the disc then grow on a time-scale of the order of a disc rotation period (similar to 0.1-1 Gyr). If, however, galaxies evolve cosmologically on a shorter time-scale, then it may not be appropriate to consider them 'isolated'. We outline simple scalings to ask whether, under realistic conditions, the time-scale for secular evolution is shorter than the time-scale for cosmological accretion and mergers. We show that this is the case in a relatively narrow but important range of perturbation amplitudes corresponding to substructure or mode/bar fractional amplitudes delta similar to 0.01-0.1, the range of most interest for observed strong bars and most pseudo-bulges. At smaller amplitudes delta < 0.1, systems are not isolated: typical discs will grow by accretion at a comparable level over even a single dynamical time. At larger amplitudes delta 0.1, the evolution is no longer secular; the direct gravitational evolution of the seed substructure swamps the internal disc response. We derive criteria for when discs can be well approximated as 'isolated' as a function of mass, redshift and disc stability. The relevant parameter space shrinks at higher mass, higher disc stability and higher z as accretion rates increase. The cosmological rate of galaxy evolution also defines a maximum bar/mode lifetime of practical interest, of similar to 0.1 t(Hubble)(z). Longer lived modes will encounter cosmological effects and will decouple from their drivers (if they are driven). C1 [Hopkins, Philip F.; Ma, Chung-Pei; Quataert, Eliot] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Keres, Dusan] 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; ITC fellowship FX We thank Lars Hernquist and T. J. Cox for helpful discussions, as well as Simon White and the anonymous referee for suggestions that greatly improved this manuscript. Support for PFH was provided by the Miller Institute for Basic Research in Science, University of California, Berkeley. DK acknowledges the support of the ITC fellowship at the Harvard College Observatory. NR 127 TC 5 Z9 5 U1 0 U2 2 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 JAN 11 PY 2010 VL 401 IS 2 BP 1131 EP 1140 DI 10.1111/j.1365-2966.2009.15700.x PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 540FS UT WOS:000273317300028 ER PT J AU Jonker, PG Miller-Jones, J Homan, J Gallo, E Rupen, M Tomsick, J Fender, RP Kaaret, P Steeghs, DTH Torres, MAP Wijnands, R Markoff, S Lewin, WHG AF Jonker, P. G. Miller-Jones, J. Homan, J. Gallo, E. Rupen, M. Tomsick, J. Fender, R. P. Kaaret, P. Steeghs, D. T. H. Torres, M. A. P. Wijnands, R. Markoff, S. Lewin, W. H. G. TI Following the 2008 outburst decay of the black hole candidate H 1743-322 in X-ray and radio SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; binaries; stars: individual: H 1743-322; X-rays: binaries ID ADVECTION-DOMINATED ACCRETION; MICROQUASAR XTE J1550-564; NOVA-MUSCAE 1991; LOW-HARD STATE; LOW/HARD STATE; MULTIWAVELENGTH OBSERVATIONS; SWIFT J1753.5-0127; QUIESCENT STATE; EVENT HORIZONS; CIRCINUS X-1 AB In this paper, we report on radio (Very Large Array and Austrialian Telescope Compact Array) and X-ray (RXTE, Chandra and Swift) observations of the outburst decay of the transient black hole candidate H 1743-322 in early 2008. We find that the X-ray light curve followed an exponential decay, levelling off towards its quiescent level. The exponential decay time-scale is approximate to 4 days and the quiescent flux corresponds to a luminosity of 3 x 10(32)(d/7.5kpc)(2)erg s(-1). This together with the relation between quiescent X-ray luminosity and orbital period reported in the literature suggests that H 1743-322 has an orbital period longer than approximate to 10 h. Both the radio and X-ray light curve show evidence for flares. The radio-X-ray correlation can be well described by a power-law with index approximate to 0.18. This is much lower than the index of approximate to 0.6-0.7 found for the decay of several black hole transients before. The radio spectral index measured during one of the radio flares while the source is in the low-hard state is -0.5 +/- 0.15, which indicates that the radio emission is optically thin. This is unlike what has been found before in black hole sources in the low-hard state. We attribute the radio flares and the low index for the radio-X-ray correlation to the presence of shocks downstream the jet flow, triggered by ejection events earlier in the outburst. We find no evidence for a change in X-ray power-law spectral index during the decay, although the relatively high extinction of N(H) approximate to 2.3 x 10(22) cm(-2) limits the detected number of soft photons and thus the accuracy of the spectral fits. C1 [Jonker, P. G.] SRON, Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. [Jonker, P. G.; Steeghs, D. T. H.; Torres, M. A. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Miller-Jones, J.] NRAO Headquarters, Charlottesville, VA 22903 USA. [Homan, J.; Gallo, E.; Lewin, W. H. G.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Rupen, M.] NRAO, Array Operat Ctr, Socorro, NM 87801 USA. [Tomsick, J.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Fender, R. P.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Kaaret, P.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Steeghs, D. T. H.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Wijnands, R.; Markoff, S.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands. RP Jonker, PG (reprint author), SRON, Netherlands Inst Space Res, Sorbonnelaan 2, NL-3584 CA Utrecht, Netherlands. EM p.jonker@sron.nl RI Steeghs, Danny/C-5468-2009; OI Steeghs, Danny/0000-0003-0771-4746; Miller-Jones, James/0000-0003-3124-2814 FU Netherlands Organisation for Scientific Research; NASA [GO8-9042A]; DTHS FX PGJ acknowledges support from a VIDI grant from the Netherlands Organisation for Scientific Research. MAPT acknowledges support from NASA grant GO8-9042A. DTHS acknowledges an STFC Advanced Fellowship. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. NR 59 TC 36 Z9 36 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 JAN 11 PY 2010 VL 401 IS 2 BP 1255 EP 1263 DI 10.1111/j.1365-2966.2009.15717.x PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 540FS UT WOS:000273317300038 ER PT J AU Sun, M Donahue, M Roediger, E Nulsen, PEJ Voit, GM Sarazin, C Forman, W Jones, C AF Sun, M. Donahue, M. Roediger, E. Nulsen, P. E. J. Voit, G. M. Sarazin, C. Forman, W. Jones, C. TI SPECTACULAR X-RAY TAILS, INTRACLUSTER STAR FORMATION, AND ULXs IN A3627 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: general; galaxies: clusters: individual (A3627); galaxies: individual (ESO 137-001, ESO 137-002); X-rays: galaxies ID MASSIVE GALAXY CLUSTER; VIRGO CLUSTER; SPIRAL GALAXIES; HI OBSERVATIONS; DISC GALAXIES; COMA CLUSTER; CHANDRA OBSERVATIONS; LUMINOSITY FUNCTION; GREAT ATTRACTOR; MILKY-WAY AB We present the discovery of spectacular double X-ray tails associated with ESO 137-001 and a possibly heated X-ray tail associated with ESO 137-002, both late-type galaxies in the closest rich cluster Abell 3627. A deep Chandra observation of ESO 137-001 allows us for the first time to examine the spatial and spectral properties of such X-ray tails in detail. Besides the known bright tail that extends to similar to 80 kpc from ESO 137-001, a fainter and narrower secondary tail with a similar length was surprisingly revealed, as well as some intriguing substructures in the main tail. There is little temperature variation along both tails. The widths of the secondary tail and the greater part of the main tail also remain nearly constant with the distance from the galaxy. All these results challenge the current simulations. The Chandra data also reveal 19 X-ray point sources around the X-ray tails. We identified six X-ray point sources as candidates of intracluster ultra-luminous X-ray sources with L(0.3-10 keV) of up to 2.5 x 10(40) erg s(-1). Gemini spectra of intracluster H II regions downstream of ESO 137-001 are also presented, as well as the velocity map of these H II regions that shows the imprint of ESO 137-001's disk rotation. For the first time, we unambiguously know that active star formation can happen in the cold interstellar medium (ISM) stripped by intracluster medium (ICM) ram pressure, and it may contribute a significant amount of the intracluster light. We also report the discovery of a 40 kpc X-ray tail of another late-type galaxy in A3627, ESO 137-002. Its X-ray tail seems hot, similar to 2 keV (compared to similar to 0.8 keV for ESO 137-001's tails). The Ha data for ESO 137-002 are also presented. We conclude that the high-pressure environment around these two galaxies is important for their bright X-ray tails and the intracluster star formation. The soft X-ray tails can reveal a great deal of the thermal history of the stripped cold ISM in mixing with the hot ICM, which is discussed along with intracluster star formation. C1 [Sun, M.; Sarazin, C.] Univ Virginia, Dept Astron, Charlottesville, VA 22901 USA. [Donahue, M.; Voit, G. M.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Roediger, E.] Univ Bremen, D-28725 Bremen, Germany. [Nulsen, P. E. J.; Forman, W.; Jones, C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Sun, M (reprint author), Univ Virginia, Dept Astron, POB 400325, Charlottesville, VA 22901 USA. EM msun@virginia.edu RI Donahue, Megan/B-5361-2012; OI Nulsen, Paul/0000-0003-0297-4493; Forman, William/0000-0002-9478-1682; Voit, Gerard/0000-0002-3514-0383 FU NASA [GO7-8081A, GO8-9083X, NNG-05GD82G]; HST [HST-GO-11683.01-A]; NASA LTSA; DFG FX M. S. is grateful to Tom Matheson for his help in the planning and the data analysis of the Gemini observations. M. S. thanks Suresh Sivanandam for the preprint of the Spitzer results and discussions. We thank Hans Bohringer, Wolfgang Kapferer, and Bernd Vollmer for discussions. We thank Keith Arnaud for the clarification on the CEMEKL model. We present data obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership. We also present data obtained with the Southern Observatory for Astrophysical Research, which is a joint project of the Brazilian Ministry of Science, the National Optical Observatories, the University of North Carolina, and Michigan State University. Wemade use of the NASA/IPAC Extragalactic Database and the Hyperleda database. The financial support for this work was provided by the NASA grant GO7-8081A, the NASA grant GO8-9083X, and the HST grant HST-GO-11683.01-A. M. D. and G. M. V. acknowledge support from a NASA LTSA grant NASA NNG-05GD82G. E. R. acknowledges funding by the DFG Priority Programme 1177 "Galaxy Evolution." NR 66 TC 57 Z9 57 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 JAN 10 PY 2010 VL 708 IS 2 BP 946 EP 964 DI 10.1088/0004-637X/708/2/946 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 536CY UT WOS:000273021000004 ER PT J AU Fu, R O'Connell, RJ Sasselov, DD AF Fu, Roger O'Connell, Richard J. Sasselov, Dimitar D. TI THE INTERIOR DYNAMICS OF WATER PLANETS SO ASTROPHYSICAL JOURNAL LA English DT Article DE convection; planetary systems ID MASS-RADIUS RELATIONSHIPS; STAGNANT LID CONVECTION; HIGH-PRESSURE ICE; OCEAN-PLANETS; SUPER-EARTHS; GALILEAN SATELLITES; TERRESTRIAL PLANET; MELTING CURVE; GPA; GANYMEDE AB The ever-expanding catalog of detected super-Earths calls for theoretical studies of their properties in the case of a substantial water layer. This work considers such water planets with a range of masses and water mass fractions (2-5 M(Earth), 0.02%-50% H(2)O). First, we model the thermal and dynamical structure of the near-surface for icy and oceanic surfaces, finding separate regimes where the planet is expected to maintain a subsurface liquid ocean and where it is expected to exhibit ice tectonics. Newly discovered exoplanets may be placed into one of these regimes given estimates of surface temperature, heat flux, and gravity. Second, we construct a parameterized convection model for the underlying ice mantle of higher ice phases, finding that materials released from the silicate-iron core should traverse the ice mantle on the timescale of 0.1 to 100 megayears. We present the dependence of the overturn times of the ice mantle and the planetary radius on total mass and water mass fraction. Finally, we discuss the implications of these internal processes on atmospheric observables. C1 [Fu, Roger; O'Connell, Richard J.] Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. [Sasselov, Dimitar D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Fu, R (reprint author), Harvard Univ, Dept Earth & Planetary Sci, 20 Oxford St, Cambridge, MA 02138 USA. EM rogerfu12@gmail.com; richard_oconnell@harvard.edu; sasselov@cfa.harvard.edu FU Harvard University Origins of Life Initiative FX We thank Diana Valencia, Lisa Kaltenegger, and Wade Hennings for discussions that led to advances in understanding and the conception of the scope of this paper. This work is supported by the Harvard University Origins of Life Initiative. NR 64 TC 29 Z9 29 U1 2 U2 13 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 JAN 10 PY 2010 VL 708 IS 2 BP 1326 EP 1334 DI 10.1088/0004-637X/708/2/1326 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 536CY UT WOS:000273021000030 ER PT J AU Voevodkin, A Borozdin, K Heitmann, K Habib, S Vikhlinin, A Mescheryakov, A Hornstrup, A Burenin, R AF Voevodkin, Alexey Borozdin, Konstantin Heitmann, Katrin Habib, Salman Vikhlinin, Alexey Mescheryakov, Alexander Hornstrup, Allan Burenin, Rodion TI FOSSIL SYSTEMS IN THE 400d CLUSTER CATALOG SO ASTROPHYSICAL JOURNAL LA English DT Article DE catalogs; galaxies: clusters: general; X-rays: galaxies: clusters ID DIGITAL SKY SURVEY; X-RAY; GALAXY GROUPS; LUMINOSITY FUNCTION; MILLENNIUM SIMULATION; DATA RELEASE; MASS; RX-J1416.4+2315; EVOLUTION; UNIVERSE AB We report the discovery of seven new fossil systems in the 400d cluster survey. Our search targets nearby, z <= 0.2, and X-ray bright, L(X) >= 10(43) erg s(-1), clusters of galaxies. Where available, we measure the optical luminosities from Sloan Digital Sky Survey images, thereby obtaining uniform sets of both X-ray and optical data. Our selection criteria identify 12 fossil systems, out of which five are known from previous studies. While in general agreement with earlier results, our larger sample size allows us to put tighter constraints on the number density of fossil clusters. It has been previously reported that fossil groups are more X-ray bright than other X-ray groups of galaxies for the same optical luminosity. We find, however, that the X-ray brightness of massive fossil systems is consistent with that of the general population of galaxy clusters and follows the same L(X)-L(opt) scaling relation. C1 [Voevodkin, Alexey; Borozdin, Konstantin; Heitmann, Katrin; Habib, Salman] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Voevodkin, Alexey; Vikhlinin, Alexey; Mescheryakov, Alexander; Burenin, Rodion] Space Res Inst IKI, Moscow, Russia. [Vikhlinin, Alexey; Mescheryakov, Alexander] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hornstrup, Allan] Tech Univ Denmark, Natl Space Inst, DK-2100 Copenhagen, Denmark. RP Voevodkin, A (reprint author), Los Alamos Natl Lab, Los Alamos, NM 87545 USA. NR 40 TC 28 Z9 28 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 JAN 10 PY 2010 VL 708 IS 2 BP 1376 EP 1387 DI 10.1088/0004-637X/708/2/1376 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 536CY UT WOS:000273021000034 ER PT J AU Young, M Elvis, M Risaliti, G AF Young, M. Elvis, M. Risaliti, G. TI THE X-RAY ENERGY DEPENDENCE OF THE RELATION BETWEEN OPTICAL AND X-RAY EMISSION IN QUASARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; galaxies: active ID ACTIVE GALACTIC NUCLEI; DIGITAL SKY SURVEY; RADIO-QUIET QUASARS; ABSORPTION-LINE QUASARS; SEYFERT-GALAXIES; DATA RELEASE; ASTRONOMICAL DATA; ACCRETION MODELS; PARAMETER SPACE; STELLAR OBJECTS AB We develop a new approach to the well-studied anti-correlation between the optical-to-X-ray spectral index, alpha(ox), and the monochromatic optical luminosity, l(opt). By cross-correlating the Sloan Digital Sky Survey DR5 quasar catalog with the XMM-Newton archive, we create a sample of 327 quasars with X-ray signal-to-noise ratio (S/N) > 6, where both optical and X-ray spectra are available. This allows alpha(ox) to be defined at arbitrary frequencies, rather than the standard 2500 angstrom and 2 keV. We find that while the choice of optical wavelength does not strongly influence the alpha(ox)-l(opt) relation, the slope of the relation does depend on the choice of X-ray energy. The slope of the relation becomes steeper when alpha(ox) is defined at low (similar to 1 keV) X-ray energies. This change is significant when compared to the slope predicted by a decrease in the baseline over which alpha(ox) is defined. The slopes are also marginally flatter than predicted at high (similar to 10 keV) X-ray energies. Partial correlation tests show that while the primary driver of alpha(ox) is l(opt), the Eddington ratio correlates strongly with alpha(ox) when l(opt) is taken into account, so accretion rate may help explain these results. We combine the alpha(ox)-l(opt) and Gamma-L(bol)/L(Edd) relations to naturally explain two results: (1) the existence of the Gamma-l(x) relation as reported in Young et al., and (2) the lack of a Gamma-l(opt) relation. The consistency of the optical/X-ray correlations establishes a more complete framework for understanding the relation between quasar emission mechanisms. We also discuss two correlations with the hard X-ray bolometric correction, which we show correlates with both alpha(ox) and Eddington ratio. This confirms that an increase in accretion rate correlates with a decrease in the fraction of up-scattered disk photons. C1 [Young, M.; Elvis, M.; Risaliti, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Young, M.] Boston Univ, Dept Astron, Boston, MA 02215 USA. [Risaliti, G.] INAF Osservatorio Arcetri, Florence, Italy. RP Young, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM myoung@cfa.harvard.edu OI Risaliti, Guido/0000-0002-3556-977X FU ESA Member States; NASA [NASA NNX07AI22G, NASA GO6-7102X]; SDSS; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England; 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 FX M.Y. thanks Ranjan Vasudevan for helpful conversations regarding this work. We thank the referee for useful comments that improved the quality of this paper. This paper is based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA, and the SDSS. 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. This research also made use of the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This work has been partially funded by NASA Grants NASA NNX07AI22G and NASA GO6-7102X. NR 55 TC 39 Z9 39 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 JAN 10 PY 2010 VL 708 IS 2 BP 1388 EP 1397 DI 10.1088/0004-637X/708/2/1388 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 536CY UT WOS:000273021000035 ER PT J AU Lee, KG Berger, E Knapp, GR AF Lee, Khee-Gan Berger, Edo Knapp, Gillian R. TI SHORT-TERM H alpha VARIABILITY IN M DWARFS SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: activity; stars: flare; stars: late-type; stars: magnetic fields ID STAR SPECTROSCOPIC SURVEY; PROPER-MOTION STARS; DIGITAL SKY SURVEY; MAGNETIC ACTIVITY; ULTRACOOL DWARFS; COOL NEIGHBORS; CHROMOSPHERIC ACTIVITY; BROWN DWARFS; NEARBY STARS; NLTT STARS AB We spectroscopically study the variability of H alpha emission in mid- to late-M dwarfs on timescales of similar to 0.1-1 hr as a proxy for magnetic variability. About 80% of our sample exhibits statistically significant variability on the full range of timescales probed by the observations, and with amplitude ratios in the range of similar to 1.2-4. No events with an order of magnitude increase in H alpha luminosity were detected, indicating that their rate is less than or similar to 0.05 hr(-1) (95% confidence level). We find a clear increase in variability with later spectral type, despite an overall decrease in H alpha "activity" (i.e., L(H alpha)/L(bol)). For the ensemble of H alpha variability events, we find a nearly order of magnitude increase in the number of events from timescales of about 10-30 minutes, followed by a roughly uniform distribution at longer durations. The event amplitudes follow an exponential distribution with a characteristic scale of Max(EW)/Min(EW) - 1 approximate to 0.7. This distribution predicts a low rate of similar to 10(-6) hr(-1) for events with Max(EW)/Min(EW) greater than or similar to 10, but serendipitous detections of such events in the past suggest that they represent a different distribution. Finally, we find a possible decline in the amplitude of events with durations of greater than or similar to 0.5 hr, which may point to a typical energy release in Ha events for each spectral type (E(H alpha) similar to L(H alpha) x t similar to const). Longer observations of individual active objects are required to further investigate this possibility. Similarly, a larger sample may shed light on whether Ha variability correlates with properties such as age or rotation velocity. C1 [Lee, Khee-Gan; Knapp, Gillian R.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Berger, Edo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Lee, KG (reprint author), Princeton Univ, Dept Astrophys Sci, Peyton Hall,Ivy Lane, Princeton, NJ 08544 USA. EM lee@astro.princeton.edu; eberger@cfa.harvard.edu NR 33 TC 22 Z9 22 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 JAN 10 PY 2010 VL 708 IS 2 BP 1482 EP 1491 DI 10.1088/0004-637X/708/2/1482 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 536CY UT WOS:000273021000043 ER PT J AU Foley, RJ Narayan, G Challis, PJ Filippenko, AV Kirshner, RP Silverman, JM Steele, TN AF Foley, Ryan J. Narayan, Gautham Challis, Peter J. Filippenko, Alexei V. Kirshner, Robert P. Silverman, Jeffrey M. Steele, Thea N. TI SN 2006bt: A PERPLEXING, TROUBLESOME, AND POSSIBLY MISLEADING TYPE Ia SUPERNOVA SO ASTROPHYSICAL JOURNAL LA English DT Article DE supernovae: general; supernovae: individual (SN 2006bt) ID HIGH-VELOCITY FEATURES; LIGHT CURVES; WHITE-DWARF; LUMINOSITY INDICATORS; FACTORY OBSERVATIONS; OPTICAL PHOTOMETRY; IMPROVED DISTANCES; DATA RELEASE; SPECTRA; SPECTROSCOPY AB SN 2006bt displays characteristics unlike those of any other known Type Ia supernova (SN Ia). We present optical light curves and spectra of SN 2006bt which demonstrate the peculiar nature of this object. SN 2006bt has broad, slowly declining light curves indicative of a hot, high-luminosity SN, but lacks a prominent second maximum in the i band as do low-luminosity SNe Ia. Its spectra are similar to those of low-luminosity SNe Ia, containing features that are only present in cool SN photospheres. Light-curve fitting methods suggest that SN 2006bt is reddened by a significant amount of dust; however, it occurred in the outskirts of its early-type host galaxy and has no strong Na D absorption in any of its spectra, suggesting a negligible amount of host-galaxy dust absorption. C II is possibly detected in our pre-maximum spectra, but at a much lower velocity than other elements. The progenitor was likely very old, being a member of the halo population of a galaxy that shows no signs of recent star formation. SNe Ia have been very successfully modeled as a one-parameter family, and this is fundamental to their use as cosmological distance indicators. SN 2006bt is a challenge to that picture, yet its relatively normal light curves allowed SN 2006bt to be included in cosmological analyses. We generate mock SN Ia data sets which indicate that contamination by similar objects will both increase the scatter of a SN Ia Hubble diagram and systematically bias measurements of cosmological parameters. However, spectra and rest-frame i-band light curves should provide a definitive way to identify and eliminate such objects. C1 [Foley, Ryan J.; Narayan, Gautham; Challis, Peter J.; Kirshner, Robert P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Narayan, Gautham] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Filippenko, Alexei V.; Silverman, Jeffrey M.; Steele, Thea N.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Foley, RJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rfoley@cfa.harvard.edu OI Narayan, Gautham/0000-0001-6022-0484 FU Alfred P. Sloan Foundation; Participating Institutions; National Science Foundation; U.S. Department of Energy; National Aeronautics and Space Administration; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England FX Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web site is http://www.sdss.org/. NR 66 TC 38 Z9 38 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 JAN 10 PY 2010 VL 708 IS 2 BP 1748 EP 1759 DI 10.1088/0004-637X/708/2/1748 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 536CY UT WOS:000273021000067 ER PT J AU Acciari, VA Aliu, E Arlen, T Aune, T Bautista, M Beilicke, M Benbow, W Bottcher, M Boltuch, D Bradbury, SM Buckley, JH Bugaev, V Byrum, K Cannon, A Cesarini, A Chow, YC Ciupik, L Cogan, P Cui, W Duke, C Falcone, A Finley, JP Finnegan, G Fortson, L Furniss, A Galante, N Gall, D Gillanders, GH Godambe, S Grube, J Guenette, R Gyuk, G Hanna, D Holder, J Hui, CM Humensky, TB 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 Millis, J Moriarty, P Nagai, T Ong, RA Otte, AN Pandel, D Perkins, JS Pichel, A 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 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 Wood, M Zitzer, B Abdo, AA Ackermann, M Ajello, M Baldini, L Ballet, J Barbiellini, G Bastieri, D Baughman, BM Bechtol, K Bellazzini, R Berenji, B Blandford, RD Bloom, ED Bonamente, E Borgland, AW Bregeon, J Brez, A Brigida, M Bruel, P Burnett, TH Caliandro, GA Cameron, RA Caraveo, PA Casandjian, JM Cavazzuti, E Cecchi, C Celik, O Chekhtman, A Cheung, CC Chiang, J Ciprini, S Claus, R Cohen-Tanugi, J Conrad, J Cutini, S Dermer, CD de Angelis, A de Palma, F Silva, EDE Drell, PS Drlica-Wagner, A Dubois, R Dumora, D Farnier, C Favuzzi, C Fegan, SJ Focke, WB Fortin, P Frailis, M Fukazawa, Y Fusco, P Gargano, F Gasparrini, D Gehrels, N Germani, S Giebels, B Giglietto, N Giommi, P Giordano, F Glanzman, T Godfrey, G Grenier, IA Grove, JE Guillemot, L Guiriec, S Hanabata, Y Hays, E Hughes, RE Jackson, MS Johannesson, G Johnson, AS Johnson, WN Kamae, T Katagiri, H Kataoka, J Kawai, N Kerr, M Knodlseder, J Kocian, ML Kuss, M Lande, J Latronico, L Longo, F Loparco, F Lott, B Lovellette, MN Lubrano, P Madejski, GM Makeev, A Mazziotta, MN McEnery, JE Meurer, C Michelson, PF Mitthumsiri, W Mizuno, T Moiseev, AA Monte, C Monzani, ME Morselli, A Moskalenko, IV Murgia, S Nolan, PL Norris, JP Nuss, E Ohsugi, T Omodei, N Orlando, E Ormes, JF Paneque, D Parent, D Pelassa, V Pepe, M Pesce-Rollins, M Piron, F Porter, TA Raino, S Rando, R Razzano, M Reimer, A Reimer, O Reposeur, T Rodriguez, AY Roth, M Ryde, F Sadrozinski, HFW Sanchez, D Sander, A Parkinson, PMS Scargle, JD Sgro, C Shaw, MS Siskind, EJ Smith, PD Spandre, G Spinelli, P Strickman, MS Suson, DJ Tajima, H Takahashi, H Tanaka, T Thayer, JB Thayer, JG Thompson, DJ Tibaldo, L Torres, DF Tosti, G Tramacere, A Uchiyama, Y Usher, TL Vasileiou, V Vilchez, N Vitale, V Waite, AP Wang, P Winer, BL Wood, KS Ylinen, T Ziegler, M Barber, SD Terndrup, DM AF Acciari, V. A. Aliu, E. Arlen, T. Aune, T. Bautista, M. Beilicke, M. Benbow, W. Boettcher, M. Boltuch, D. Bradbury, S. M. Buckley, J. H. Bugaev, V. Byrum, K. Cannon, A. Cesarini, A. Chow, Y. C. Ciupik, L. Cogan, P. Cui, W. Duke, C. Falcone, A. Finley, J. P. Finnegan, G. Fortson, L. Furniss, A. Galante, N. Gall, D. Gillanders, G. H. Godambe, S. Grube, J. Guenette, R. Gyuk, G. Hanna, D. Holder, J. Hui, C. M. Humensky, T. B. 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. Millis, J. Moriarty, P. Nagai, T. Ong, R. A. Otte, A. N. Pandel, D. Perkins, J. S. Pichel, A. 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. 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. Wood, M. Zitzer, B. Abdo, A. A. Ackermann, M. Ajello, M. Baldini, L. Ballet, J. Barbiellini, G. Bastieri, D. Baughman, B. M. Bechtol, K. Bellazzini, R. Berenji, B. Blandford, R. D. Bloom, E. D. Bonamente, E. Borgland, A. W. Bregeon, J. Brez, A. Brigida, M. Bruel, P. Burnett, T. H. Caliandro, G. A. Cameron, R. A. Caraveo, P. A. Casandjian, J. M. Cavazzuti, E. Cecchi, C. Celik, Oe Chekhtman, A. Cheung, C. C. Chiang, J. Ciprini, S. Claus, R. Cohen-Tanugi, J. Conrad, J. Cutini, S. Dermer, C. D. de Angelis, A. de Palma, F. do Couto e Silva, E. Drell, P. S. Drlica-Wagner, A. Dubois, R. Dumora, D. Farnier, C. Favuzzi, C. Fegan, S. J. Focke, W. B. Fortin, P. Frailis, M. Fukazawa, Y. Fusco, P. Gargano, F. Gasparrini, D. Gehrels, N. Germani, S. Giebels, B. Giglietto, N. Giommi, P. Giordano, F. Glanzman, T. Godfrey, G. Grenier, I. A. Grove, J. E. Guillemot, L. Guiriec, S. Hanabata, Y. Hays, E. Hughes, R. E. Jackson, M. S. Johannesson, G. Johnson, A. S. Johnson, W. N. Kamae, T. Katagiri, H. Kataoka, J. Kawai, N. Kerr, M. Knoedlseder, J. Kocian, M. L. Kuss, M. Lande, J. Latronico, L. Longo, F. Loparco, F. Lott, B. Lovellette, M. N. Lubrano, P. Madejski, G. M. Makeev, A. Mazziotta, M. N. McEnery, J. E. Meurer, C. Michelson, P. F. Mitthumsiri, W. Mizuno, T. Moiseev, A. A. Monte, C. Monzani, M. E. Morselli, A. Moskalenko, I. V. Murgia, S. Nolan, P. L. Norris, J. P. Nuss, E. Ohsugi, T. Omodei, N. Orlando, E. Ormes, J. F. Paneque, D. Parent, D. Pelassa, V. Pepe, M. Pesce-Rollins, M. Piron, F. Porter, T. A. Raino, S. Rando, R. Razzano, M. Reimer, A. Reimer, O. Reposeur, T. Rodriguez, A. Y. Roth, M. Ryde, F. Sadrozinski, H. F. -W. Sanchez, D. Sander, A. Parkinson, P. M. Saz Scargle, J. D. Sgro, C. Shaw, M. S. Siskind, E. J. Smith, P. D. Spandre, G. Spinelli, P. Strickman, M. S. Suson, D. J. Tajima, H. Takahashi, H. Tanaka, T. Thayer, J. B. Thayer, J. G. Thompson, D. J. Tibaldo, L. Torres, D. F. Tosti, G. Tramacere, A. Uchiyama, Y. Usher, T. L. Vasileiou, V. Vilchez, N. Vitale, V. Waite, A. P. Wang, P. Winer, B. L. Wood, K. S. Ylinen, T. Ziegler, M. Barber, S. D. Terndrup, D. M. CA VERITAS Collaboration Fermi LAT Collaboration TI DISCOVERY OF VERY HIGH ENERGY GAMMA RAYS FROM PKS 1424+240 AND MULTIWAVELENGTH CONSTRAINTS ON ITS REDSHIFT SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE BL Lacertae objects: individual (PKS 1424+240=VER J1427+237), gamma rays: observations ID BL-LACERTAE OBJECTS; LARGE-AREA TELESCOPE; BACKGROUND-RADIATION; SOURCE LIST; VERITAS; ASTRONOMY; EMISSION; SPECTRA; BLAZARS; MISSION AB We report the first detection of very high energy(83) (VHE) gamma-ray emission above 140 GeV from PKS 1424+240, a BL Lac object with an unknown redshift. The photon spectrum above 140 GeV measured by VERITAS is well described by a power law with a photon index of 3.8 +/- 0.5(stat) +/- 0.3(syst) and a flux normalization at 200 GeV of (5.1 +/- 0.9(stat) +/- 0.5(syst)) x 10(-11) TeV-1 cm(-2) s(-1), where stat and syst denote the statistical and systematical uncertainties, respectively. The VHE flux is steady over the observation period between MJD 54881 and 55003 (from 2009 February 19 to June 21). Flux variability is also not observed in contemporaneous high-energy observations with the Fermi Large Area Telescope. Contemporaneous X-ray and optical data were also obtained from the Swift XRT and MDM observatory, respectively. The broadband spectral energy distribution is well described by a one-zone synchrotron self-Compton model favoring a redshift of less than 0.1. Using the photon index measured with Fermi in combination with recent extragalactic background light absorption models it can be concluded from the VERITAS data that the redshift of PKS 1424+240 is less than 0.66. C1 [Aune, T.; Furniss, A.; Otte, A. N.; Williams, D. A.; Porter, T. A.; Sadrozinski, H. F. -W.; Parkinson, P. M. Saz; Ziegler, M.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 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.; Chow, Y. C.; Ong, R. A.; Vassiliev, V. V.; Weinstein, A.; Wood, M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Bautista, M.; Cogan, P.; Guenette, R.; Hanna, D.; Maier, G.; McCann, A.; McCutcheon, M.; Ragan, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Beilicke, M.; Buckley, J. H.; Bugaev, V.; Krawczynski, H.; McArthur, S.; Thibadeau, S.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Boettcher, M.] Ohio Univ, Inst Astrophys, Dept Phys & Astron, Athens, OH 45701 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.; Grube, J.; Quinn, J.; Ward, J. E.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Cesarini, A.; Gillanders, G. H.; Lang, M. J.] 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. [Cui, W.; Finley, J. P.; Gall, D.; Millis, J.; 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. [Falcone, A.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 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. [Humensky, T. B.; Swordy, S. P.; Wakely, S. P.; Weisgarber, T.; Wissel, S.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 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. [Krennrich, F.; Nagai, T.; Pohl, M.; Schroedter, M.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland. [Pichel, A.] Inst Astron & Fis Espacio, RA-1428 Buenos Aires, DF, Argentina. [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. [Abdo, A. A.; Chekhtman, A.; Dermer, C. D.; Grove, J. E.; Johnson, W. N.; Lovellette, M. N.; Makeev, A.; Strickman, M. S.; Wood, K. S.] USN, Div Space Sci, Res Lab, Washington, DC 20375 USA. [Abdo, A. A.] Natl Acad Sci, Natl Res Council Res Associate, Washington, DC 20001 USA. [Ackermann, M.; Ajello, M.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Cameron, R. A.; Chiang, J.; Claus, R.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Dubois, R.; Focke, W. B.; Glanzman, T.; Godfrey, G.; Johannesson, G.; Johnson, A. S.; Kamae, T.; Kocian, M. L.; Lande, J.; Madejski, G. M.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Paneque, D.; Reimer, A.; Reimer, O.; Shaw, M. S.; Tajima, H.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; 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.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Cameron, R. A.; Chiang, J.; Claus, R.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Dubois, R.; Focke, W. B.; Glanzman, T.; Godfrey, G.; Johannesson, G.; Johnson, A. S.; Kamae, T.; Kocian, M. L.; Lande, J.; Madejski, G. M.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Paneque, D.; Reimer, A.; Reimer, O.; Shaw, M. S.; Tajima, H.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; Waite, A. P.; Wang, P.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Baldini, L.; Bellazzini, R.; Bregeon, J.; Brez, A.; Kuss, M.; Latronico, L.; Omodei, N.; Pesce-Rollins, M.; Razzano, M.; Sgro, C.; Spandre, G.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Ballet, J.; Casandjian, J. M.; Grenier, I. A.; Tibaldo, L.] Univ Paris Diderot, Lab AIM, CEA Saclay, Serv Astrophys,CEA IRFU,CNRS, F-91191 Gif Sur Yvette, France. [Barbiellini, G.; Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy. [Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy. [Bastieri, D.; Rando, R.; Tibaldo, L.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy. [Bastieri, D.; Rando, R.; Tibaldo, L.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy. [Baughman, B. M.; Hughes, R. E.; Sander, A.; Smith, P. D.; Winer, B. L.] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Bonamente, E.; Cecchi, C.; Ciprini, S.; Germani, S.; Lubrano, P.; Pepe, M.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy. [Bonamente, E.; Cecchi, C.; Ciprini, S.; Germani, S.; Lubrano, P.; Pepe, M.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [Brigida, M.; Caliandro, G. A.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Univ Politecn Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy. [Brigida, M.; Caliandro, G. A.; de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Monte, C.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy. [Bruel, P.; Fegan, S. J.; Fortin, P.; Giebels, B.; Sanchez, D.] Ecole Polytech, CNRS, Lab Leprince Ringuet, IN2P3, F-91128 Palaiseau, France. [Burnett, T. H.; Kerr, M.; Roth, M.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy. [Cavazzuti, E.; Cutini, S.; Gasparrini, D.; Giommi, P.] ASI, Sci Data Ctr, I-00044 Rome, Italy. [Celik, Oe; Moiseev, A. A.; Vasileiou, V.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. [Celik, Oe; Vasileiou, V.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA. [Chekhtman, A.; Makeev, A.] George Mason Univ, Fairfax, VA 22030 USA. [Cohen-Tanugi, J.; Farnier, C.; Nuss, E.; Pelassa, V.; Piron, F.] Univ Montpellier 2, Lab Phys Theor & Astroparticules, CNRS, IN2P3, Montpellier, France. [Conrad, J.; Jackson, M. S.; Meurer, C.] Stockholm Univ, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden. [Conrad, J.; Jackson, M. S.; Meurer, C.; Ryde, F.; Ylinen, T.] AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden. [de Angelis, A.; Frailis, M.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy. [de Angelis, A.; Frailis, M.] Ist Nazl Fis Nucl, Sez Trieste, Grp Collegato Udine, I-33100 Udine, Italy. [Dumora, D.; Guillemot, L.; Lott, B.; Parent, D.; Reposeur, T.] Univ Bordeaux, Ctr Etud Nucl Bordeaux Gradignan, UMR 5797, F-33175 Gradignan, France. [Dumora, D.; Guillemot, L.; Lott, B.; Parent, D.; Reposeur, T.] CNRS, Ctr Etud Nucl Bordeaux Gradignan, IN2P3, UMR 5797, F-33175 Gradignan, France. [Fukazawa, Y.; Hanabata, Y.; Katagiri, H.; Mizuno, T.; Ohsugi, T.; Takahashi, H.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan. [Gehrels, N.; Moiseev, A. A.] Univ Maryland, College Pk, MD 20742 USA. [Guiriec, S.] Univ Alabama, Huntsville, AL 35899 USA. [Jackson, M. S.; Ryde, F.; Ylinen, T.] AlbaNova, Royal Inst Technol KTH, Dept Phys, SE-10691 Stockholm, Sweden. [Kataoka, J.; Kawai, N.] Tokyo Inst Technol, Dept Phys, Meguro, Tokyo 1528551, Japan. [Kataoka, J.] Waseda Univ, Shinjuku Ku, Tokyo 1698050, Japan. [Kawai, N.] Inst Phys & Chem Res RIKEN, Cosm Radiat Lab, Wako, Saitama 3510198, Japan. [Knoedlseder, J.; Vilchez, N.] CNRS UPS, Ctr Etud Spatiale Rayonnements, F-31028 Toulouse 4, France. [Morselli, A.; Vitale, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy. [Norris, J. P.; Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA. [Orlando, E.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Porter, T. A.; Sadrozinski, H. F. -W.; Parkinson, P. M. Saz; Ziegler, M.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria. [Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria. [Rodriguez, A. Y.; Torres, D. F.] Inst Ciencies Espai IEEC CSIC, Barcelona 08193, Spain. [Scargle, J. D.] NASA, Div Space Sci, Ames Res Ctr, Moffett Field, CA 94035 USA. [Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA. [Suson, D. J.] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA. [Torres, D. F.] Inst Catalana Recerca & Estudis Avancats, Barcelona, Spain. [Tramacere, A.] CIFS, I-10133 Turin, Italy. [Uchiyama, Y.] JAXA, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. [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. [Barber, S. D.] Univ Oklahoma, Homer L Dodge Dept Phys & Astron, Norman, OK 73019 USA. [Terndrup, D. M.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Terndrup, D. M.] Natl Sci Fdn, Arlington, VA 22230 USA. [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. RP Furniss, A (reprint author), Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA. EM nepomuk.otte@gmail.com; amy.furniss@gmail.com; jchiang@slac.stanford.edu RI Johannesson, Gudlaugur/O-8741-2015; Gargano, Fabio/O-8934-2015; Loparco, Francesco/O-8847-2015; Moskalenko, Igor/A-1301-2007; Mazziotta, Mario /O-8867-2015; Sgro, Carmelo/K-3395-2016; Torres, Diego/O-9422-2016; 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; Nolan, Patrick/A-5582-2009; Kuss, Michael/H-8959-2012; giglietto, nicola/I-8951-2012; Tosti, Gino/E-9976-2013; Rando, Riccardo/M-7179-2013; Hays, Elizabeth/D-3257-2012; Johnson, Neil/G-3309-2014; Reimer, Olaf/A-3117-2013; OI Johannesson, Gudlaugur/0000-0003-1458-7036; Gargano, Fabio/0000-0002-5055-6395; Loparco, Francesco/0000-0002-1173-5673; Moskalenko, Igor/0000-0001-6141-458X; Mazziotta, Mario /0000-0001-9325-4672; Torres, Diego/0000-0002-1522-9065; giommi, paolo/0000-0002-2265-5003; De Angelis, Alessandro/0000-0002-3288-2517; Cui, Wei/0000-0002-6324-5772; Frailis, Marco/0000-0002-7400-2135; Cesarini, Andrea/0000-0002-8611-8610; Caraveo, Patrizia/0000-0003-2478-8018; 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; Gasparrini, Dario/0000-0002-5064-9495; Tramacere, Andrea/0000-0002-8186-3793; Baldini, Luca/0000-0002-9785-7726; Sgro', Carmelo/0000-0001-5676-6214; SPINELLI, Paolo/0000-0001-6688-8864; Rando, Riccardo/0000-0001-6992-818X; Ward, John E/0000-0003-1973-0794; Bastieri, Denis/0000-0002-6954-8862; Omodei, Nicola/0000-0002-5448-7577; Pesce-Rollins, Melissa/0000-0003-1790-8018; Pandel, Dirk/0000-0003-2085-5586; Lang, Mark/0000-0003-4641-4201; Cutini, Sara/0000-0002-1271-2924 FU K. A. Wallenberg Foundation FX Royal Swedish Academy of Sciences Research Fellow, funded by a grant from the K. A. Wallenberg Foundation. NR 37 TC 44 Z9 44 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JAN 10 PY 2010 VL 708 IS 2 BP L100 EP L106 DI 10.1088/2041-8205/708/2/L100 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 540CJ UT WOS:000273308000007 ER PT J AU Zimmermann, B Zimmermann, A Lark, RM Elsenbeer, H AF Zimmermann, Beate Zimmermann, Alexander Lark, Richard Murray Elsenbeer, Helmut TI Sampling procedures for throughfall monitoring: A simulation study SO WATER RESOURCES RESEARCH LA English DT Article ID TROPICAL RAIN-FOREST; MIXED DECIDUOUS FOREST; GASH ANALYTICAL-MODEL; MARITIME PINE STAND; SPATIAL VARIABILITY; SIZE REQUIREMENTS; CHEMISTRY BENEATH; INTERCEPTION LOSS; WESTERN AMAZONIA; HARDWOOD FOREST AB What is the most appropriate sampling scheme to estimate event-based average throughfall? A satisfactory answer to this seemingly simple question has yet to be found, a failure which we attribute to previous efforts' dependence on empirical studies. Here we try to answer this question by simulating stochastic throughfall fields based on parameters for statistical models of large monitoring data sets. We subsequently sampled these fields with different sampling designs and variable sample supports. We evaluated the performance of a particular sampling scheme with respect to the uncertainty of possible estimated means of throughfall volumes. Even for a relative error limit of 20%, an impractically large number of small, funnel-type collectors would be required to estimate mean throughfall, particularly for small events. While stratification of the target area is not superior to simple random sampling, cluster random sampling involves the risk of being less efficient. A larger sample support, e.g., the use of trough-type collectors, considerably reduces the necessary sample sizes and eliminates the sensitivity of the mean to outliers. Since the gain in time associated with the manual handling of troughs versus funnels depends on the local precipitation regime, the employment of automatically recording clusters of long troughs emerges as the most promising sampling scheme. Even so, a relative error of less than 5% appears out of reach for throughfall under heterogeneous canopies. We therefore suspect a considerable uncertainty of input parameters for interception models derived from measured throughfall, in particular, for those requiring data of small throughfall events. C1 [Zimmermann, Beate; Elsenbeer, Helmut] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Zimmermann, Alexander; Elsenbeer, Helmut] Univ Potsdam, Inst Geoecol, D-14476 Potsdam, Germany. [Lark, Richard Murray] Rothamsted Res, W Common, Harpenden AL5 2JQ, Herts, England. RP Zimmermann, B (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama. EM zimmermannb@si.edu RI Zimmermann, Alexander/B-6831-2011; Zimmermann, Beate/B-5164-2012; Lark, Richard/G-6744-2012 OI Lark, Richard/0000-0003-2571-8521 FU The HSBC Climate Partnership, a partnership between HSBC and The Climate Group; Earthwatch Institute; Smithsonian Tropical Research Institute; WWF; German Research Foundation [E1 255/6-1]; German Academic Exchange Service (DAAD); U. K. Biotechnology and Biological Sciences Research Council FX This research was sponsored as part of The HSBC Climate Partnership, a partnership between HSBC and The Climate Group, Earthwatch Institute, Smithsonian Tropical Research Institute, and WWF. A.Z. and H. E. acknowledge support from the German Research Foundation (E1 255/6-1). B.Z. and H.E. acknowledge partial support by the German Academic Exchange Service (DAAD). R.M.L.'s input is part of the program for Mathematical and Computational Biology at Rothamsted Research, sponsored by the U. K. Biotechnology and Biological Sciences Research Council. We thank Luise Neumann-Cosel, Barbel Ehrig, Silja Hund, Anna Schurkmann, and Frank Base for participating in the field work. NR 71 TC 23 Z9 24 U1 3 U2 29 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0043-1397 J9 WATER RESOUR RES JI Water Resour. Res. PD JAN 6 PY 2010 VL 46 AR W01503 DI 10.1029/2009WR007776 PG 15 WC Environmental Sciences; Limnology; Water Resources SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water Resources GA 542QN UT WOS:000273509900002 ER PT S AU von Hippel, T Kilic, M Munn, J Williams, K Harris, H Thorstensen, J Liebert, J DeGennaro, S Jeffery, E Jefferys, B Stein, N van Dyk, D AF von Hippel, Ted Kilic, Mukremin Munn, Jeff Williams, Kurtis Harris, Hugh Thorstensen, John Liebert, Jim DeGennaro, Steven Jeffery, Elizabeth Jefferys, Bill Stein, Nathan van Dyk, David BE Werner, K Rauch, T TI Deriving the Age of an Individual WD: SDSS, Bok, USNO, and Bayes SO 17TH EUROPEAN WHITE DWARF WORKSHOP SE AIP Conference Proceedings LA English DT Proceedings Paper CT 17th European White Dwarf Workshop CY AUG 16-20, 2010 CL Tubingen, GERMANY SP German Res Fdn, Univ Tubingen DE stellar ages; white dwarfs; Bayesian statistics ID DIGITAL-SKY-SURVEY; DWARF LUMINOSITY FUNCTION; COLOR-MAGNITUDE DIAGRAMS; STAR CLUSTER PARAMETERS; COOL WHITE-DWARFS; STELLAR EVOLUTION; ISOCHRONES; MODELS AB We report on ancient white dwarfs found in the proper motion survey we are conducting at the Bok and USNO telescopes. To date we have surveyed approximately 2800 square degrees of sky and identified numerous WDs with Teff <= 6000. A subset of these WDs are high velocity objects that most likely belong to the Galactic halo population. Where possible, we are acquiring trigonometric parallaxes to constrain the WD masses. We apply a new Bayesian modeling approach to these WDs that consistently incorporates precursor evolutionary timescales, the initial-final mass relation, WD interior and atmosphere models, and uses the observed magnitudes, distances, etc. to derive the distribution of WD age as a function of uncertainties in the observational parameters. C1 [von Hippel, Ted] Siena Coll, Loudonville, NY 12211 USA. [von Hippel, Ted; Williams, Kurtis; DeGennaro, Steven; Jefferys, Bill] Univ Texas Austin, Austin, TX 78712 USA. [Kilic, Mukremin] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Munn, Jeff] Dartmouth Coll, Hanover, NH 03755 USA. [Liebert, Jim] Univ Arizona, Tucson, AZ 85721 USA. [Jeffery, Elizabeth] Space Telescope Sci Inst, Baltimore, MD 37000 USA. [Jefferys, Bill] Univ Vermont, Burlington, VT 05405 USA. [Stein, Nathan] Harvard Univ, Cambridge, MA 02138 USA. [van Dyk, David] Univ Calif Irvine, Irvine, CA 92717 USA. [Harris, Hugh] US Naval Observ, Washington, DC 20392 USA. RP von Hippel, T (reprint author), Siena Coll, Loudonville, NY 12211 USA. OI Williams, Kurtis/0000-0002-1413-7679 FU National Aeronautics and Space Administration through Office of Space Science [NAG5-13070]; National Science Foundation [AST-0307315, AST-0607480] FX This material is based upon work supported by the National Aeronautics and Space Administration under Grant No. NAG5-13070 issued through the Office of Space Science. This material is also based on work supported by the National Science Foundation under grants AST-0307315 and AST-0607480. NR 14 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0823-4 J9 AIP CONF PROC PY 2010 VL 1273 BP 141 EP 145 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BTK36 UT WOS:000287165200029 ER PT S AU Hoard, DW Debes, JH Wachter, S Leisawitz, DT Cohen, M AF Hoard, D. W. Debes, J. H. Wachter, S. Leisawitz, D. T. Cohen, M. BE Werner, K Rauch, T TI The WISE InfraRed Excesses around Degenerates (WIRED) Survey SO 17TH EUROPEAN WHITE DWARF WORKSHOP SE AIP Conference Proceedings LA English DT Proceedings Paper CT 17th European White Dwarf Workshop CY AUG 16-20, 2010 CL Tubingen, GERMANY SP German Res Fdn, Univ Tubingen ID WHITE-DWARFS; CATALOG AB The Wide-field Infrared Survey Explorer (WISE) is a NASA medium class Explorer mission that performed an all sky survey in four infrared bands. We present an overview of the WISE InfraRed Excesses around Degenerates (WIRED) Survey, which has the goals of characterizing white dwarf stars in the WISE bands, confirming objects known to have infrared excess from past observations, and revealing new examples of white dwarfs with infrared excess that can be attributed to unresolved companions or debris disks. We obtained preliminary WISE detections (S/N > 2) in at least one band of 405 white dwarfs from the 9316 unique possible targets in the Sloan Digital Sky Survey Data Release 4 Catalog of Spectroscopically Identified White Dwarfs (not all potential targets were available in the sky coverage used here). A companion paper in this volume discusses specific results from our target detections. C1 [Hoard, D. W.; Wachter, S.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Hoard, D. W.; Leisawitz, D. T.] Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Smithsonian Astrophy Observ, Cambridge, MA 02138 USA. [Wachter, S.] CALTECH, IPAC, Pasadena, CA 91125 USA. [Cohen, M.] Monterey Res Astronom, Marina Del Rey, CA 93933 USA. RP Hoard, DW (reprint author), CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. FU NASA; UKIRT Infrared Deep Sky Survey (UKIDSS); Two Micron All Sky Survey (2MASS); NSF; Sloan DigitalSky Survey (SDSS); Alfred P.Sloan Foundation; U.S.Dept. of Energy, NASA; apanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England FX This work is based on data from: WISE, which is a joint project of the University of California, LosAngeles, and the Jet Propulsion Laboratory (JPL), California Institute of Technology (Caltech), funded by NASA; the UKIRT Infrared Deep Sky Survey (UKIDSS); the Two Micron All Sky Survey (2MASS), a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center(IPAC)/Caltech,funded by NASA and the NSF; and the Sloan DigitalSky Survey (SDSS). Funding for the SDSS and SDSS-II was provided by the Alfred P.Sloan Foundation, the Participating Institution, the NSF, the U.S.Dept. of Energy, NASA, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. We used the SIMBAD database, operated at CDS, Strasbourg, France, and the NASA/IPAC Infrared Science Archive, operated by JPL, Caltech, under a contract with NASA. NR 11 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0823-4 J9 AIP CONF PROC PY 2010 VL 1273 BP 170 EP 173 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BTK36 UT WOS:000287165200035 ER PT S AU Adamczak, J Werner, K Rauch, T Schuh, S Drake, JJ Kruk, JW AF Adamczak, J. Werner, K. Rauch, T. Schuh, S. Drake, J. J. Kruk, J. W. BE Werner, K Rauch, T TI Analysis of Chandra-LETG spectra of two DA white dwarfs and a PG 1159 star SO 17TH EUROPEAN WHITE DWARF WORKSHOP SE AIP Conference Proceedings LA English DT Proceedings Paper CT 17th European White Dwarf Workshop CY AUG 16-20, 2010 CL Tubingen, GERMANY SP German Res Fdn, Univ Tubingen DE White dwarfs; Stars: Individual: LB 1919; GD 246; Chandra; X-ray spectroscopy; PG 1159 stars; Individual Objects: PG 1520+525 ID ABUNDANCES AB We present results of model-atmosphere analyses of soft X-ray spectra of three hot WDs. These are the relatively iron-rich DA GD246, the surprisingly metal-poor DA LB 1919, and the H-deficient PG1159-type star PG1520+525. The two DAs are modeled with chemically stratified and with homogeneous NLTE models in order to constrain metal abundances. FUSE and HST spectra are also employed. For the PG 1159 star the effective temperature can be constrained to a precision that is not attained with optical and UV spectroscopy alone. C1 [Adamczak, J.; Werner, K.; Rauch, T.] Univ Tubingen, Inst Astron & Astrophys, Kepler Ctr Astro & Particle Phys, D-72076 Tubingen, Germany. [Schuh, S.] Univ Gottingen, Gottingen, Germany. [Drake, J. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. [Kruk, J. W.] NASA, Goddard Space Flight Ctr, Washington, DC USA. RP Adamczak, J (reprint author), Univ Tubingen, Inst Astron & Astrophys, Kepler Ctr Astro & Particle Phys, D-72076 Tubingen, Germany. EM adamczak@astro.uni-tuebingen.de; werner@astro.uni-tuebingen.de; rauch@astro.uni-tuebingen.de; schuh@astro.physik.uni-goettingen.de RI Kruk, Jeffrey/G-4047-2012 NR 13 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0823-4 J9 AIP CONF PROC PY 2010 VL 1273 BP 406 EP 411 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BTK36 UT WOS:000287165200084 ER PT S AU Kowalski, PM Kilic, M Pavlov, GG AF Kowalski, Piotr M. Kilic, Mukremin Pavlov, George G. BE Werner, K Rauch, T TI Ab initio Stellar Astrophysics: Reliable Modeling of Cool White Dwarf Atmospheres SO 17TH EUROPEAN WHITE DWARF WORKSHOP SE AIP Conference Proceedings LA English DT Proceedings Paper CT 17th European White Dwarf Workshop CY AUG 16-20, 2010 CL Tubingen, GERMANY SP German Res Fdn, Univ Tubingen DE white dwarfs; stars: atmopsheres ID DIGITAL-SKY-SURVEY AB Over the last decade ab initio modeling of material properties has become widespread in diverse fields of research. It has proved to be a powerful tool for predicting various properties of matter under extreme conditions. We apply modern computational chemistry and materials science methods, including density functional theory (DFT), to solve lingering problems in the modeling of the dense atmospheres of cool white dwarfs (T-eff < 7000 K). Our work on the revision and improvements of the absorption mechanisms in the hydrogen and helium dominated atmospheres resulted in a new set of atmosphere models. By inclusion of the Ly-alpha red wing opacity we successfully fitted the entire spectral energy distributions of known cool DA stars. In the subsequent work we fitted the majority of the coolest stars with hydrogen-rich models. This finding challenges our understanding of the spectral evolution of cool white dwarfs. We discuss a few examples, including the cool companion to the pulsar PSR J0437-4715. The two problems important for the understanding of cool white dwarfs are the behavior of negative hydrogen ion and molecular carbon in a fluid-like, helium dominated medium. Using ab initio methods we investigate the stability and opacity of these two species in dense helium. Our investigation of C-2 indicates that the absorption features observed in the "peculiar" DQp white dwarfs resemble the absorption of perturbed C-2 in dense helium. C1 [Kowalski, Piotr M.] GFZ German Res Ctr Geosci, Helmholtz Ctr Potsdam, D-14473 Potsdam, Germany. [Kilic, Mukremin] Smithsonian Astrophys Observat, Cambridge, MA 02138 USA. [Pavlov, George G.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. RP Kowalski, PM (reprint author), GFZ German Res Ctr Geosci, Helmholtz Ctr Potsdam, D-14473 Potsdam, Germany. EM kowalski@gfz-potsdam.de; mkilic@cfa.harvard.edu RI Kowalski, Piotr/L-7411-2013 OI Kowalski, Piotr/0000-0001-6604-3458 NR 21 TC 1 Z9 1 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0823-4 J9 AIP CONF PROC PY 2010 VL 1273 BP 418 EP 423 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BTK36 UT WOS:000287165200086 ER PT S AU Debes, JH Kilic, M AF Debes, J. H. Kilic, M. BE Werner, K Rauch, T TI Results from a Magellan Spectroscopic DAZ Monitoring Campaign SO 17TH EUROPEAN WHITE DWARF WORKSHOP SE AIP Conference Proceedings LA English DT Proceedings Paper CT 17th European White Dwarf Workshop CY AUG 16-20, 2010 CL Tubingen, GERMANY SP German Res Fdn, Univ Tubingen DE circumstellar material; white dwarfs; spectroscopy ID COOL WHITE-DWARFS; METAL ABUNDANCE PATTERNS; ACCRETION; DISKS AB The MIKE optical spectrograph on the Magellan Telescopes is a powerful instrument for detecting and monitoring the faint metal lines present in nearby DAZ white dwarfs. With a spectral resolution of 30,000 and spectra with S/N>20 that cover from 3500 angstrom to 9500 angstrom, we can both monitor the Ca H and K lines as well as search for other metal lines of Mg and Fe. We present monitoring of 30 southern DAZs for variability in their Ca H and K lines, presenting some of our strongest candidates for variability. In addition to these white dwarfs, we have searched other white dwarfs for evidence of metal line absorption. In the process we have found two new DAZs that reside within 15 pc. C1 [Debes, J. H.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kilic, M.] Smithsonian Astrophys Observ, Cambridge, MA USA. RP Debes, JH (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NR 16 TC 2 Z9 2 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0823-4 J9 AIP CONF PROC PY 2010 VL 1273 BP 488 EP 491 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BTK36 UT WOS:000287165200101 ER PT J AU Phillips, JD Popescu, EM Reasenberg, RD Rocco, E Thapa, R AF Phillips, J. D. Popescu, E. M. Reasenberg, R. D. Rocco, E. Thapa, R. GP IEEE TI Demonstration of Semiconductor Laser Tracking Frequency Distance Gauge SO 2010 CONFERENCE ON LASERS AND ELECTRO-OPTICS (CLEO) AND QUANTUM ELECTRONICS AND LASER SCIENCE CONFERENCE (QELS) LA English DT Proceedings Paper CT Conference on Lasers and Electro-Optics (CLEO)/Quantum Electronics and Laser Science Conference (QELS) CY MAY 16-21, 2010 CL San Jose, CA AB We present results from the Semiconductor-Laser Tracking Frequency distance Gauge having Allan deviation of 5 pm. The simple and rugged SL-TFG will achieve sub-pm accuracy. It is required for space-based astronomical instruments and gravitational experiments. C1 [Phillips, J. D.; Popescu, E. M.; Reasenberg, R. D.; Rocco, E.; Thapa, R.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Phillips, JD (reprint author), Smithsonian Astrophys Observ, MS63,60 Garden St, Cambridge, MA 02138 USA. EM jphillips@cfa.harvard.edu RI Popescu, Eugeniu/B-7342-2012 NR 6 TC 0 Z9 0 U1 0 U2 2 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 978-1-55752-890-2 PY 2010 PG 2 WC Engineering, Electrical & Electronic; Optics; Physics, Applied SC Engineering; Optics; Physics GA BUW45 UT WOS:000290513600223 ER PT B AU Narayan, R Tchekhovskoy, A McKinney, J AF Narayan, Ramesh Tchekhovskoy, Alexander McKinney, Jonathan BE Maraschi, L Ghisellini, G DellaCeca, R Tavecchio, F TI Numerical Studies of Relativistic Jets SO ACCRETION AND EJECTION IN AGN : A GLOBAL VIEW SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Conference on Accretion and Ejection in AGN: A Global View CY JUN 22-26, 2009 CL Como, ITALY SP Insubria Univ, Phys Dept, Brera Astronom Observ, Natl Inst Astrophys, Giovanni Pareschi ID RAY BURST OUTFLOWS; BLACK-HOLE; ALFVENIC SOLUTIONS; ACCRETION DISK; SIMULATIONS; MAGNETOHYDRODYNAMICS; ENERGY; MAGNETOSPHERE; ACCELERATION; SCHEME AB The connection between collimation and acceleration of magnetized relativistic jets is discussed. The focus is on recent numerical simulations which shed light on some longstanding problems. C1 [Narayan, Ramesh; Tchekhovskoy, Alexander] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [McKinney, Jonathan] Stanford Univ, Kavli Inst Particle Astrophys & Cosmology, Stanford, CA 94305 USA. RP Narayan, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU NASA [NNX08AH32G]; NSF [NSF AST-0805832]; Harvard FAS Research Computing Group FX This work was supported in part by NASA grant NNX08AH32G and NSF grant NSF AST-0805832. The simulations were run on the Odyssey cluster supported by the Harvard FAS Research Computing Group and on the TeraGrid resources (Catlett et al. 2007) provided by the Louisiana Optical Network Initiative (http://www.loni.org) with the support of NSF. NR 36 TC 3 Z9 3 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-734-6 J9 ASTR SOC P PY 2010 VL 427 BP 127 EP + PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BUO06 UT WOS:000289881400028 ER PT B AU Beilicke, M Baring, MC De Geronimo, C Dowkontt, P Garson, A Grindlay, J Harding, AK Hong, JS Krawczynski, H Kurfess, J Li, Q Martin, J Novikova, EI Wulf, EA AF Beilicke, M. Baring, M. C. De Geronimo, C. Dowkontt, P. Garson, A., III Grindlay, J. Harding, A. K. Hong, J. S. Krawczynski, H. Kurfess, J. Li, Q. Martin, J. Novikova, E. I. Wulf, E. A. BE Maraschi, L Ghisellini, G DellaCeca, R Tavecchio, F TI HX-POL - A Balloon-Borne Hard X-Ray Polarimeter SO ACCRETION AND EJECTION IN AGN : A GLOBAL VIEW SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Conference on Accretion and Ejection in AGN: A Global View CY JUN 22-26, 2009 CL Como, ITALY SP Insubria Univ, Phys Dept, Brera Astronom Observ, Natl Inst Astrophys, Giovanni Pareschi AB The design and estimated performance of a balloon-borne hard Xray polarimeter called HX-POL is reported. The experiment uses a combination of Si and Cadmium Zinc Telluride (CZT) detectors to measure the polarization of 50 500 keV X-rays through the dependence of the angular distribution of Compton scattered photons on the polarization direction. On a 15-30-day balloon flight, HX-POL would allow one to measure the polarization of bright Crab-like sources for polarization degrees down to a, few %. Hard X-ray polarization measurements provide unique venues for the study of particle acceleration processes by compact objects and relativistic outflows. C1 [Beilicke, M.; Dowkontt, P.; Garson, A., III; Krawczynski, H.; Li, Q.; Martin, J.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Kurfess, J.] Praxis Inc, Alexandria, VA 22303 USA. [De Geronimo, C.] Brookhaven Natl Lab, Instrumentat Div, Upton, NY 11973 USA. [Baring, M. C.] Rice Univ, Dept Phys & Astron, Houston, TX USA. [Harding, A. K.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20770 USA. [Grindlay, J.; Hong, J. S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Beilicke, M (reprint author), Washington Univ, Dept Phys, St Louis, MO 63130 USA. RI Wulf, Eric/B-1240-2012; Harding, Alice/D-3160-2012 FU NASA [NNX07AH37G] FX The Washington University group acknowledges support by NASA (grant NNX07AH37G). NR 5 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-734-6 J9 ASTR SOC P PY 2010 VL 427 BP 187 EP + PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BUO06 UT WOS:000289881400039 ER PT B AU Siemiginowska, A Czerny, B Janiuk, A Stawarz, L Guainazzi, M Celotti, A Migliori, G Tengstrand, O AF Siemiginowska, Aneta Czerny, Bozena Janiuk, Agnieszka Stawarz, Lukasz Guainazzi, Matteo Celotti, Annalisa Migliori, Giulia Tengstrand, Olaf BE Maraschi, L Ghisellini, G DellaCeca, R Tavecchio, F TI Intermittent Activity of Jets in AGN SO ACCRETION AND EJECTION IN AGN : A GLOBAL VIEW SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Conference on Accretion and Ejection in AGN: A Global View CY JUN 22-26, 2009 CL Como, ITALY SP Insubria Univ, Phys Dept, Brera Astronom Observ, Natl Inst Astrophys, Giovanni Pareschi ID RADIATION PRESSURE INSTABILITY; COMPACT SYMMETRIC OBJECTS; MICROQUASAR GRS 1915+105; X-RAY JET; GALACTIC NUCLEI; RADIO GALAXIES; ACCRETION DISK; BLACK-HOLES; QUASAR; EVOLUTION AB Large scale X-ray jets that extend to > 100 kpc distances from the host galaxy indicate the importance of jets interactions with the environment on many different physical scales. Morphology of X-ray clusters indicate that the radio-jet activity of a cD galaxy is intermittent. This intermittency might be a result of a feedback and/or interactions between galaxies within the cluster. Here we consider the radiation pressure instability operating on short timescales (< 10(5) years) as the origin of the intermittent behaviour. We test whether this instability can be responsible for short ages (< 10(4) years) of Compact Symmetric Objects measured by hot spots propagation velocities in VLBI observations. We model the accretion disk evolution and constrain model parameters that may explain the observed compact radio structures and over-abundance of GPS sources. We also describe effects of consequent outbursts. C1 [Siemiginowska, Aneta] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Czerny, Bozena; Janiuk, Agnieszka] Copernicus Astron Ctr, PL-00716 Warsaw, Poland. [Stawarz, Lukasz] Stanford Univ, KAVLI, Stanford, CA 94305 USA. [Guainazzi, Matteo; Tengstrand, Olaf] ESA, European Space Astron, E-28691 Madrid, Spain. [Celotti, Annalisa; Migliori, Giulia] SISSA ISAS, I-34151 Trieste, Italy. RP Siemiginowska, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Czerny, Bozena/A-2363-2015 OI Czerny, Bozena/0000-0001-5848-4333 FU NASA [NAS8-39073, GO5-6113X, GO8-9125A, NNX07AQ55G] FX AS thanks the organizers for the invitation to the meeting. This research is funded in part by NASA contract NAS8-39073. Partial support for this work was provided by the NASA grants GO5-6113X, GO8-9125A and NNX07AQ55G. NR 33 TC 2 Z9 2 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-734-6 J9 ASTR SOC P PY 2010 VL 427 BP 326 EP + PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BUO06 UT WOS:000289881400076 ER PT B AU Singh, V Shastri, P Risaliti, G Athreya, R AF Singh, Veeresh Shastri, Prajval Risaliti, Guido Athreya, Ramana BE Maraschi, L Ghisellini, G DellaCeca, R Tavecchio, F TI Radio and X-ray Emission from Low-Luminosity AGNs: Testing Unification Hypothesis SO ACCRETION AND EJECTION IN AGN : A GLOBAL VIEW SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Conference on Accretion and Ejection in AGN: A Global View CY JUN 22-26, 2009 CL Como, ITALY SP Insubria Univ, Phys Dept, Brera Astronom Observ, Natl Inst Astrophys, Giovanni Pareschi AB We investigate the low-frequency radio properties and the X-ray spectral properties of a sample of Seyfert galaxies in order to compare the two subtypes of Seyferts and rigorously test the predictions of Seyfert unification. C1 [Singh, Veeresh; Shastri, Prajval] Indian Inst Astrophys, Bangalore 560034, Karnataka, India. [Risaliti, Guido] Ist Nazl Fis Nucl, Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Risaliti, Guido] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Athreya, Ramana] Natl Ctr Radio Astrophys, Pune 411007, Maharashtra, India. RP Singh, V (reprint author), Indian Inst Astrophys, Bangalore 560034, Karnataka, India. NR 4 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-734-6 J9 ASTR SOC P PY 2010 VL 427 BP 391 EP + PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BUO06 UT WOS:000289881400089 ER PT J AU Ehrenfreund, P Peter, N Schrogl, KU Logsdon, JM AF Ehrenfreund, P. Peter, N. Schrogl, K. U. Logsdon, J. M. TI Cross-cultural management supporting global space exploration SO ACTA ASTRONAUTICA LA English DT Article DE Cross-cultural management; Space policy; Space exploration; International cooperation; Cultural dimension AB A new era of space exploration has begun that may soon expand into a global endeavor mainly driven by socio-economic motives. Currently the main space powers, namely the United States, Russia, Europe, Japan, Canada as well as new rising space powers China and India, are pursuing national exploration programs to explore robotically and later with humans the Earth-Moon-Mars space. New axes of partnerships and cooperation mechanisms have emerged in the last decades. However, in order to achieve highly ambitious goals such as establishing human bases on the Moon, journeys to Mars and the construction of new infrastructures in space, international space cooperation has to be optimized to reduce costs and reap the benefits of worldwide expertise. Future ambitious space exploration endeavors are a long-term undertaking that Could influence countries to look beyond their own interests and see the advantages that a larger program can bring. This paper provides new concepts for managing global space exploration in the framework of cross-cultural management, an element often neglected in the planning of future partnerships. Published by Elsevier Ltd. C1 [Ehrenfreund, P.; Logsdon, J. M.] George Washington Univ, Elliott Sch Int Affairs, Inst Space Policy, Washington, DC 20052 USA. [Peter, N.; Schrogl, K. U.] ESPI, A-1030 Vienna, Austria. [Logsdon, J. M.] Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20013 USA. RP Ehrenfreund, P (reprint author), George Washington Univ, Elliott Sch Int Affairs, Inst Space Policy, 1957 E St,Suite 403, Washington, DC 20052 USA. EM pehren@gwu.edu FU NASA [NNX08AG78G]; NASA Astrobiology Institute NAI FX PE is supported by NASA Grant NNX08AG78G and the NASA Astrobiology Institute NAI. NR 17 TC 6 Z9 6 U1 1 U2 4 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 JAN-FEB PY 2010 VL 66 IS 1-2 BP 245 EP 256 DI 10.1016/j.actaastro.2009.05.030 PG 12 WC Engineering, Aerospace SC Engineering GA 526PT UT WOS:000272305000025 ER PT J AU Nataf, DM Stanek, KZ Bakos, GA AF Nataf, D. M. Stanek, K. Z. Bakos, G. A. TI HAT Discovery of 76 Bright Periodic Variable Stars Toward the Galactic Bulge SO ACTA ASTRONOMICA LA English DT Article DE Techniques: photometric; Galaxy: bulge; Stars: variables: general ID GRAVITATIONAL LENSING EXPERIMENT; SKY AUTOMATED SURVEY; INTERSTELLAR EXTINCTION LAW; RED CLUMP STARS; 8.0 MU-M; MICROLENSING EVENTS; IMAGE SUBTRACTION; SOUTHERN-HEMISPHERE; ECLIPSING BINARIES; SPECTRAL-ANALYSIS AB We report on photometric I-band observations of 147 bright (8 < I < 13) periodic variable stars toward the Galactic bulge including 76 new discoveries. We used one of the HATnet telescopes to obtain 151 exposures spanning 88 nights in 2005 of an 8 degrees 4 x 8 degrees 4 field of view (FOV) approximately centered on (l,b) = (1.73, -4.68). We observed the Galactic bulge in 2005 as part of a microlensing feasibility study, and here we discuss the periodic variable stars we found in our data. Among our discoveries we count 52 new eclipsing binaries and 24 other periodic variable stars. C1 [Nataf, D. M.; Stanek, K. Z.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Bakos, G. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Nataf, DM (reprint author), Ohio State Univ, Dept Astron, 140 W 18th Ave, Columbus, OH 43210 USA. EM nataf@astronomy.ohio-state.edu; kstanek@astronomy.ohio-state.edu; gbakos@cfa.harvard.edu FU NSF [AST-0757888]; NASA [NEG04GN74G, NNX 08AF23G] FX DMN is partially supported by the NSF grant No. AST-0757888. HATNet operations have been funded by NASA grants NEG04GN74G, NNX 08AF23G and SAO IRandD grants. We thank J.D. Hartman for assistance with use of the VARTOOLS package, and G. Pojmanski for his "lc" program. We made use of the Simbad database, operated in Strasbourg, France by the Centre de Donnees astronomiques de Strasbourg. NR 53 TC 6 Z9 6 U1 0 U2 1 PU COPERNICUS FOUNDATION POLISH ASTRONOMY PI WARSAW PA AL UJAZDOWSKIE 4, 00-478 WARSAW, POLAND SN 0001-5237 J9 ACTA ASTRONOM JI Acta Astron. PY 2010 VL 60 IS 3 BP 261 EP 282 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 663WM UT WOS:000282920900006 ER PT J AU Rutkowski, A Olech, A Poleski, R Sobolewska, M Kankiewicz, P Ak, T Boyd, D AF Rutkowski, A. Olech, A. Poleski, R. Sobolewska, M. Kankiewicz, P. Ak, T. Boyd, D. TI 2009 Superoutburst of Dwarf Nova 1RXS J053234.9+624755 SO ACTA ASTRONOMICA LA English DT Article DE Accretion, accretion disks; novae, cataclysmic variables; Stars: dwatf novae; Stars: individual: 1RXS J053234.9+624755 ID QUASI-PERIODIC OSCILLATIONS; VARIABLES EXPERIMENT CURVE; CATACLYSMIC VARIABLES; HOT-SPOT; VW-HYI; Z-CHA; SUPERHUMPS AB We present photometric observations of the dwarf nova 1RXS J053234.9+624755. We performed a detailed analysis of the superoutburst that occurred in August 2009. We found the superhump period to be P-sh = 0.057122(14)days. Based on the O-C diagram we conclude that P-sh increased during the plateau at the rate of dP(sh)/dt = (9.24 +/- 1.4). 10(-5). Both the O-C analysis and evolution of the superhumps light curve favor the model in which superhumps originate in a variable source located in the vicinity of the hot spot. In addition, the evolution of the light curve suggests that the superhump light source approaches the disk plane as the superoutburst declines. Detailed analysis of the superoutburst plateau phase enabled us to detect a signal which we interpret as apsidal motion of the accretion disk. We detected additional modulations during the final stage of the superoutburst characterized by periods of 104 s and 188 s which we tentatively interpret as quasi periodic oscillations. Estimations of A(0) and A(n) are in agreement with the dependence between the amplitude of superhumps and the orbital inclination. C1 [Rutkowski, A.; Ak, T.] TUBITAK Natl Observ, TR-07058 Antalya, Turkey. [Olech, A.] Polish Acad Sci, Nicholas Copernicus Astron Ctr, PL-00716 Warsaw, Poland. [Poleski, R.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. [Sobolewska, M.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Sobolewska, M.] Fdn Res & Technol Hellas, IESL, Iraklion 71110, Crete, Greece. [Sobolewska, M.] Univ Crete, Dept Phys, Iraklion 71003, Crete, Greece. [Kankiewicz, P.] Jan Kochanowski Univ Humanities & Sci, Inst Phys, Div Astrophys, PL-25406 Kielce, Poland. [Ak, T.] Istanbul Univ, Fac Sci, Dept Astron & Space Sci, TR-34119 Istanbul, Turkey. [Boyd, D.] British Astron Assoc, Variable Star Sect, W Challow OX12 9TX, England. RP Rutkowski, A (reprint author), TUBITAK Natl Observ, Akdeniz Univ Campus, TR-07058 Antalya, Turkey. EM artur@tug.tubitak.gov.tr FU Polish MNiSW [N203 301 335]; TUBITAK FX This work was partly supported by the Polish MNiSW grant no. N203 301 335. Artur Rutkowski has been supported by 2221-Visiting Scientist Fellowship Program of TUBITAK. AR is also grateful to Prof. Zelci Eker for inspiring discussions. Skinakas Observatory is a collaborative project of the University of Crete and the Foundation for Research and Technology-Hellas. We would like to thank the Skinakas Observatory staff for their help and assistance. NR 27 TC 2 Z9 2 U1 0 U2 2 PU COPERNICUS FOUNDATION POLISH ASTRONOMY PI WARSAW PA AL UJAZDOWSKIE 4, 00-478 WARSAW, POLAND SN 0001-5237 J9 ACTA ASTRONOM JI Acta Astron. PY 2010 VL 60 IS 4 BP 337 EP 355 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 714AV UT WOS:000286780100003 ER PT J AU Pecio, A Burns, JR Weitzman, SH AF Pecio, Anna Burns, John R. Weitzman, Stanley H. TI Modifications for insemination in the male reproductive system in Gladulocaudinae and Stevardiinae (Teleostei: Characiformes: Characidae) SO ACTA BIOLOGICA CRACOVIENSIA SERIES BOTANICA LA English DT Meeting Abstract C1 [Pecio, Anna] Jagiellonian Univ, Inst Zool, PL-30060 Krakow, Poland. [Burns, John R.] George Washington Univ, Dept Biol Sci, Washington, DC 20052 USA. [Weitzman, Stanley H.] Smithsonian Inst, Natl Museum Nat Hist, Dept Zool, Washington, DC 20560 USA. EM anna.pecio@uj.edu.pl NR 4 TC 0 Z9 0 U1 0 U2 0 PU POLSKA AKAD NAUK PI KRAKOW PA ODDZIAL W KRAKOWIE UL, SLAWKOWSKA 17, 31-018 KRAKOW, POLAND SN 0001-5296 J9 ACTA BIOL CRACOV BOT JI Acta Biol. Crac. Ser. Bot. PY 2010 VL 52 SU 1 BP 33 EP 33 PG 1 WC Plant Sciences SC Plant Sciences GA 669YT UT WOS:000283386900022 ER PT J AU Kawai, K Fukui, D Sato, M Harada, M Maeda, K AF Kawai, Kuniko Fukui, Dai Sato, Masahiko Harada, Masashi Maeda, Kishio TI Vespertilio murinus Linnaeus, 1758 confirmed in Japan from morphology and mitochondrial DNA SO ACTA CHIROPTEROLOGICA LA English DT Article DE Vespertilio murinus; mtDNA; cytochrome-b; ND1; migration; occurrence; Japan ID BATS; PHYLOGENIES; SEQUENCES; RABIES AB In December 2005, three bats of indeterminate identity were captured in northern Japan. Their forearm lengths were slightly smaller than the average for Vespertilio sinensis. We identified these three individuals as V murinus using both morphological and molecular approaches, and discussed their possible migration or vagrancy routes. Prior to the first record of V murinus on Rebun Island near Hokkaido in 2002, there was no record of this species in Japan. These new occurrences illustrate the importance of determining possible migration or vagrancy routes of bats for understanding and preventing the spread of zoonotic diseases. C1 [Kawai, Kuniko] Hokkaido Univ, Field Sci Ctr No Biosphere, Sapporo, Hokkaido, Japan. [Kawai, Kuniko] Smithsonian Inst, Div Mammals, Natl Museum Nat Hist, Washington, DC 20560 USA. [Fukui, Dai] Hokkaido Res Ctr, Forestry & Forest Prod Res Inst, Sapporo, Hokkaido, Japan. [Sato, Masahiko] Rishiri Town Museum, Rishiri Isl, Hokkaido, Japan. [Harada, Masashi] Osaka City Univ, Lab Anim Ctr, Grad Sch Med, Abeno Ku, Osaka 558, Japan. [Maeda, Kishio] Nara Univ Educ, Ctr Nat Environm Educ, Nara, Japan. RP Kawai, K (reprint author), Hokkaido Univ, Field Sci Ctr No Biosphere, Sapporo, Hokkaido, Japan. EM kkawai@fsc.hokudai.ac.jp RI Fukui, Dai/D-6100-2013 FU JSPS [PD08885]; KAKENHI [20710180] FX We thank Yasushi Niimura and Sayako Hikosaka (Haboro Ranger office, Hokkaido Regional Environment office, Ministry of the Environment), Takuya Ishigooka and Eri Ishikawa (Hokkaido Seabird Center), Mihoko Sato (Friends of Hokkaido Seabird Center), Shigeki Sakakibara (Kitahiroshima High School) and Hideo Shintani for providing information and samples. We are grateful to Kyle Armstrong, Lazaro M. Echenique-Diaz, and Kristofer Helgen for comments and English proofreading. This work was supported by JSPS Research Fellowships (Grant-in-Aid No. PD08885) and KAKENHI (Grant-in-Aid No. 20710180). NR 39 TC 2 Z9 3 U1 0 U2 2 PU MUSEUM & INST ZOOLOGY PAS-POLISH ACAD SCIENCES PI WARSAW PA WILCZA STREET 64, 00-679 WARSAW, POLAND SN 1508-1109 J9 ACTA CHIROPTEROL JI Acta Chiropt. PY 2010 VL 12 IS 2 BP 463 EP 470 DI 10.3161/150811010X538034 PG 8 WC Zoology SC Zoology GA 700VM UT WOS:000285772400020 ER PT J AU Ren, D Shih, CK Labandeira, CC AF Ren Dong Shih Chungkun Labandeira, Conrad C. TI New Jurassic Pseudopolycentropodids from China (Insecta: Mecoptera) SO ACTA GEOLOGICA SINICA-ENGLISH EDITION LA English DT Article DE Pseudopolycentropodidae; Mecoptera; fossil; new taxa; Jurassic; China ID INNER-MONGOLIA; ARCHOSTEMATA; COLEOPTERA AB In this paper two new species of fossil Pseudopolycentropus Handlirsch, 1906 are described: Pseudopolycentropus janeannae sp. nov. and P. novokshonovi, sp. nov. All of them were recovered from the Middle Jurassic non-marine sedimentary strata of northeastern China. The new material from China reveals that the early diversification of pseudopolycentropodids was well underway by the Middle Jurassic. C1 [Ren Dong; Shih Chungkun] Capital Normal Univ, Coll Life Sci, Beijing 100048, Peoples R China. [Labandeira, Conrad C.] Natl Museum Nat Hist, Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. RP Ren, D (reprint author), Capital Normal Univ, Coll Life Sci, Beijing 100048, Peoples R China. EM rendong@mail.cnu.edu.cn FU National Natural Science Foundation of China [30430100, 40872022]; Beijing Natural Science Foundation [5082002]; Beijing Municipal Commission of Education FX The research was supported by the National Natural Science Foundation of China (30430100, 40872022), the Beijing Natural Science Foundation (5082002) and Key and PHR Project of Beijing Municipal Commission of Education. NR 20 TC 30 Z9 31 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1000-9515 J9 ACTA GEOL SIN-ENGL JI Acta Geol. Sin.-Engl. Ed. PY 2010 VL 84 IS 1 BP 22 EP 30 PG 9 WC Geosciences, Multidisciplinary SC Geology GA 548TY UT WOS:000273991600003 ER PT J AU Ren, D Labandeira, CC Shih, CK AF Ren Dong Labandeira, Conrad C. Shih ChungKun TI New Mesozoic Mesopsychidae (Mecoptera) from Northeastern China SO ACTA GEOLOGICA SINICA-ENGLISH EDITION LA English DT Article DE Mecoptera; Mesopsychidae; plant-insect associations; diet; new genus; new species; proboscis; Jurassic; structural convergence; China ID CRETACEOUS AGE; INNER-MONGOLIA; MIDDLE; POLLINATION; DIPTERA; INSECTA; BEDS AB The Mesozoic family Mesopsychidae Tillyard, 1917 presently consists of seven described genera and 13 species from the mid-Triassic to the Early Cretaceous of Australia, South Africa and Eurasia. In the present paper one new genus and three new species of fossil mesopsychids are described that add significant distributional and stratigraphic extensions to the family. This finding documents the first formal record of fossil Mesopsychidae in China. Both Lichnomesopsyche gloriae gen. et sp. nov. and L. daohugouensis gen. et sp. nov. were found from the Middle Jurassic Jiulongshan Formation of Inner Mongolia, whereas Vitimopsyche kozlovi sp. nov., of mid Early Cretaceous age, was collected from the Jehol Biota of northern Hebei Province. This new, well-preserved material from China reveals complete and previously unknown body features, including head, antennae, mouthparts, legs and abdomen. The delicate and long proboscides of these new taxa indicate that they were feeding on externally exposed, nutrient-rich fluids of gymnospermous ovulate fructifications, and incapable of piercing surface epidermis - attributable principally to the absence of stylets. These proboscides originated, perhaps multiply, among basal Mecoptera and are functionally and structurally convergent with equivalent mouthparts borne by fossil and extant Diptera, Lepidoptera, Neuroptera and Coleoptera. C1 [Ren Dong; Shih ChungKun] Capital Normal Univ, Coll Life Sci, Beijing 100048, Peoples R China. [Labandeira, Conrad C.] Natl Museum Nat Hist, Smithsonian Inst, Dept Paleobiol, Washington, DC 20013 USA. [Labandeira, Conrad C.] Univ Maryland, Dept Entomol, College Pk, MD 20742 USA. RP Ren, D (reprint author), Capital Normal Univ, Coll Life Sci, Beijing 100048, Peoples R China. EM rendong@mail.cnu.edu.cn FU National Natural Science Foundation of China [40872022]; Nature Science Foundation of Beijing [5082002]; Beijing Municipal Commission of Education FX This research is supported by the National Natural Science Foundation of China (No. 40872022), the Nature Science Foundation of Beijing (No.5082002) and Scientific Research Key Program and PHR Project of Beijing Municipal Commission of Education. This is contribution 180 of the Evolution of Terrestrial Ecosystems consortium at the National Museum of Natural History in Washington, D.C., U.S.A. NR 44 TC 26 Z9 28 U1 3 U2 7 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1000-9515 J9 ACTA GEOL SIN-ENGL JI Acta Geol. Sin.-Engl. Ed. PY 2010 VL 84 IS 4 BP 720 EP 731 PG 12 WC Geosciences, Multidisciplinary SC Geology GA 642KN UT WOS:000281212100012 ER PT J AU Cardoso, P Almeida, APG AF Cardoso, Pedro Almeida, A. Paulo G. TI SPIDER POISONING IN PORTUGAL Fact or Myth? SO ACTA MEDICA PORTUGUESA LA Portuguese DT Article ID NECROTIC ARACHNIDISM; UNITED-STATES; BITES; ARANEAE; DISTRIBUTIONS; MYTHOLOGY AB SPIDER POISONING IN PORTUGAL Fact or Myth? There are 800 known species of spiders in Portugal. Of these, only two may cause any kind of medical condition: the Mediterranean black-widow (Latrodectus tredecimguttatus) and the violin spider (Loxosceles rufescens). Both are relatively common in the country, the latter inclusively in urban areas. It is frequent in Portugal for some types of necrotic lesion to be attributed to spider bites. However, as in the rest of the world, evidences are often circumstantial. Most probably, some of the reported cases may in fact represent misdiagnoses of serious conditions such as infections by Streptococcus group A or Methicillin resistant Staphylococcus aureus. The correct diagnosis of spider poisoning must always be submitted to the following steps: (1) confirmation or observation of the biting, with verification of medical signs compatible with it; (2) the spider should be captured immediately or right after the bite, dead or alive; (3) identification of the spider by a taxonomist. It is extremely important that the medical community does not associate any necrotic lesion with a spider bite based on merely circumstantial evidence. Doing it is to neglect the real cause of such condition and to delay the effective cure. In reality, given their rarity, spider bite lesions should be relegated to the end of the differential diagnostic list of necrotic skin lesions. C1 [Cardoso, Pedro] Univ Acores, Azorean Biodivers Grp CITA A, Azores, Portugal. [Cardoso, Pedro] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. [Almeida, A. Paulo G.] Univ Nova Lisboa, Unidade Entomol Med, Inst Higiene & Med Trop, P-1200 Lisbon, Portugal. RP Cardoso, P (reprint author), Univ Acores, Azorean Biodivers Grp CITA A, Azores, Portugal. RI Almeida, Antonio Paulo Gouvei/I-2541-2012; Cardoso, Pedro/A-8820-2008 OI Almeida, Antonio Paulo Gouvei/0000-0003-0751-4488; Cardoso, Pedro/0000-0001-8119-9960 NR 27 TC 3 Z9 3 U1 0 U2 5 PU ORDEM MEDICOS PI LISBON PA AV ALMIRANTE GAGO COUTINHO, 151, LISBON, 1749-084, PORTUGAL SN 1646-0758 J9 ACTA MEDICA PORT JI Acta Medica Port. PD JAN-FEB PY 2010 VL 23 IS 1 BP 33 EP 38 PG 6 WC Medicine, General & Internal SC General & Internal Medicine GA 572VO UT WOS:000275862200004 PM 20353705 ER PT B AU Ubelaker, DH AF Ubelaker, D. H. BE Vieira, DN Busuttil, A Cusack, D Beth, P TI RECENT ADVANCES IN FORENSIC ANTHROPOLOGY SO ACTA MEDICINAE LEGALIS ET SOCIALIS SE Documentos LA English DT Article; Book Chapter AB Forensic Anthropology is a dynamic field that continues to evolve with new research and augmented experience through case applications. The primary components of forensic anthropology (recovery, determination of human status, age at death, sex, ancestry, stature, and time since death, identification and assessment of evidence of foul play) all have advanced in recent years. The nature of this advancement reflects sustained research initiatives, growing numbers of scholars involved in the field, professionalization and the close link between forensic anthropology and the larger academic field of physical anthropology. C1 Smithsonian Inst, Washington, DC 20560 USA. RP Ubelaker, DH (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU UNIV COIMBRA PI COIMBRA PA RUA DA ILHA, COIMBRA, 3000-214, PORTUGAL BN 978-989-26-0173-1; 978-989-26-0049-9 J9 DOCUMENTOS PY 2010 BP 29 EP 32 D2 10.14195/978-989-26-0173-1 PG 4 WC Medicine, Legal SC Legal Medicine GA BC3XB UT WOS:000352024100005 ER PT S AU Davis, WN Reid, PB Schwartz, DA AF Davis, William N. Reid, Paul B. Schwartz, Daniel A. BE Khounsary, AM ODell, SL Restaino, SR TI Finite element analyses of thin film active grazing incidence X-ray optics SO ADAPTIVE X-RAY OPTICS SE Proceedings of SPIE-The International Society for Optical Engineering LA English DT Proceedings Paper CT Conference on Adaptive X-Ray Optics CY AUG 03-05, 2010 CL San Diego, CA SP SPIE DE x-ray optics; adjustable optics; piezo-electric; thin films; finite element analysis AB The Chandra X-ray Observatory, with its sub-arc second resolution, has revolutionized X-ray astronomy by revealing an extremely complex X-ray sky and demonstrating the power of the X-ray window in exploring fundamental astrophysical problems. Larger area telescopes of still higher angular resolution promise further advances. We are engaged in the development of a mission concept, Generation-X, a 0.1 arc second resolution x-ray telescope with tens of square meters of collecting area, 500 times that of Chandra. To achieve these two requirements of imaging and area, we are developing a grazing incidence telescope comprised of many mirror segments. Each segment is an adjustable mirror that is a section of a paraboloid or hyperboloid, aligned and figure corrected in situ on-orbit. To that end, finite element analyses of thin glass mirrors are performed to determine influence functions for each actuator on the mirrors, in order to develop algorithms for correction of mirror deformations. The effects of several mirror mounting schemes are also studied. The finite element analysis results, combined with measurements made on prototype mirrors, will be used to further refine the correction algorithms. C1 [Davis, William N.; Reid, Paul B.; Schwartz, Daniel A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Davis, WN (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 3 TC 4 Z9 4 U1 1 U2 3 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-8194-8299-0 J9 P SOC PHOTO-OPT INS PY 2010 VL 7803 AR 78030P DI 10.1117/12.862522 PG 12 WC Astronomy & Astrophysics; Optics; Physics, Applied SC Astronomy & Astrophysics; Optics; Physics GA BSU54 UT WOS:000285829000020 ER PT S AU Reid, PB Davis, W Schwartz, DA Trolier-McKinstry, S Wilke, RHT AF Reid, Paul B. Davis, William Schwartz, Daniel A. Trolier-McKinstry, Susan Wilke, Rudeger H. T. BE Khounsary, AM ODell, SL Restaino, SR TI Technology challenges of active x-ray optics for astronomy SO ADAPTIVE X-RAY OPTICS SE Proceedings of SPIE-The International Society for Optical Engineering LA English DT Proceedings Paper CT Conference on Adaptive X-Ray Optics CY AUG 03-05, 2010 CL San Diego, CA SP SPIE DE x-ray optics; adjustable optics; active optics; piezo-electric; thin films; Gen-X ID GENERATION-X; TELESCOPES AB Adjustable x-ray optics offer the promise of much higher imaging resolution with lightweight optics, providing the key technology for the development of the next generation of astronomical x-ray telescopes such as Generation-X. These adjustable grazing incidence optics might be adjusted only once, on-orbit. To produce theses optics will require the development of several component technologies along with their integration into a new mirror concept. In this paper we define a number of the key technologies necessary for adjustable x-ray optics for astronomy, give a brief description of the issues involved, and some status of these activities being developed as part of our adjustable optics development program at the Smithsonian Astrophysical Observatory. C1 [Reid, Paul B.; Davis, William; Schwartz, Daniel A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Reid, PB (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM pried@cfa.harvard.edu OI Trolier-McKinstry, Susan/0000-0002-7267-9281 NR 19 TC 2 Z9 2 U1 0 U2 2 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-8194-8299-0 J9 P SOC PHOTO-OPT INS PY 2010 VL 7803 AR 78030I DI 10.1117/12.862502 PG 9 WC Astronomy & Astrophysics; Optics; Physics, Applied SC Astronomy & Astrophysics; Optics; Physics GA BSU54 UT WOS:000285829000013 ER PT S AU Schwartz, DA Brissenden, R Freeman, M Gaetz, T Gorenstein, P Jerius, D Juda, M Reid, P Wolk, S Saha, T Zhang, W O'Dell, S Trolier-McKinstry, S Wilke, D AF Schwartz, Daniel A. Brissenden, Roger Freeman, Mark Gaetz, Terrance Gorenstein, Paul Jerius, Diab Juda, Michael Reid, Paul Wolk, Scott Saha, Timo Zhang, Will O'Dell, Stephen Trolier-McKinstry, Susan Wilke, Derek CA Gen-X Team BE Khounsary, AM ODell, SL Restaino, SR TI On-orbit adjustment concepts for the Generation-X Observatory SO ADAPTIVE X-RAY OPTICS SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Adaptive X-Ray Optics CY AUG 03-05, 2010 CL San Diego, CA SP SPIE DE X-ray optics; adaptive optics; X-ray astronomy; Generation-X Observatory ID RAY ASTRONOMY; TELESCOPES AB Generation-X is required to be an X-ray observatory with 50 m(2) effective collecting area and 0.1 arcsec half-power diameter (HPD) angular resolution at 1 keV. It is conceived that a launch vehicle such as that studied for the Ares V will carry a monolithic 16-m-diameter mirror to the earth-sun L2 point. Even with such a vehicle, the reflectors comprising the approximate to 250 nested shells must be extremely light-weight. Therefore their figure and alignment cannot be achieved on the ground, and likely could not be maintained through the launch environment. We will present a conceptual solution to those constraints: adjustable X-ray optics, as a case of "adaptive" optics where the stability once in orbit should require adjustments no more frequently than yearly. The figure would be adjusted via thin-film actuators deposited directly to the back (non-reflecting) side of each element. This bi-morph configuration would impart in-plane strains via the piezoelectric or electrostrictive effect. Requirements of the adjustment are to the order of a few nanometer precision. Each shell, and each module, must also be aligned, to tolerances of about 0.1 micrometer. We conceive that on-orbit data would be acquired by a built-in Hartmann system for the alignment adjustments and low-order figure, and by ring profile measurements of a very bright celestial X-ray source to correct figure errors up to the mid-frequency range of several hundredths cycles mm(-1). C1 [Schwartz, Daniel A.; Brissenden, Roger; Freeman, Mark; Gaetz, Terrance; Gorenstein, Paul; Jerius, Diab; Juda, Michael; Reid, Paul; Wolk, Scott] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Schwartz, DA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM das@cfa.harvard.edu OI O'Dell, Stephen/0000-0002-1868-8056; Juda, Michael/0000-0002-4375-9688; Wolk, Scott/0000-0002-0826-9261; Trolier-McKinstry, Susan/0000-0002-7267-9281 NR 12 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-8194-8299-0 J9 PROC SPIE PY 2010 VL 7803 AR 78030J DI 10.1117/12.862353 PG 10 WC Astronomy & Astrophysics; Optics; Physics, Applied SC Astronomy & Astrophysics; Optics; Physics GA BSU54 UT WOS:000285829000014 ER PT S AU Babb, JF AF Babb, James F. BE Arimondo, E Berman, PR Lin, CC TI Casimir Effects in Atomic, Molecular, and Optical Physics SO ADVANCES IN ATOMIC, MOLECULAR, AND OPTICAL PHYSICS, VOL 59 SE Advances In Atomic Molecular and Optical Physics LA English DT Review; Book Chapter ID LONG-RANGE POTENTIALS; HELIUM RYDBERG STATES; GAUGE ELECTRODYNAMICS ANALYSIS; ALKALI-METAL ATOMS; DER-WAALS FORCES; 2 HYDROGEN ATOMS; DISPERSION FORCES; ELECTROMAGNETIC-FIELD; RETARDED INTERACTION; INTERACTION ENERGIES AB The long-range interaction between two atoms and the long-range interaction between an ion and an electron are compared at small and large intersystem separations. The vacuum dressed atom formalism is applied and found to provide a framework for interpretation of the similarities between the two cases. The van der Waals forces or Casimir-Polder potentials are used to obtain insight into relativistic and higher multipolar terms. C1 Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Babb, JF (reprint author), Harvard Smithsonian Ctr Astrophys, ITAMP, MS 14,60 Garden St, Cambridge, MA 02138 USA. OI Babb, James/0000-0002-3883-9501 NR 89 TC 7 Z9 7 U1 2 U2 18 PU ELSEVIER ACADEMIC PRESS INC PI SAN DIEGO PA 525 B STREET, SUITE 1900, SAN DIEGO, CA 92101-4495 USA SN 1049-250X BN 978-0-12-381021-2 J9 ADV ATOM MOL OPT PHY JI Adv. Atom. Mol. Opt. Phys. PY 2010 VL 59 BP 1 EP 20 DI 10.1016/S1049-250X(10)59001-3 PG 20 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA BAJ34 UT WOS:000304330200001 ER PT B AU Leonidaki, I Zezas, A Boumis, P AF Leonidaki, I. Zezas, A. Boumis, P. BE Tsinganos, K Hatzidimitriou, D Matsakos, T TI New X-ray and Optical SNRs in Six Nearby Galaxies SO ADVANCES IN HELLENIC ASTRONOMY DURING THE IYA09 SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 9th International Conference of the Hellenic-Astronomical-Society CY SEP 20-24, 2009 CL Univ Athens, Athens, GREECE SP Hellen Astron Soc HO Univ Athens AB We present the results from a study of the SNR populations in six nearby galaxies (NGC 2403, NGC 3077, NGC 4214, NGC 4395, NGC 4449 and NGC 5204) based on Chandra archival data. We have detected a sample of 244 discrete X-ray sources with fluxes down to 10(-17) erg s(-1) cm(-2). A total number of 37 X-ray detected SNRs are identified, 30 of which are new, based on their X-ray colors and spectroscopy. We discuss the SNR properties (luminosity, temperature, density) of the X-ray detected SNRs in order to obtain information on their interaction with their environment. We also compare the luminosity distributions of X-ray SNRs in different types of galaxies with the number of our X-ray detected SNRs and we indicate differences between the SNR populations in spiral and irregular galaxies. On the basis of a multi-wavelength study of SNRs, we obtained deep images in the [S II] and H alpha emission lines and we initially classified a large number of optical candidate SNRs based on their [S II] /H alpha ratio. Follow-up spectro-photometric observations for a number of the candidate SNRs have also been obtained and their spectral signatures suggest that the detected emission originates from shock-heated gas. C1 [Leonidaki, I.; Boumis, P.] Natl Observ Athens, Inst Astron & Astrophys, Athens 15236, Greece. [Zezas, A.] Univ Crete, Dept Phys, Iraklion, Greece. [Zezas, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Leonidaki, I (reprint author), Natl Observ Athens, Inst Astron & Astrophys, Athens 15236, Greece. NR 3 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-728-5 J9 ASTR SOC P PY 2010 VL 424 BP 223 EP + PG 3 WC Astronomy & Astrophysics; Education, Scientific Disciplines; History & Philosophy Of Science SC Astronomy & Astrophysics; Education & Educational Research; History & Philosophy of Science GA BTR13 UT WOS:000287834100051 ER PT B AU Antoniou, V Zezas, A Hatzidimitriou, D Kalogera, V AF Antoniou, V. Zezas, A. Hatzidimitriou, D. Kalogera, V. BE Tsinganos, K Hatzidimitriou, D Matsakos, T TI Small Magellanic Cloud: Star-Formation History and X-ray Binary Populations SO ADVANCES IN HELLENIC ASTRONOMY DURING THE IYA09 SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 9th International Conference of the Hellenic-Astronomical-Society CY SEP 20-24, 2009 CL Univ Athens, Athens, GREECE SP Hellen Astron Soc HO Univ Athens ID VELOCITIES AB Using Chandra, XMM-Newton and optical photometric catalogs we study the young XRB populations of the SMC. We find that the Be-XRBs are observed in regions with star formation (SF) rate bursts similar to 25-60 Myr ago. The similarity of this age with the age of maximum occurrence of the Be phenomenon (similar to 40 Myr) indicates that the presence of a circumstellar decretion disk plays a significant role in the number of observed XRBs in the 10-100 Myr age range. We also find that regions with strong but more recent SF (e.g. the Wing) are deficient in Be-XRBs. By correlating the number of observed Be-XRBs with the formation rate of their parent populations, we measure a Be-XRB production rate of similar to 1 system per 10(-6) M-circle dot/yr. Finally, we use the strong localization of the Be-XRB systems in order to set limits on the kicks imparted on the neutron star during the supernova explosion. C1 [Antoniou, V.; Zezas, A.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Antoniou, V.; Zezas, A.] Univ Crete, Dept Phys, Iraklion GR-71003, Greece. [Hatzidimitriou, D.] Univ Athens, Dept Phys, GR-15784 Athens, Greece. [Kalogera, V.] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. RP Antoniou, V (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM vantoniou@head.cfa.harvard.edu NR 8 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-728-5 J9 ASTR SOC P PY 2010 VL 424 BP 230 EP 232 PG 3 WC Astronomy & Astrophysics; Education, Scientific Disciplines; History & Philosophy Of Science SC Astronomy & Astrophysics; Education & Educational Research; History & Philosophy of Science GA BTR13 UT WOS:000287834100052 ER PT B AU Gazeas, KD Papathanassoglou, DA AF Gazeas, K. D. Papathanassoglou, D. A. BE Tsinganos, K Hatzidimitriou, D Matsakos, T TI Applications of the Stellar Spectrograph of the University of Athens Observatory SO ADVANCES IN HELLENIC ASTRONOMY DURING THE IYA09 SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 9th International Conference of the Hellenic-Astronomical-Society CY SEP 20-24, 2009 CL Univ Athens, Athens, GREECE SP Hellen Astron Soc HO Univ Athens AB The high quality stellar spectra, recorded with the stellar spectrograph constructed at the Laboratory of Astronomy and Applied Optics of the University of Athens, allows the spectral classification of stars brighter than 9 mag, as well as the measurement of radial velocities of binary systems. The primary application of the spectrograph will be the study of eclipsing binaries, where the lack of spectroscopic observations limits the theoretical models. The spectrograph can be also used for observations of transient phenomena, such as novae, supernovae, comets and cataclysmic variable stars, but also for support observations of larger telescopes around the world. C1 [Gazeas, K. D.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Gazeas, K. D.; Papathanassoglou, D. A.] Univ Athens, Dept Astrophys Astron & Mech, GR-15784 Athens, Greece. RP Gazeas, KD (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-728-5 J9 ASTR SOC P PY 2010 VL 424 BP 433 EP + PG 2 WC Astronomy & Astrophysics; Education, Scientific Disciplines; History & Philosophy Of Science SC Astronomy & Astrophysics; Education & Educational Research; History & Philosophy of Science GA BTR13 UT WOS:000287834100097 ER PT S AU Skapin, AS Ropret, P AF Skapin, A. Sever Ropret, P. BE Hawkes, PW TI Identification of Historical Pigments in Wall Layers by Combination of Optical and Scanning Electron Microscopy Coupled with Energy-Dispersive Spectroscopy SO ADVANCES IN IMAGING AND ELECTRON PHYSICS, VOL 163 SE Advances in Imaging and Electron Physics LA English DT Review; Book Chapter ID SYNTHETIC ORGANIC PIGMENTS; X-RAY-EMISSION; RAMAN-SPECTROSCOPY; IN-SITU; ART; PAINTINGS; MICROANALYSIS; POTTERY; MAPS; SEM C1 [Skapin, A. Sever] Slovenian Natl Bldg & Civil Engn Inst, Ljubljana 1000, Slovenia. [Ropret, P.] Inst Protect Cultural Heritage Slovenia, Conservat Ctr, Res Inst, Ljubljana 1000, Slovenia. [Ropret, P.] Smithsonian Inst, Museum Conservat Inst, Suitland, MD 20746 USA. RP Skapin, AS (reprint author), Slovenian Natl Bldg & Civil Engn Inst, Dimiceva 12, Ljubljana 1000, Slovenia. NR 42 TC 2 Z9 2 U1 2 U2 9 PU ELSEVIER ACADEMIC PRESS INC PI SAN DIEGO PA 525 B STREET, SUITE 1900, SAN DIEGO, CA 92101-4495 USA SN 1076-5670 BN 978-0-12-381314-5 J9 ADV IMAG ELECT PHYS JI Adv. Imag. Electron Phys. PY 2010 VL 163 BP 141 EP 163 DI 10.1016/S1076-5670(10)63004-2 PG 23 WC Physics, Applied SC Physics GA BQA27 UT WOS:000280489700004 ER PT B AU Hoorn, C Roddaz, M Dino, R Soares, E Uba, C Ochoa-Lozano, D Mapes, R AF Hoorn, Carina Roddaz, Martin Dino, Rodolfo Soares, Emilio Uba, Cornelius Ochoa-Lozano, Diana Mapes, Russell BE Hoorn, C Wesselingh, FP TI The Amazonian Craton and its influence on past fluvial systems (Mesozoic-Cenozoic, Amazonia) SO AMAZONIA: LANDSCAPE AND SPECIES EVOLUTION: A LOOK INTO THE PAST LA English DT Article; Book Chapter ID WHITE-SAND FORESTS; TRACE-ELEMENT GEOCHEMISTRY; FORELAND BASIN; SOUTH-AMERICA; CENTRAL ANDES; LATE MIOCENE; SEDIMENTARY BASINS; DRAINAGE PATTERNS; ECUADORIAN ANDES; MANTLE PLUMES AB The Amazonian Craton is an old geological feature of Archaean/Proterozoic age that has determined the character of fluvial systems in Amazonia throughout most of its past. This situation radically changed during the Cenozoic, when uplift of the Andes reshaped the relief and drainage patterns of northern South America. Here we review the sedimentary characteristics of Amazonian rivers and compare these with four fluvial depositional settings from the Meso-Cenozoic sedimentary record. These sedimentary units are the Alter do Chao Formation (Brazil, Late Cretaceous-Paleogene), the Petaca Formation (Bolivia, Late Oligocene to Middle Miocene), the Mariname and Apaporis Sand Units (Colombia, Miocene), and the Iquitos White Sand Unit (Peru, Late Miocene-Pliocene). This review illustrates that the river systems born on the craton share features such as sediment texture and composition, depositional environments and transport directions. Evidence for the diminished role of cratonic fluvial systems and the onset of Neogene Andean uplift can be identified in the sedimentary record by changes in sediment provenance and transport directions. Although the Andean uplift and related processes discontinued the major Amazonian-born fluvial systems it also created new topographic features such as the Iquitos and Fitzcarrald Arches. These newly formed reliefs triggered a new generation of rivers, some of which are presently known as biodiversity hotspots. C1 [Hoorn, Carina] Univ Amsterdam, Inst Biodivers & Ecosyst Anal, NL-1098 SM Amsterdam, Netherlands. [Roddaz, Martin] Univ Toulouse, Lab Mecanismes & Transferts Geol, F-31400 Toulouse, France. [Dino, Rodolfo] Ilha Fundao, BR-21941915 Rio De Janeiro, RJ, Brazil. [Soares, Emilio] Univ Fed Amazonas, BR-69077000 Manaus, Amazonas, Brazil. [Uba, Cornelius] Univ Potsdam, Inst Geowissensch, D-14476 Golm, Germany. [Ochoa-Lozano, Diana] Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archeol, Balboa, Ancon, Panama. [Mapes, Russell] Univ N Carolina, Dept Geol Sci, Chapel Hill, NC 27599 USA. RP Hoorn, C (reprint author), Univ Amsterdam, Inst Biodivers & Ecosyst Anal, Kruislaan 318, NL-1098 SM Amsterdam, Netherlands. EM carina.hoorn@milne.cc; mroddaz@lmtg.obs-mip.fr; dino@petrobras.com.br; easoares@ufam.edu.br; ubaeji@yahoo.com; dochoa1709@yahoo.com NR 122 TC 8 Z9 9 U1 1 U2 4 PU WILEY-BLACKWELL PI CHICHESTER PA THE ATRIUM, SOUTHERN GATE, CHICHESTER, WEST SUSSEX PO19 8SQ, ENGLAND BN 978-1-4443-0641-5; 978-1-4051-8113-6 PY 2010 BP 103 EP 122 PG 20 WC Evolutionary Biology; Geosciences, Multidisciplinary SC Evolutionary Biology; Geology GA BA7CZ UT WOS:000337463900008 ER PT B AU Jaramillo, C Hoorn, C Silva, SAF Leite, F Herrera, F Quiroz, L Dino, R Antonioli, L AF Jaramillo, Carlos Hoorn, Carina Silva, Silane A. F. Leite, Fatima Herrera, Fabiany Quiroz, Luis Dino, Rodolfo Antonioli, Luzia BE Hoorn, C Wesselingh, FP TI The origin of the modern Amazon rainforest: implications of the palynological and palaeobotanical record SO AMAZONIA: LANDSCAPE AND SPECIES EVOLUTION: A LOOK INTO THE PAST LA English DT Article; Book Chapter ID NORTHERN SOUTH-AMERICA; WESTERN AMAZONIA; EARLY MIOCENE; CERREJON FORMATION; MARINE INCURSIONS; ANDEAN TECTONICS; MIDDLE MIOCENE; LATE PALEOCENE; RIVER SYSTEM; LATE EOCENE AB Northern South America harbours a highly diversified forest vegetation. However, it is not clear when this remarkable diversity was attained and how it was produced. Is the high diversity the product of a positive speciation-extinction balance that accumulated species over long time periods, or is it the product of high origination rates over short time periods, or both? Middle Cretaceous floras, although very poorly studied, are dominated by non-angiosperm taxa. By the Paleocene, pollen and macrobotanical fossils suggest that the basic phylogenetic composition and floral physiognomy of Neotropical rainforests were already present. Hence there was a profound change in Amazonian flora during the Late Cretaceous, that still needs to be documented. Levels of Paleocene diversity are much lower than those of modern tropical rainforests. By the Early Eocene, however, pollen diversity was very high, exceeding values of modern rainforests. At the Eocene-Oligocene a major drop in diversity coincided with an episode of global cooling. The palynological and palaeobotanical records of Amazonia suggest that high levels of diversity existed during the Miocene, a period when the boundary conditions for sustaining a rainforest (e. g. low seasonality, high precipitation, edaphic heterogeneous substrate) were met. The predecessor of the present rainforest was formed during the Paleogene and Neogene when the western Amazon lowlands were affected by Andean tectonism, which radically changed drainage systems and promoted wetland development. An overall global cooling during the Neogene also may have affected the rainforest, decreasing its area and expanding adjacent savanna belts. Recent events like the Quaternary ice ages also played a role in the forest dynamics and composition, although it seems to have been minor. In this chapter we will review the main characteristics of the Neogene palynological and palaeobotanical records in Amazonia, and we will make some comparisons with pre- and post-Neogene records. The data indicate that the Amazonian rainforest is more likely to be a product of a dynamic geological history stretching back over the past 25 million years rather than the last few hundred thousand years. C1 [Jaramillo, Carlos; Herrera, Fabiany; Quiroz, Luis] Smithsonian Trop Res Inst, Balboa, Panama. [Hoorn, Carina] Univ Amsterdam, Inst Biodivers & Ecosyst Anal, NL-1098 SM Amsterdam, Netherlands. [Silva, Silane A. F.] INPA, Coordenacao Pesquisas Bot, Lab Palinol, Manaus, Amazonas, Brazil. [Leite, Fatima] Univ Brasilia, Inst Geosci, BR-70910900 Brasilia, DF, Brazil. [Quiroz, Luis] Univ Saskatchewan, Dept Geol Sci, Saskatoon, SK S7N 5E2, Canada. [Dino, Rodolfo] Ilha Fundao, BR-21941915 Rio De Janeiro, RJ, Brazil. [Antonioli, Luzia] Univ Estado Rio De Janeiro, Fac Geol DEPA, BR-20550900 Rio De Janeiro, RJ, Brazil. RP Jaramillo, C (reprint author), Smithsonian Trop Res Inst, Box 0843-03092, Balboa, Panama. EM JaramilloC@si.edu; carina.hoorn@milne.cc; silane.silva@gmail.com; fprleite@gmail.com; fabianyht@yahoo.com.mx; luisignacioquiroz@gmail.com; dino@petrobras.com.br; antonioli@novanet.com.br NR 104 TC 32 Z9 35 U1 2 U2 12 PU WILEY-BLACKWELL PI CHICHESTER PA THE ATRIUM, SOUTHERN GATE, CHICHESTER, WEST SUSSEX PO19 8SQ, ENGLAND BN 978-1-4443-0641-5; 978-1-4051-8113-6 PY 2010 BP 317 EP 334 PG 18 WC Evolutionary Biology; Geosciences, Multidisciplinary SC Evolutionary Biology; Geology GA BA7CZ UT WOS:000337463900020 ER PT B AU Antonelli, A Quijada-Mascarenas, A Crawford, AJ Bates, JM Velazco, PM Wuster, W AF Antonelli, Alexandre Quijada-Mascarenas, Adrian Crawford, Andrew J. Bates, John M. Velazco, Paul M. Wuester, Wolfgang BE Hoorn, C Wesselingh, FP TI Molecular studies and phylogeography of Amazonian tetrapods and their relation to geological and climatic models SO AMAZONIA: LANDSCAPE AND SPECIES EVOLUTION: A LOOK INTO THE PAST LA English DT Article; Book Chapter ID MITOCHONDRIAL-DNA SEQUENCES; COMPLEX EVOLUTIONARY HISTORY; POPULATION GENETIC-STRUCTURE; RIVERINE BARRIER HYPOTHESIS; BATS TRIBE DICLIDURINI; SOUTH-AMERICA; LOWLAND FOREST; PHYLOGENETIC-RELATIONSHIPS; NICHE CONSERVATISM; ANDEAN TECTONICS AB Explaining the origins and evolution of Amazonian biodiversity continues to be an outstanding question in evolutionary biology. A plethora of mechanisms for promoting diversification has been proposed, generally invoking ecological and vicariance processes associated with major geological, hydrological and climatic events in the history of the Amazon drainage basin. Here, we review recent advances on this topic in the light of a rich new source of information: molecular phylogenetics and especially phylogeography. We present a comparison of phylogeographical studies covering over 50 clades of amphibians, birds, non-avian reptiles and mammals, focusing on studies where estimates of divergence times were explicitly calculated. We then discuss the congruence of the speciation patterns found in these studies with previous hypotheses of diversification. Based on the estimates of crown group ages, we conclude that a high proportion of present-day diversity is a result of Neogene diversification. The origin of most clades clearly predates the Pleistocene by a considerable margin, refuting the long-held hypothesis that repeated expansion and contraction of lowland forests during Pleistocene climatic changes would be responsible for most of the Amazonian biodiversity. However, some evidence from phylogenetic and distributional patterns suggests that climate cycles did trigger speciation. Speciose lineages of tetrapods tend to be older than groups containing one to a few species, with a few notable exceptions. Considering each tetrapod group alone, amphibians and non-avian reptiles are generally older than birds, while mammals contain both recent and ancient clades of approximately the same number of species. Finally, we make recommendations about future research approaches and animal systems that deserve further attention from phylogeographers. C1 [Antonelli, Alexandre] Univ Zurich, Inst Systemat Bot, CH-8008 Zurich, Switzerland. [Antonelli, Alexandre] Univ Gothenburg, Gothenburg, Sweden. [Quijada-Mascarenas, Adrian] Univ Arizona, Sch Nat Resources, Tucson, AZ 85721 USA. [Crawford, Andrew J.] Smithsonian Trop Res Inst, Naos Mol Labs, Balboa, Ancon, Panama. [Crawford, Andrew J.] Univ Los Andes, Bogota, Colombia. [Bates, John M.; Velazco, Paul M.] Field Museum Nat Hist, Dept Zool, Chicago, IL 60605 USA. [Wuester, Wolfgang] Bangor Univ, Sch Biol Sci, Bangor LL57 2UW, Gwynedd, Wales. RP Antonelli, A (reprint author), Univ Zurich, Inst Systemat Bot, Zollikerstr 107, CH-8008 Zurich, Switzerland. EM alexandre.antonelli@systbot.uzh.ch; adrianquijada@hotmail.com; andrew@dna.ac; jbates@fieldmuseum.org; pvelazco@fieldmuseum.org; w.wuster@bangor.ac.uk RI Wuster, Wolfgang/B-2879-2008 OI Wuster, Wolfgang/0000-0002-4890-4311 NR 217 TC 49 Z9 50 U1 0 U2 6 PU WILEY-BLACKWELL PI CHICHESTER PA THE ATRIUM, SOUTHERN GATE, CHICHESTER, WEST SUSSEX PO19 8SQ, ENGLAND BN 978-1-4443-0641-5; 978-1-4051-8113-6 PY 2010 BP 386 EP 404 PG 19 WC Evolutionary Biology; Geosciences, Multidisciplinary SC Evolutionary Biology; Geology GA BA7CZ UT WOS:000337463900025 ER PT B AU Deutsch, JI AF Deutsch, James I. BE Arbeit, M Trusnik, R TI NASA's FIFTY YEARS OF UPS AND DOWNS: RIGHT STUFF, WRONG STUFF, AND FIXING STUFF ON THE FRONTIERS OF SPACE SO AMERICA IN MOTION LA English DT Proceedings Paper CT 15th International Colloquium of American Studies CY SEP 07-10, 2008 CL Palacky Univ, Olomouc, CZECH REPUBLIC SP Palacky Univ, Czech & Slovak Assoc Amer Studies, Govt US Amer, Off Publ Affairs, Prague, Czech Republic HO Palacky Univ DE National Aeronautics and Space Administration; frontiers; space race; astronauts AB The image and reputation of the National Aeronautics and Space Administration suffered from a series of embarrassing incidents in 2007. However, over the course of its 50-year history, the agency has endured other public relations challenges, primarily relating to its ventures in human spaceflight. One of NASA's notable successes was in applying the image of the frontier to outer space. Whether NASA will be able to recapture the public's excitement in future space exploration remains to be seen. C1 [Deutsch, James I.] Ctr Folklife & Cultural Heritage, Smithsonian Inst, Washington, DC 20024 USA. EM deutschj@si.edu NR 32 TC 0 Z9 0 U1 0 U2 0 PU PALACKY UNIV PI OLOMOUC PA OLOMOUC, KRIZKOVSKEHO 8, OLOMOUC, 771 47, CZECH REPUBLIC BN 978-80-244-2458-3 PY 2010 BP 205 EP 218 PG 14 WC Cultural Studies SC Cultural Studies GA BXN32 UT WOS:000296489500012 ER PT J AU Correa, E Jaramillo, C Manchester, S Gutierrez, M AF Correa, Edwin Jaramillo, Carlos Manchester, Steven Gutierrez, Mauricio TI A FRUIT AND LEAVES OF RHAMNACEOUS AFFINITIES FROM THE LATE CRETACEOUS (MAASTRICHTIAN) OF COLOMBIA SO AMERICAN JOURNAL OF BOTANY LA English DT Article DE Berhamniphyllum, Colombia; Guaduas Formation; late Cretaceous; Maastrichtian; Paliureae; Rhamnaceae ID NORTH-AMERICA; BIOGEOGRAPHY; ANGIOSPERMS; OLIGOCENE; FLORA; TREE; PALIURUS; HISTORY; MIOCENE; PUEBLA AB Although Rhamnaceae are distributed worldwide today, the former hypothesis for its Laurasian origins may need to be reconsidered in view of recently discovered fossils from the Guaduas Formation of central Colombia (similar to 68 Ma), including fossil leaves (Berhamniphyllum) and a fruit (Archaeopaliurus boyacensis). Recent phylogenetic studies calibrate the stem of Rhamnaceae at 64 Ma and divide the family into three groups, rhamnoid, ampeloziziphoid, and ziziphoid. Although the fruit, Archaeopaliurus boyacensis, resembles that of Paliurus and suggests a relationship to the Paliureae in the ziziphoid group, associated leaves of Berhamniphyllum conform in architecture to those found today only in the Rhamneae tribe. The Maastrichtian age of these fossils predates the ages previously estimated for the Rhamneae tribe (28.5 Ma) and the Paliureae tribe (31.6 Ma) using a modified clock approach. Based on the new megafossil evidence, two alternative ideas are proposed: (1) that these fossils predate the extant tribes or (2) that the family diversified into modern tribes earlier than previously proposed. C1 [Correa, Edwin; Jaramillo, Carlos; Gutierrez, Mauricio] Smithsonian Trop Res Inst, Panama City, Panama. [Manchester, Steven] Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA. [Gutierrez, Mauricio] Univ Chile, Fac Ciencias, Dept Ciencias Ecol, Santiago, Chile. RP Jaramillo, C (reprint author), Smithsonian Trop Res Inst, Panama City, Panama. EM jaramilloc@si.edu FU Smithsonian Paleobiology Endowment Fund; Unrestricted Endowments SI; ACGGP-Ares FX The authors thank Dr. David Dilcher, the AJB Editor-in-Chief, Associate Editor, and two anonymous reviewers for valuable commentaries. This project was supported by the Smithsonian Paleobiology Endowment Fund and the Unrestricted Endowments SI Grants and the ACGGP-Ares fund. Thanks to ICP-Ecopetrol S. A. for logistic support. NR 61 TC 13 Z9 15 U1 1 U2 10 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 JAN PY 2010 VL 97 IS 1 BP 71 EP 79 DI 10.3732/ajb.0900093 PG 9 WC Plant Sciences SC Plant Sciences GA 542UM UT WOS:000273523700007 PM 21622368 ER PT J AU Marzke, MW Tocheri, MW Steinberg, B Femiani, JD Reece, SP Linscheid, RL Orr, CM Marzke, RF AF Marzke, M. W. Tocheri, M. W. Steinberg, B. Femiani, J. D. Reece, S. P. Linscheid, R. L. Orr, C. M. Marzke, R. F. TI Comparative 3D Quantitative Analyses of Trapeziometacarpal Joint Surface Curvatures Among Living Catarrhines and Fossil Hominins SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Article DE thumb; morphology; stereophotogrammetry; laser scanning; geometric modeling ID THUMB CARPOMETACARPAL JOINT; OLDUVAI-GORGE; METACARPAL JOINT; AUSTRALOPITHECUS-AFARENSIS; MORPHOLOGICAL AFFINITIES; CONTACT AREAS; HAND; HOMO; EVOLUTIONARY; STABILITY AB Comparisons of joint surface curvature at the base of the thumb have long been made to discern differences among living and fossil primates in functional capabilities of the hand. However, the complex shape of this joint makes it difficult to quantify differences among taxa. The purpose of this study is to determine whether significant differences in curvature exist among selected catarrhine genera and to compare these genera with hominin(1) fossils in trapeziometacarpal curvature. Two 3D approaches are used to quantify curvatures of the trapezial and metacarpal joint surfaces: (1) stereophotogrammetry with nonuniform rational B-spline (NURBS) calculation of joint curvature to compare modern humans with captive chimpanzees and (2) laser scanning with a quadric-based calculation of curvature to compare modern humans and wild-caught Pan, Gorilla, Pongo, and Papio. Both approaches show that Homo has significantly lower curvature of the joint surfaces than does Pan. The second approach shows that Gorilla has significantly more curvature than modern humans, while Pongo overlaps with humans and African apes. The surfaces in Papio are more cylindrical and flatter than in Homo. Australopithecus afarensis resembles African apes more than modern humans in curvatures, whereas the Homo habilis trapezial metacarpal surface is flatter than in all genera except Papio. Neandertals fall at one end of the modern human range of variation, with smaller dorsovolar curvature. Modern human topography appears to be derived relative to great apes and Australopithecus and contributes to the distinctive human morphology that facilitates forceful precision and power gripping, fundamental to human manipulative activities. Am J Phys Anthropol. 141:38-51, 2010. (C) 2009 Wiley-Liss, Inc. C1 [Marzke, M. W.; Orr, C. M.] Arizona State Univ, Sch Human Evolut & Social Change, Tempe, AZ 85287 USA. [Tocheri, M. W.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Human Origins Program, Washington, DC 20013 USA. [Steinberg, B.] Oregon State Univ, Corvallis, OR 97331 USA. [Femiani, J. D.] Arizona State Univ, Div Comp Studies, Tempe, AZ 85287 USA. [Linscheid, R. L.] Mayo Clin, Rochester, MN 55905 USA. [Orr, C. M.] Arizona State Univ, Inst Human Origins, Tempe, AZ 85287 USA. [Marzke, R. F.] Arizona State Univ, Dept Phys & Astron, Tempe, AZ 85287 USA. RP Marzke, MW (reprint author), Arizona State Univ, Sch Human Evolut & Social Change, Tempe, AZ 85287 USA. EM mary.marzke@asu.edu OI Tocheri, Matthew/0000-0001-7600-8998 FU National Science Foundation [IIS 998016]; National Institutes of Health, Division of Research Resources [U42RR15090-01]; Smithsonian Institution Fellowship Program; ASU College of Liberal Arts and Sciences FX Grant sponsor: National Science Foundation; Grant number: IIS 998016; Grant sponsor: National Institutes of Health, Division of Research Resources; Grant number: U42RR15090-01; Grant sponsors: The Smithsonian Institution Fellowship Program, The ASU College of Liberal Arts and Sciences. NR 67 TC 26 Z9 26 U1 1 U2 9 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PD JAN PY 2010 VL 141 IS 1 BP 38 EP 51 DI 10.1002/ajpa.21112 PG 14 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 534SR UT WOS:000272918100005 PM 19544574 ER PT J AU Griffin, NL Richmond, BG AF Griffin, Nicole L. Richmond, Brian G. TI Joint Orientation and Function in Great Ape and Human Proximal Pedal Phalanges SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Article DE Australopithecus afarensis; dorsal canting; hallux; metatarsophalangeal joint ID AUSTRALOPITHECUS-AFARENSIS; POSITIONAL BEHAVIOR; SEX-DIFFERENCES; PAN-PANISCUS; HUMAN FOOT; HOMINIDS; WALKING; ARBOREALITY; LOCOMOTION; CHIMPANZEE AB Previous studies have referred to the degree of dorsal canting of the base of the proximal phalanx as an indicator of human-like metatarsophalangeal joint function and thus a diagnostic trait of habitual bipedality in the fossil record. Here, we used a simple method to investigate differences in forefoot function on a finer scale. Building on Duncan et al.'s (Am J Phys Anthropol 93 [1994] 67-81) research, we tested whether dorsal canting reflects differences between sexes in locomotor behavior, whether habitual shoe wear influences dorsal canting in humans, and whether proximal joint morphology differs between rays in Pan and humans. Our results corroborate previous research in showing that humans have proximal phalanges with joint orientations that are significantly more dorsal than, but overlap with, those of great apes. We also found that male gorillas have significantly more dorsally canted second proximal phalanges than their female counterparts, while the opposite pattern between the sexes was found in Pan troglodytes. Inter-ray comparisons indicate that Pan have more dorsally canted first proximal phalanges than second proximal phalanges, while the opposite pattern was found in humans. Minimally shod humans have slightly but significantly more dorsally canted second proximal phalanges than those of habitually shod humans, indicating that phalanges of unshod humans provide the most appropriate comparative samples for analyses of early hominins. Overall, our analysis suggests that though the measurement of dorsal canting is limited in its sensitivity to certain intraspecific differences in function, phalangeal joint orientation reflects interspecific differences in joint function, with the caveat that different patterns of forefoot function during gait can involve similar articular sets of metatarsophalangeal joints. Am J Phys Anthropol 141:116-123, 2010. (C) 2009 Wiley-Liss, Inc. C1 [Griffin, Nicole L.; Richmond, Brian G.] George Washington Univ, Ctr Adv Study Hominid Paleobiol, Washington, DC 20052 USA. [Richmond, Brian G.] Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20560 USA. RP Griffin, NL (reprint author), George Washington Univ, Ctr Adv Study Hominid Paleobiol, 2110 G St NW, Washington, DC 20052 USA. EM nlgriff@gwmail.gwu.edu FU NSF [BCS-0726124, IGERT 9987590, IGERT 0801634]; George Washington University; Sigma Xi; L.S.B. Leakey Foundation FX Grant sponsor: NSF; Grant numbers: BCS-0726124, IGERT 9987590, IGERT 0801634 Grant sponsors: George Washington University (Cotlow Field Research Fund and Selective Excellence Fellowship for Hominid Paleobiology), Sigma Xi (Grant-in-Aid of Research), L.S.B. Leakey Foundation. NR 42 TC 16 Z9 16 U1 5 U2 12 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PD JAN PY 2010 VL 141 IS 1 BP 116 EP 123 DI 10.1002/ajpa.21121 PG 8 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 534SR UT WOS:000272918100010 PM 19554617 ER PT J AU Behrensmeyer, AK Harmon, EH AF Behrensmeyer, Anna K. Harmon, Elizabeth H. TI Taphonomy and paleoccology of the AL 333 hominin fossil assemblage, Hadar, Ethiopia. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 79th Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 14-17, 2010 CL Albuquerque, NM SP Amer Assoc Phys Anthropol C1 [Behrensmeyer, Anna K.] Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. [Harmon, Elizabeth H.] CUNY Hunter Coll, Dept Anthropol, New York, NY 10021 USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2010 SU 50 BP 65 EP 65 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 565LT UT WOS:000275295200060 ER PT J AU Castillo, E Dudar, C AF Castillo, Eric Dudar, Christopher TI Quantifying variation at the occipito-cervical articular surfaces using 3D scanning technology. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 79th Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 14-17, 2010 CL Albuquerque, NM SP Amer Assoc Phys Anthropol C1 [Castillo, Eric; Dudar, Christopher] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, 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 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2010 SU 50 BP 79 EP 79 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 565LT UT WOS:000275295200123 ER PT J AU Chirchir, H Richmond, BG Griffin, NL Nakatsukasa, M Zeininger, A Ketcham, RA AF Chirchir, Habiba Richmond, Brian G. Griffin, Nicole L. Nakatsukasa, Masato Zeininger, Angel Ketcham, Richard A. TI Hand biomechanics and trabecular architecture in hominoid metacarpals. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 79th Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 14-17, 2010 CL Albuquerque, NM SP Amer Assoc Phys Anthropol C1 [Chirchir, Habiba; Ketcham, Richard A.] George Washington Univ, Hominid Paleobiol Doctoral Program, Dept Anthropol, Washington, DC 20052 USA. [Chirchir, Habiba; Richmond, Brian G.] George Washington Univ, Ctr Adv Study Hominid Paleobiol, Washington, DC 20052 USA. [Richmond, Brian G.] Smithsonian Inst, Human Origins Program, Washington, DC 20560 USA. [Griffin, Nicole L.] Duke Univ, Dept Evolutionary Anthropol, Durham, NC 27706 USA. [Nakatsukasa, Masato] Kyoto Univ, Lab Phys Anthropol, Grad Sch Sci, Kyoto 6068501, Japan. [Zeininger, Angel] Univ Texas Austin, Dept Anthropol, Austin, TX 78712 USA. [Ketcham, Richard A.] Univ Texas Austin, Dept Geol Sci, Austin, TX 78712 USA. NR 0 TC 1 Z9 1 U1 0 U2 1 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2010 SU 50 BP 81 EP 81 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 565LT UT WOS:000275295200130 ER PT J AU Crofoot, M Caillaud, D Salvador, L Scarpino, S Boyer, D Ryan, S Walsh, P AF Crofoot, Margaret Caillaud, Damien Salvador, Liliana Scarpino, Samuel Boyer, Denis Ryan, Sadie Walsh, Peter TI No need for violence: episodic memory and scramble competition can explain primate "war zones". SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 79th Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 14-17, 2010 CL Albuquerque, NM SP Amer Assoc Phys Anthropol C1 [Walsh, Peter] Max Planck Inst Evolutionary Anthropol, Leipzig, Germany. [Ryan, Sadie] Univ Calif Santa Barbara, Natl Ctr Ecol Anal & Synth, Santa Barbara, CA 93106 USA. [Boyer, Denis] Univ Nacl Autonoma Mexico, Inst Fis, Dept Sistemas Complejos, Mexico City 04510, DF, Mexico. [Salvador, Liliana] Princeton Univ, Dept Ecol & Evolutionary Biol, Princeton, NJ 08544 USA. [Caillaud, Damien; Scarpino, Samuel] Univ Texas Austin, Sect Integrat Biol, Austin, TX 78712 USA. [Crofoot, Margaret] Max Planck Inst Ornithol, Div Migrat & Immunoecol, Radolfzell am Bodensee, Germany. [Crofoot, Margaret] Smithsonian Trop Res Inst, Balboa, Panama. NR 0 TC 0 Z9 0 U1 0 U2 1 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2010 SU 50 BP 88 EP 88 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 565LT UT WOS:000275295200160 ER PT J AU Green, DJ Richmond, BG Miran, SL AF Green, David J. Richmond, Brian G. Miran, Sara L. TI Mouse shoulder morphological development responds to locomotor differences in climbing and running. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 79th Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 14-17, 2010 CL Albuquerque, NM SP Amer Assoc Phys Anthropol C1 [Green, David J.] George Washington Univ, Hominid Paleobiol Doctoral Program, Washington, DC 20052 USA. [Green, David J.; Richmond, Brian G.] George Washington Univ, Ctr Adv Study Hominid Paleobiol, Washington, DC 20052 USA. [Green, David J.; Richmond, Brian G.; Miran, Sara L.] George Washington Univ, Dept Anthropol, Washington, DC 20052 USA. [Richmond, Brian G.] Smithsonian Inst, Human Origins Program, Natl Museum Nat Hist, Washington, DC 20560 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 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2010 SU 50 BP 116 EP 116 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 565LT UT WOS:000275295200283 ER PT J AU Griffin, NL Ketcham, RA D'Aout, K Postnov, A De Clerck, N Ryan, TM Richmond, BG AF Griffin, Nicole L. Ketcham, Richard A. D'Aout, Kristiaan Postnov, Andrei De Clerck, Nora Ryan, Tim M. Richmond, Brian G. TI Comparative forefoot trabecular bone architecture in extant hominids. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 79th Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 14-17, 2010 CL Albuquerque, NM SP Amer Assoc Phys Anthropol C1 [Griffin, Nicole L.] Duke Univ, Dept Evolutionary Anthropol, Durham, NC 27706 USA. [Ketcham, Richard A.] Univ Texas Austin, Dept Geol Sci, Austin, TX 78712 USA. [D'Aout, Kristiaan] Univ Antwerp, Dept Biol, Antwerp, Belgium. [D'Aout, Kristiaan] Royal Zool Soc Antwerp, Ctr Res & Conservat, Antwerp, Belgium. [Postnov, Andrei; De Clerck, Nora] Univ Antwerp, Dept Biomed Sci, Antwerp, Belgium. [Ryan, Tim M.] Penn State Univ, Dept Anthropol, University Pk, PA 16802 USA. [Richmond, Brian G.] George Washington Univ, Ctr Adv Study Hominid Paleobiol, Washington, DC 20052 USA. [Richmond, Brian G.] Smithsonian Inst, Human Origins Program, Washington, DC 20560 USA. RI Postnov, Andrey/M-6906-2015 NR 0 TC 0 Z9 0 U1 0 U2 3 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2010 SU 50 BP 117 EP 117 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 565LT UT WOS:000275295200288 ER PT J AU Guatelli-Steinberg, D Ferrell, R Spence, J AF Guatelli-Steinberg, Debbie Ferrell, Rebecca Spence, Jennifer TI Linear enamel hypoplasia as an indicator of physiological stress ingreat apes: reviewing the evidence in light of species differences in enamel growth. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 79th Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 14-17, 2010 CL Albuquerque, NM SP Amer Assoc Phys Anthropol C1 [Guatelli-Steinberg, Debbie; Spence, Jennifer] Ohio State Univ, Dept Anthropol, Columbus, OH 43210 USA. [Ferrell, Rebecca] Smithsonian Inst, Dept Anthropol, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2010 SU 50 BP 118 EP 118 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 565LT UT WOS:000275295200293 ER PT J AU Indriati, E Swisher, CC Lepre, C Quinn, RL Suriyanto, RA Hascaryo, AT Feibel, CS Pobiner, BL Anton, SC AF Indriati, E. Swisher, C. C., III Lepre, C. Quinn, R. L. Suriyanto, R. A. Hascaryo, A. T. Feibel, C. S. Pobiner, B. L. Anton, S. C. TI The age of the 20 meter Solo River Terrace, Ngandong (Java, Indonesia) reconsidered. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 79th Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 14-17, 2010 CL Albuquerque, NM SP Amer Assoc Phys Anthropol C1 [Indriati, E.; Suriyanto, R. A.; Hascaryo, A. T.] Gadjah Mada Univ, Fac Med, Lab Bio & Paleoanthropol, Yogyakarta, Indonesia. [Swisher, C. C., III; Feibel, C. S.] Rutgers State Univ, Dept Earth & Planetary Sci, Piscataway, NJ 08855 USA. [Lepre, C.] William Paterson Univ, Dept Anthropol, Wayne, NJ USA. [Quinn, R. L.] Loyola Univ, Dept Anthropol, New Orleans, LA 70118 USA. [Pobiner, B. L.] Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20560 USA. [Anton, S. C.] NYU, Dept Anthropol, Ctr Study Human Origins, New York, NY 10003 USA. NR 0 TC 1 Z9 1 U1 3 U2 5 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2010 SU 50 BP 132 EP 132 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 565LT UT WOS:000275295200355 ER PT J AU Marden, K Hunt, DR AF Marden, Kerriann Hunt, David R. TI Traumatic lesions and other pathological conditions observed in subadult human remains from Chaco Canyon SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 79th Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 14-17, 2010 CL Albuquerque, NM SP Amer Assoc Phys Anthropol C1 [Marden, Kerriann; Hunt, David R.] Smithsonian Inst, Dept Anthropol, Natl Museum Nat Hist, Washington, DC 20560 USA. [Marden, Kerriann] Tulane Univ, Dept Anthropol, New Orleans, LA 70118 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 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2010 SU 50 BP 163 EP 163 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 565LT UT WOS:000275295200491 ER PT J AU Mckeown, AH May, JE Owsley, DW Kelso, WM Straube, BA AF Mckeown, Ashley H. May, Jamie E. Owsley, Douglas W. Kelso, William M. Straube, Beverly A. TI Life and death Jamestown: Bioarchaeology of an early 17(th)-century colonial cemetery. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 79th Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 14-17, 2010 CL Albuquerque, NM SP Amer Assoc Phys Anthropol C1 [Mckeown, Ashley H.] Univ Montana, Dept Anthropol, Missoula, MT 59812 USA. [Owsley, Douglas W.] Smithsonian Inst, Dept Anthropol, Natl Museum Nat Hist, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 1 U2 6 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2010 SU 50 BP 167 EP 167 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 565LT UT WOS:000275295200510 ER PT J AU Richmond, BG Bennett, MR Harris, JWK Behrensmeyer, AK Braun, DR Carnation, S Chirchir, H Green, DJ Kiura, P Mbua, E AF Richmond, Brian G. Bennett, Matthew R. Harris, John W. K. Behrensmeyer, Anna K. Braun, David R. Carnation, Stevie Chirchir, Habiba Green, David J. Kiura, Purity Mbua, Emma TI The anatomy of footprints from Koobi Fora, Kenya. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 79th Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 14-17, 2010 CL Albuquerque, NM SP Amer Assoc Phys Anthropol C1 [Richmond, Brian G.] George Washington Univ, Ctr Adv Study Hominid Paleobiol, Dept Anthropol, Washington, DC 20052 USA. [Richmond, Brian G.] Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20560 USA. [Bennett, Matthew R.] Bournemouth Univ, Sch Conservat Sci, Poole BH12 5BB, Dorset, England. [Harris, John W. K.] Rutgers State Univ, Dept Anthropol, Piscataway, NJ 08855 USA. [Behrensmeyer, Anna K.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. [Braun, David R.] Univ Cape Town, Dept Archaeol, ZA-7700 Rondebosch, South Africa. [Carnation, Stevie] SUNY Stony Brook, Interdepartmental Doctoral Program Anthropol Sci, Stony Brook, NY USA. [Chirchir, Habiba; Green, David J.] George Washington Univ, Hominid Paleobiol Doctoral Program, Dept Anthropol, Washington, DC 20052 USA. NR 0 TC 3 Z9 3 U1 0 U2 2 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2010 SU 50 BP 197 EP 197 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 565LT UT WOS:000275295200645 ER PT J AU Schroer, KE Gordon, AD Richmond, BG AF Schroer, Katherine E. Gordon, Adam D. Richmond, Brian G. TI How long were australopithecine toes? SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 79th Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 14-17, 2010 CL Albuquerque, NM SP Amer Assoc Phys Anthropol C1 [Schroer, Katherine E.] George Washington Univ, Hominid Palcobiol Doctoral Program, Dept Anthropol, Washington, DC 20052 USA. [Schroer, Katherine E.; Richmond, Brian G.] George Washington Univ, Ctr Adv Study Hominid Paleobiol, Dept Anthropol, Washington, DC 20052 USA. [Gordon, Adam D.] SUNY Albany, Dept Anthropol, Albany, NY 12222 USA. [Richmond, Brian G.] Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2010 SU 50 BP 209 EP 209 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 565LT UT WOS:000275295200699 ER PT J AU Waxenbaum, EB Stock, MK Hunt, DR AF Waxenbaum, Erin B. Stock, Michala K. Hunt, David R. TI Metric assessment of the human bicondylar angle. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 79th Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 14-17, 2010 CL Albuquerque, NM SP Amer Assoc Phys Anthropol C1 [Waxenbaum, Erin B.; Stock, Michala K.] Northwestern Univ, Dept Anthropol, Evanston, IL 60208 USA. [Hunt, David R.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20560 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 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2010 SU 50 BP 239 EP 240 PG 2 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 565LT UT WOS:000275295200830 ER PT J AU Wlliams, EM Richmond, BG AF Wlliams, Erin Marie Richmond, Brian G. TI Hand pressure during Oldowan stone tool production SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 79th Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 14-17, 2010 CL Albuquerque, NM SP Amer Assoc Phys Anthropol C1 [Wlliams, Erin Marie] George Washington Univ, Hominid Paleobiol Doctoral Program, Dept Anthropol, Washington, DC 20052 USA. [Wlliams, Erin Marie; Richmond, Brian G.] George Washington Univ, Ctr Adv Study Hominid Paleobiol, Dept Anthropol, Washington, DC 20052 USA. [Richmond, Brian G.] Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20560 USA. NR 0 TC 1 Z9 1 U1 0 U2 0 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2010 SU 50 BP 243 EP 243 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 565LT UT WOS:000275295200848 ER PT J AU Wood, B AF Wood, Bernard TI The functional and phylogenetic implications of Paranthropus boisei gnathic and dental morphology. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 79th Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 14-17, 2010 CL Albuquerque, NM SP Amer Assoc Phys Anthropol C1 [Wood, Bernard] George Washington Univ, Ctr Adv Study Hominin Paleobiol, Dept Anthropol, Washington, DC USA. [Wood, Bernard] Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, 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 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2010 SU 50 BP 246 EP 247 PG 2 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 565LT UT WOS:000275295200862 ER PT J AU Loaiza, JR Scott, ME Bermingham, E Rovira, J Conn, JE AF Loaiza, Jose R. Scott, Marilyn E. Bermingham, Eldredge Rovira, Jose Conn, Jan E. TI Evidence for Pleistocene Population Divergence and Expansion of Anopheles albimanus in Southern Central America SO AMERICAN JOURNAL OF TROPICAL MEDICINE AND HYGIENE LA English DT Article ID MITOCHONDRIAL-DNA ANALYSIS; GENE FLOW; STATISTICAL TESTS; COALESCENT THEORY; DARLINGI DIPTERA; CLIMATE-CHANGE; HISTORY; MALARIA; PANAMA; CULICIDAE AB The micro-geographic structure of Anopheles albimanus was studied in southern Central America using partial sequences of the mtDNA cytochrome oxidase subunit I gene (COI). Analysis of molecular variance supported significant genetic structure between populations from Costa Rica and western Panama versus those from central-eastern Panama (Phi(CT)=0.33), whereas the within group divergence was shallow and statistically insignificant (Phi(ST)=0.08). Furthermore, a statistical parsimony network depicted three divergent groups of haplotypes that were not evenly distributed across the study area. Our findings are in partial agreement with previous studies, yet they do not support physical barriers to gene flow or contemporary isolation by distance in this region. Instead, three co-occurring groups of An. albimanus may be the result of multiple introductions, most likely caused by historical fragmentation and subsequent secondary contact. In addition, the molecular signature of population expansion of An. albimanus was detected in central-eastern Panama approximately 22,000 years ago (95% confidence interval [CI] 10,183-38,1.69). We hypothesize that the population structure of An. albimanus, as determined by our COI locus analysis, is the result of late Pleistocene climatic changes in northern South America. C1 [Loaiza, Jose R.; Scott, Marilyn E.] McGill Univ, Dept Nat Resource Sci, Ste Anne De Bellevue, PQ H9X 3V9, Canada. McGill Univ, Inst Parasitol, Montreal, PQ H3A 2T5, Canada. [Bermingham, Eldredge] Smithsonian Trop Res Inst, Balboa Ancon, Panama. [Rovira, Jose] Inst Conmemorat Gorgas Estudios Salud, Dept Med Entomol, Panama City, Panama. [Conn, Jan E.] New York State Dept Hlth, Wadsworth Ctr, Griffin Lab, Slingerlands, NY USA. RP Loaiza, JR (reprint author), McGill Univ, Dept Nat Resource Sci, 21,111 Lakeshore Rd, Ste Anne De Bellevue, PQ H9X 3V9, Canada. EM jose.loaiza@mail.mcgill.ca; marilyn.scott@mcgill.ca; bermingham@si.edu; jrovira@gorgas.gob.pa; jconn@wadsworth.org RI Scott, Marilyn/L-5347-2015; OI Conn, Jan/0000-0002-5301-7020 FU Secretariat for Science, Technology and Innovation of Panama (SENACYT) [COL08-066]; Smithsonian Tropical Research Institute (STRI); Organization of American States (OAS); Natural Sciences and Engineering Research Council of Canada (NSERC); National Institutes of Health (NIH) [(AI) R0154139-02]; Fonds Quebecois de la recherche sur la nature et les technologies (FQRNT) FX The Secretariat for Science, Technology and Innovation of Panama (SENACYT) through a scholarship and research grant COL08-066 awarded to Jose Loaiza, partially financed this research. Additional financial support was provided by the Smithsonian Tropical Research Institute (STRI), the Organization of American States (OAS), Natural Sciences and Engineering Research Council of Canada (NSERC), and National Institutes of Health (NIH) grant (AI) R0154139-02 to JEC. Research at the Institute of Parasitology is supported by a regroupement strategique from Fonds Quebecois de la recherche sur la nature et les technologies (FQRNT). NR 63 TC 22 Z9 22 U1 0 U2 6 PU AMER SOC TROP MED & HYGIENE PI MCLEAN PA 8000 WESTPARK DR, STE 130, MCLEAN, VA 22101 USA SN 0002-9637 J9 AM J TROP MED HYG JI Am. J. Trop. Med. Hyg. PD JAN PY 2010 VL 82 IS 1 BP 156 EP 164 DI 10.4269/ajtmh.2010.09-0423 PG 9 WC Public, Environmental & Occupational Health; Tropical Medicine SC Public, Environmental & Occupational Health; Tropical Medicine GA 540VF UT WOS:000273367400030 PM 20065014 ER PT J AU Baugh, AT Ryan, MJ AF Baugh, Alexander T. Ryan, Michael J. TI Temporal updating during phonotaxis in male tungara frogs (Physalaemus pustulosus) SO AMPHIBIA-REPTILIA LA English DT Article DE acoustic communication; male phonotaxis; Physalaemus pustulosus; temporal updating ID MATE CHOICE; ADVERTISEMENT CALLS; MIDWIFE TOADS; BEHAVIOR; SIGNALS; FREQUENCY AB In acoustically advertising anurans the male courtship call elicits species-typical responses from conspecifics - usually phonotactic approach and mate choice in gravid females and an evoked vocal response in adult males. Males in several species, however, are also known to perform phonotaxis, sometimes with the same acoustic preferences as females. Female tungara frogs are known to update their phonotactic approach as male advertisement signals change dynamically in attractiveness. Here we show that males also perform such temporal updating during phonotaxis in response to dynamic playbacks. While males exhibit slower phonotactic approaches than females, their responsiveness to dynamic changes in call complexity does not differ significantly compared to females. These results demonstrate that males are sensitive to the location of preferred call types on a moment-to-moment basis and suggest that similarities between male and female sexual behaviour in anurans might often be overlooked. We suggest that anuran phonotaxis is more widespread and serves different functions in reproductive females and males. Lastly, these temporal updating results suggest that male frogs are highly selective about site selection in a chorus. C1 [Baugh, Alexander T.] Univ Texas Austin, Sect Integrat Biol, Austin, TX 78712 USA. [Ryan, Michael J.] Smithsonian Trop Res Inst, Balboa Ancon, Panama. RP Baugh, AT (reprint author), Max Planck Inst Ornithol, Deparment Migrat & Immunoecol, Schlossallee 2, D-78315 Radolfzell am Bodensee, Germany. EM alex.baugh@gmail.com RI Baugh, Alexander/E-4777-2010; OI Baugh, Alexander/0000-0003-2032-892X FU NSF [IOB 0544096] FX We would like to thank the two anonymous reviewers whose insightful comments improved this manuscript. The Smithsonian Tropical Research Institute provided logistical support for this study and Autoridad Nacional del Ambiente approved scientific permits in the Republic of Panama. Funding was contributed by NSF grant number IOB 0544096 to M. Ryan. Animal use was approved by the IACUC (06041701) at The University of Texas at Austin. NR 25 TC 0 Z9 0 U1 0 U2 4 PU BRILL ACADEMIC PUBLISHERS PI LEIDEN PA PLANTIJNSTRAAT 2, P O BOX 9000, 2300 PA LEIDEN, NETHERLANDS SN 0173-5373 J9 AMPHIBIA-REPTILIA JI Amphib. Reptil. PY 2010 VL 31 IS 4 BP 449 EP 454 DI 10.1163/017353710X518388 PG 6 WC Zoology SC Zoology GA 676PH UT WOS:000283924000001 ER PT J AU Lattanzi, V Thorwirth, S Halfen, DT Muck, LA Ziurys, LM Thaddeus, P Gauss, J McCarthy, MC AF Lattanzi, Valerio Thorwirth, Sven Halfen, DeWayne T. Mueck, Leonie Anna Ziurys, Lucy M. Thaddeus, Patrick Gauss, Juergen McCarthy, Michael C. TI Bonding in the Heavy Analogue of Hydrogen Cyanide: The Curious Case of Bridged HPSi SO ANGEWANDTE CHEMIE-INTERNATIONAL EDITION LA English DT Article DE multiple bonds; phosphorous; quantum-chemical calculations; rotational spectroscopy; silicon ID SILICON-CONTAINING MOLECULES; X-RAY-STRUCTURE; SILYLIDENE-PHOSPHANES; MICROWAVE-SPECTRA; GROUND-STATE; PHOSPHORUS; IRC+10216; PHOSPHINE; PHOSPHASILENES; ARSANES C1 [Mueck, Leonie Anna; Gauss, Juergen] Johannes Gutenberg Univ Mainz, Inst Phys Chem, D-55099 Mainz, Germany. [Lattanzi, Valerio; Thaddeus, Patrick; McCarthy, Michael C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lattanzi, Valerio; Thaddeus, Patrick; McCarthy, Michael C.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. [Thorwirth, Sven] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Thorwirth, Sven] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Halfen, DeWayne T.; Ziurys, Lucy M.] Univ Arizona, Dept Chem, Tucson, AZ 85721 USA. [Halfen, DeWayne T.; Ziurys, Lucy M.] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. [Halfen, DeWayne T.; Ziurys, Lucy M.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Gauss, J (reprint author), Johannes Gutenberg Univ Mainz, Inst Phys Chem, D-55099 Mainz, Germany. EM gauss@uni-mainz.de; mccarthy@cfa.harvard.edu RI Thorwirth, Sven/C-6217-2011; OI Thorwirth, Sven/0000-0001-8200-6710; McCarthy, Michael/0000-0001-9142-0008; Mueck, Leonie/0000-0002-9890-5451; Halfen, DeWayne/0000-0003-2483-3616 FU National Science Foundation (NSF) Center for Chemical Innovation (CCI) [CHE 08-47919]; NSF [AST 06-02282]; Deutsche Forschungsgemeinschaft (DFG) [TH1301/3-1, GA370/5-1]; Graduate School of Excellence "MAINZ" FX Financial support for the work in Cambridge and Tucson is provided by the National Science Foundation (NSF) Center for Chemical Innovation (CCI) grant CHE 08-47919. D.T.H. is supported by a NSF Astronomy and Astrophysics Post-doctoral Fellowship (AST 06-02282). S.T. and J.G. gratefully acknowledge funding by the Deutsche Forschungsgemeinschaft (DFG) through grants TH1301/3-1 and GA370/5-1. L.A.M. is supported by a fellowship by the Graduate School of Excellence "MAINZ". NR 31 TC 20 Z9 20 U1 0 U2 4 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA PO BOX 10 11 61, D-69451 WEINHEIM, GERMANY SN 1433-7851 J9 ANGEW CHEM INT EDIT JI Angew. Chem.-Int. Edit. PY 2010 VL 49 IS 33 BP 5661 EP 5664 DI 10.1002/anie.201001938 PG 4 WC Chemistry, Multidisciplinary SC Chemistry GA 638JP UT WOS:000280891000008 PM 20818754 ER PT J AU Baugh, AT Ryan, MJ AF Baugh, Alexander T. Ryan, Michael J. TI Mate choice in response to dynamic presentation of male advertisement signals in tungara frogs SO ANIMAL BEHAVIOUR LA English DT Article DE acoustic communication; decision-making process; mate choice; phonotaxis; Physalaemus pustulosus; temporal updating; tungara frog ID PHYSALAEMUS-PUSTULOSUS; ARGININE VASOTOCIN; SEXUAL SELECTION; FEMALE PREFERENCE; NEOTROPICAL FROG; CALLING BEHAVIOR; CRICKET FROGS; TRAITS; STRATEGIES; PHONOTAXIS AB Signalling is a dynamic process that often occurs over brief timescales, particularly in the acoustic modality. Numerous studies of mate choice and acoustic communication have identified signal parameters essential for species recognition and mate preferences, although these studies have rarely considered the dynamic nature of these processes. Here we investigate mate choice behaviour in female tungara frogs, Physalaemus pustulosus, in response to temporally dynamic presentations of male advertisement calls. Our results demonstrate that females are sensitive to the location of preferred call types on a moment-to-moment basis, and that responses are influenced by the continued presence, complexity, sound pressure level and inherent attractiveness of individual male signals. In general, our results support the notion that decision making during mate choice is an open-ended process that is sensitive to interruption and persuasion from competing signallers. We show that for a species in which females actively compare multiple signallers simultaneously, the criterion that predicts the degree of commitment to an initial mate approach is whether there is a state change in the complexity of signals. (C) 2009 The Association for the Study of Animal Behaviour. Published by Elsevier Ltd. All rights reserved. C1 [Baugh, Alexander T.; Ryan, Michael J.] Univ Texas Austin, Sect Integrat Biol, Austin, TX 78712 USA. [Baugh, Alexander T.; Ryan, Michael J.] Univ Texas Austin, Inst Neurosci, Austin, TX 78712 USA. [Ryan, Michael J.] Smithsonian Trop Res Inst, Balboa Ancon, Panama. RP Baugh, AT (reprint author), Univ Texas Austin, Sect Integrat Biol, 1 Univ Stn,C0930, Austin, TX 78712 USA. EM baugh@mail.utexas.edu RI Baugh, Alexander/E-4777-2010; OI Baugh, Alexander/0000-0003-2032-892X FU National Science Foundation [IOB 0544096]; University of Texas at Austin [06041701] FX We thank A. Dapper, N. Lessios, A. Lea and L. Ziegler for their assistance with data collection and two anonymous referees for improving this manuscript. The Smithsonian Tropical Research Institute provided logistical support for this study and Autoridad Nacional del Ambiente approved scienti. c permits in the Republic of Panama. Funding was contributed by National Science Foundation grant number IOB 0544096 to M.J. Ryan. Animal use was approved by the IACUC (no. 06041701) at The University of Texas at Austin. NR 44 TC 21 Z9 21 U1 2 U2 14 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0003-3472 EI 1095-8282 J9 ANIM BEHAV JI Anim. Behav. PD JAN PY 2010 VL 79 IS 1 BP 145 EP 152 DI 10.1016/j.anbehav.2009.10.015 PG 8 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA 536EY UT WOS:000273027500019 ER PT J AU Sberze, M Cohn-Haft, M Ferraz, G AF Sberze, M. Cohn-Haft, M. Ferraz, G. TI Old growth and secondary forest site occupancy by nocturnal birds in a neotropical landscape SO ANIMAL CONSERVATION LA English DT Article DE secondary forest; old growth; nocturnal birds; occupancy; detection; spatial autocorrelation; Amazon forest ID UNCERTAIN FUTURE; BRAZILIAN AMAZON; LAND-USE; COMMUNITIES; FRAGMENTS; PROBABILITIES; BIODIVERSITY; ASSEMBLAGES; CLIMATE; POINT AB High rates of old growth (OG) forest destruction and difficult farming conditions result in increasing cover of secondary forests (SF) in the Amazon. In this setting, it is opportune to ask which animals use newly available SF and which stay restricted to OG. This study presents a comparison of SF and OG site occupancy by nocturnal birds in terra firme forests of the Amazon Guianan shield, north of Manaus, Brazil. We tested species-specific occupancy predictions for two owls (Lophostrix cristata/Glaucidium hardyi), two potoos (Nyctibius leucopterus/Nyctibius griseus) and two nightjars (Caprimulgus nigrescens/Nyctidromus albicollis). For each pair, we predicted that one species would have higher occupancy in OG while the other would either be indifferent to forest type or favor SF sites. Data were collected in 30 OG and 24 SF sites with monthly samples from December 2007 to December 2008. Our analytic approach accounts for the possibility of detection failure and for spatial autocorrelation in occupancy, thus leading to strong inferences about changes in occupancy between forest types and between species. Nocturnal bird richness and community composition were indistinguishable between OG and SF sites. Owls were relatively indifferent to forest type. Potoos followed the a priori predictions, and one of the nightjars (C. nigrescens) favored SF instead of OG as predicted. Only one species, Nyctib. leucopterus, clearly favored OG. The landscape context of our SF study sites, surrounded by a vast expanse of continuous OG forest, partially explains the resemblance between SF and OG fauna but leaves unexplained the higher occupancy for SF than OG sites for several study species. The causal explanation of high SF occupancy remains an open question, but the result itself motivates further comparisons for other groups, as well as recognition of the conservation potential of SF. C1 [Sberze, M.; Ferraz, G.] Smithsonian Trop Res Inst, Inst Nacl Pesquisas Amazonia, Biol Dynam Forest Fragments Project, BR-69011970 Manaus, Brazil. [Cohn-Haft, M.] Inst Nacl de Pesquisas da Amazonia, Ecol Dept & Sci Collect Birds, Manaus, Brazil. [Ferraz, G.] Fiocruz MS, Inst Leonidas & Maria Deane, Manaus, Brazil. RP Ferraz, G (reprint author), Smithsonian Trop Res Inst, Inst Nacl Pesquisas Amazonia, Biol Dynam Forest Fragments Project, Av Andre Araujo 1753, BR-69011970 Manaus, Brazil. EM ferrazg@si.edu RI Ferraz, Goncalo/C-3860-2008 OI Ferraz, Goncalo/0000-0001-8748-0462 NR 58 TC 19 Z9 19 U1 3 U2 17 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1367-9430 EI 1469-1795 J9 ANIM CONSERV JI Anim. Conserv. PD JAN PY 2010 VL 13 IS 1 BP 3 EP 11 DI 10.1111/j.1469-1795.2009.00312.x PG 9 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 550RA UT WOS:000274144800002 ER PT J AU Dent, DH AF Dent, D. H. TI Defining the conservation value of secondary tropical forests SO ANIMAL CONSERVATION LA English DT Editorial Material ID UNCERTAIN FUTURE; BIODIVERSITY; BUTTERFLIES; COMMUNITIES; EXTINCTION; FRAGMENTS C1 Smithsonian Trop Res Inst, Balboa, Panama. RP Dent, DH (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Panama. EM daisy.h.dent@gmail.com RI Dent, Daisy/L-3549-2016 OI Dent, Daisy/0000-0002-1219-7344 NR 21 TC 4 Z9 4 U1 1 U2 13 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1367-9430 J9 ANIM CONSERV JI Anim. Conserv. PD JAN PY 2010 VL 13 IS 1 BP 14 EP 15 DI 10.1111/j.1469-1795.2010.00346.x PG 2 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 550RA UT WOS:000274144800004 ER PT J AU Ferraz, G Sberze, M Cohn-Haft, M AF Ferraz, G. Sberze, M. Cohn-Haft, M. TI Using occupancy estimates to fine-tune conservation concerns RESPONSE SO ANIMAL CONSERVATION LA English DT Editorial Material ID BIODIVERSITY; EXTINCTION C1 [Ferraz, G.; Sberze, M.] Smithsonian Trop Res Inst, Inst Nacl Pesquisas Amazonia, Biol Dynam Forest Fragments Project, Manaus, Brazil. [Cohn-Haft, M.] Inst Nacl de Pesquisas da Amazonia, Ecol Dept & Sci Collect Birds, Manaus, Brazil. RP Ferraz, G (reprint author), Smithsonian Trop Res Inst, Inst Nacl Pesquisas Amazonia, Biol Dynam Forest Fragments Project, Manaus, Brazil. RI Ferraz, Goncalo/C-3860-2008 OI Ferraz, Goncalo/0000-0001-8748-0462 NR 13 TC 2 Z9 2 U1 0 U2 3 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1367-9430 J9 ANIM CONSERV JI Anim. Conserv. PD JAN PY 2010 VL 13 IS 1 BP 19 EP 20 PG 2 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 550RA UT WOS:000274144800006 ER PT J AU Oliveira, LC Hankerson, SJ Dietz, JM Raboy, BE AF Oliveira, L. C. Hankerson, S. J. Dietz, J. M. Raboy, B. E. TI Key tree species for the golden-headed lion tamarin and implications for shade-cocoa management in southern Bahia, Brazil SO ANIMAL CONSERVATION LA English DT Article DE Leontopithecus chrysomelas; diet; sleeping sites; agroforest; cabruca management; Atlantic forest ID ATLANTIC FOREST TREES; CACAO PLANTATIONS; LEONTOPITHECUS-CHRYSOMELAS; BIODIVERSITY CONSERVATION; SOUTHEASTERN BRAZIL; LANDSCAPE; AGROFORESTRY; DIVERSITY; BEHAVIOR; ECOLOGY AB The golden-headed lion tamarin Leontopithecus chrysomelas occurs in the Atlantic forest of southern Bahia, Brazil, where shade-cocoa agroforestry (known as cabruca) predominates. The economic decline of the cocoa industry has caused many landowners to convert cabruca into cattle pasture or diversify their plantations with other crops. These and prior anthropogenic disturbances such as habitat fragmentation are threatening lion tamarin persistence. For some lion tamarin groups, cabruca comprises a large part of their home range. Considering these factors, the maintenance of the biological diversity in cabruca favorable to golden-headed lion tamarins is of considerable interest to their long-term survival. Here we identify plant species that provide food and sleeping sites for the lion tamarins and examine their occurrence in cabruca plantations, in order to investigate alternatives for conservation management practices that benefit both lion tamarins and cabruca. We determined the total number of trees and the frequency of individuals and species used for food and sleeping sites by lion tamarins in Una Biological Reserve, Bahia, from 1998 to 2006. We used this information to compare the richness and frequency of use across habitats (cabruca, mature and secondary) and to create a ranking index considering various components of a tree species' utility to the lion tamarins. Lion tamarins used 155 tree species, 93 for food and 93 for sleeping sites. Fifty-five species were ranked as 'Extremely Valuable,' eight as 'Valuable' and 92 as 'Of Interest.' Of 48 families, Myrtaceae and Sapotaceae were used the most. Cabruca contained fewer individual trees used by lion tamarins, but the highest frequency of use per tree compared with other habitats, indicating the large influence of single trees in these plantations. Using the key tree species identified in our study in the management of cabruca would be of considerable benefit to the long-term survival of lion tamarins. C1 [Oliveira, L. C.; Dietz, J. M.; Raboy, B. E.] IESB, BR-45653145 Salvador, Brazil. [Oliveira, L. C.] Univ Maryland, Dept Biol, College Pk, MD 20742 USA. [Hankerson, S. J.] Univ Maryland, Grad Program Behav Ecol Evolut & Systemat, College Pk, MD 20742 USA. [Raboy, B. E.] Smithsonian Inst, Natl Zool Pk, Dept Conservat Biol, Washington, DC 20008 USA. RP Oliveira, LC (reprint author), IESB, Rua Araujo Pinho,72-3 Andar Ctr Ilheus, BR-45653145 Salvador, Brazil. EM leoecol@umd.edu RI Oliveira, Leonardo/G-1290-2012 OI Oliveira, Leonardo/0000-0002-1774-0713 FU Lion Tamarins of Brazil Fund; Durrell Wildlife Conservation Trust; Margot Marsh Biodiversity Foundation; Tulsa Zoo; Sigma Xi; NSF; Wildlife Conservation Society; International Foundation of Science; The Rufford Small Grants Foundation; Idea Wild; Brazilian Higher Education Authority (Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior) FX We thank the Brazilian Institute of Environment and Renewable Natural Resources (Instituto Brasileiro do Meio Ambiente e dos Recursos Naturais Renovaveis), especially Saturnino Neto de Sousa and Paulo Cesar Cruz, for allowing us to work in Una Biological Reserve and for the use of the reserve headquarters. We are grateful to the owners of the Fazenda Incom for allowing us access to their cabruca forest while studying our focal groups. We also thank our field assistants Daniel Batista, Gilvan Gomes Mota, Gilvanio Gomes Mota, Jose Renato and Jiomario dos Santos Souza. Andre M. de Carvalho, Jomar Gomes Jardim and Sergio Sant'Ana from the Cacao Research Center (Centro de Pesquisas do Cacau) of the Executive Commission for Cacao Cultivation (CEPLAC), Itabuna, and Ze Lima da Paixao from the Santa Cruz State University (UESC), Itabuna, identified the plants. We are grateful to Gotz Schroth for suggestions on an earlier version of the paper. Financial support was kindly provided to B. E. R. and J. M. D. by the Lion Tamarins of Brazil Fund, the Durrell Wildlife Conservation Trust, the Margot Marsh Biodiversity Foundation, and the Tulsa Zoo, to B. E. R. by Sigma Xi, and to L. C. O. from the NSF (Research and Training Grant to the University of Maryland), Seeds of Change, the Wildlife Conservation Society, International Foundation of Science, The Rufford Small Grants Foundation and Idea Wild. L. C. O. received a Brazilian Higher Education Authority (Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior)/Fulbright Fellowship for PhD. NR 41 TC 19 Z9 19 U1 5 U2 37 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1367-9430 J9 ANIM CONSERV JI Anim. Conserv. PD JAN PY 2010 VL 13 IS 1 BP 60 EP 70 DI 10.1111/j.1469-1795.2009.00296.x PG 11 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 550RA UT WOS:000274144800013 ER PT J AU Senda, A Hatakeyama, E Kobayashi, R Fukuda, K Uemura, Y Saito, T Packer, C Oftedal, OT Urashima, T AF Senda, Akitsugu Hatakeyama, Emi Kobayashi, Rui Fukuda, Kenji Uemura, Yusuke Saito, Tadao Packer, Craig Oftedal, Olav T. Urashima, Tadasu TI Chemical characterization of milk oligosaccharides of an African lion (Panthera leo) and a clouded leopard (Neofelis nebulosa) SO ANIMAL SCIENCE JOURNAL LA English DT Article DE African lion; carnivora; clouded leopard; felidae; milk oligosaccharides ID POLAR BEAR; COLOSTRUM; SAMPLE; TRISACCHARIDES AB The Carnivora include the superfamilies Canoidea and Feloidea. In species of Canoidea other than the domestic dog, Canis lupus, the milk contains only traces of lactose and much larger concentrations of oligosaccharides. In this study, lactose was found to be the dominant saccharide in the milk or colostrum of two species of Feloidea, namely the African lion (Panthera leo) and the clouded leopard (Neofelis nebulosa). In addition to lactose, the following oligosaccharides were characterized in the milk of a lion; Neu5Gc(alpha 2-3)Gal(beta 1-4)Glc (3'-NGc-SL), Fuc(alpha 1-2)Gal(beta 1-4)Glc (2'-fucosyllactose) and GalNAc(alpha 1-3)[Fuc(alpha 1-2)]Gal(beta 1-4)Glc (A-tetrasaccharide). The colostrum of a clouded leopard contained 3'-NGc-SL, Gal(alpha 1-3)Gal(beta 1-4)Glc (isoglobotriose) and A-tetrasaccharide. These oligosaccharides differ in some respects from those previously identified in another species of Feloidea, the spotted hyena (Crocuta crocuta). These milks contained 3'-NGc-SL and A-tetrasaccharide, while spotted hyena colostrum did not; however, it contained Neu5Ac(alpha 2-3)Gal(beta 1-4)Glc (3'-NAc-SL) and Gal(alpha 1-3)[Fuc(alpha 1-2)]Gal(beta 1-4)Glc (B-tetrasaccharide). C1 [Senda, Akitsugu; Hatakeyama, Emi; Fukuda, Kenji; Urashima, Tadasu] Obihiro Univ Agr & Vet Med, Grad Sch Food Hyg, Obihiro, Hokkaido 0808555, Japan. [Kobayashi, Rui] Obihiro Univ Agr & Vet Med, Dept Bioresource Chem, Obihiro, Hokkaido 0808555, Japan. [Uemura, Yusuke] Kitasato Univ, Sch Sci, Dept Chem, Sagamihara, Kanagawa 228, Japan. [Saito, Tadao] Tohoku Univ, Grad Sch Agr, Sendai, Miyagi 980, Japan. [Packer, Craig] Univ Minnesota, Dept Ecol Evolut & Behav, St Paul, MN 55108 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 FU Ministry of Education, Culture, Sports, Science, and Technology, Japan FX This study was partially supported from a grant from Global COE Program 'Frontier Program for Animal Global Health and Hygiene', Ministry of Education, Culture, Sports, Science, and Technology, Japan. We thank Dr JeffWyatt of the Seneca Park Zoo, Rochester, NY for providing the clouded leopard colostrum samples, and Tanzania Wildlife Research Institute for authorization to sample lions in Serengeti National Park, Tanzania. Michael Jakubasz of the Nutrition Laboratory, National Zoological Park, Washington DC assisted with initial processing of the samples. NR 30 TC 5 Z9 5 U1 0 U2 8 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1344-3941 J9 ANIM SCI J JI Anim. Sci. J. PY 2010 VL 81 IS 6 BP 687 EP 693 DI 10.1111/j.1740-0929.2010.00787.x PG 7 WC Agriculture, Dairy & Animal Science SC Agriculture GA 685QS UT WOS:000284643800010 PM 21108689 ER PT J AU Diver, K AF Diver, Kim TI Beyond Area and Isolation: Forest Dynamics and Change in Plant Species Richness Patterns on Islands SO ANNALS OF THE ASSOCIATION OF AMERICAN GEOGRAPHERS LA English DT Article DE forest dynamics; Great Lakes; island biogeography; species richness; white pine ID SOUTHERN-BOREAL FOREST; PINUS-STROBUS L.; WHITE-PINE; SPATIAL PATTERNS; AGE STRUCTURE; SUCCESSION; VEGETATION; BIOGEOGRAPHY; DIVERSITY; QUEBEC AB As an alternative to classic island biogeography analyses (i.e., species-area and species-isolation relationships), the influence of overstory dominance and regeneration on understory plant species richness was examined on temperate, freshwater islands. Research analyses tested whether understory species richness correlated with overstory species richness; whether plant species richness correlated with the number of dominant tree species on an island; whether plant species richness differed between islands with dissimilar canopy dominants; and whether the current overstory tree species are regenerating on the islands. Thirty-five islands were sampled from Ontario's Massasauga Provincial Park. Sampled islands were located using stratified random selection based on variations in size and location. Species richness was recorded along transects on each island. Forest data (e.g., stem counts, diameter measurements) were collected in stratified random quadrats along the transects. Understory species richness was correlated with overstory species richness. The twenty-seven islands dominated (as indicated by importance values) by Pinus strobus L. (Eastern white pine) had greater species richness than islands with nonpine dominance. Islands dominated by multiple overstory tree species had larger overall plant species richness than islands with one dominant tree species. Regeneration trends indicated that current overstory dominance will persist. Size-class distributions, however, suggest that large and round islands are likely to shift in dominance from pine to pine-oak dominance, which is expected to correlate with an increase in overall plant species richness. The results provide a baseline set of hypotheses for research using this approach in a host of geographic regions. C1 Smithsonian Trop Res Inst, DPO, FL 34002 USA. RP Diver, K (reprint author), Smithsonian Trop Res Inst, Attn Kim Diver MRC 0580-12,Unit 9100 Box 0948, DPO, FL 34002 USA. EM diverkc@gmail.com NR 42 TC 2 Z9 2 U1 1 U2 13 PU ROUTLEDGE JOURNALS, TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXFORDSHIRE, ENGLAND SN 0004-5608 EI 1467-8306 J9 ANN ASSOC AM GEOGR JI Ann. Assoc. Am. Geogr. PY 2010 VL 100 IS 5 BP 1110 EP 1127 AR PII 928640198 DI 10.1080/00045608.2010.517738 PG 18 WC Geography SC Geography GA 682PV UT WOS:000284416400007 ER PT S AU Bastian, N Covey, KR Meyer, MR AF Bastian, Nate Covey, Kevin R. Meyer, Michael R. BE Blandford, R Faber, SM VanDishoeck, E Kormendy, J TI A Universal Stellar Initial Mass Function? A Critical Look at Variations SO ANNUAL REVIEW OF ASTRONOMY AND ASTROPHYSICS, VOL 48 SE Annual Review of Astronomy and Astrophysics LA English DT Review; Book Chapter DE chemical evolution of galaxies; galaxy evolution; star formation; stellar clusters; stellar populations; substellar objects ID STAR-FORMING REGION; LARGE-MAGELLANIC-CLOUD; ORION NEBULA CLUSTER; TELESCOPE ACS OBSERVATIONS; TO-LIGHT RATIOS; NEAREST STARBURST CLUSTER; TULLY-FISHER RELATION; MAIN-SEQUENCE STARS; YOUNG OPEN CLUSTERS; METAL-POOR STARS AB Whether the stellar initial mass function (IMF) is universal or is instead sensitive to environmental conditions is of critical importance: The IMF influences most observable properties of stellar populations and thus galaxies, and detecting variations in the IMF could provide deep insights into the star formation process. This review critically examines reports of IMF variations, with a view toward whether other explanations are sufficient given the evidence. Studies of the field, young clusters and associations, and old globular clusters suggest that the vast majority were drawn from a universal system IMF: a power law of Salpeter index (Gamma = 1.35) above a few solar masses, and a log normal or shallower power law (Gamma similar to 0-0.25) for lower mass stars. The shape and universality of the substellar IMF is still under investigation. Observations of resolved stellar populations and the integrated properties of most galaxies are also consistent with a universal IMF, suggesting no gross variations over much of cosmic time. Indications of "nonstandard" IMFs in specific local and extragalactic environments clearly warrant further study. However, there is no clear evidence that the IMF varies strongly and systematically as a function of initial conditions after the first few generations of stars. C1 [Bastian, Nate] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Covey, Kevin R.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Covey, Kevin R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Meyer, Michael R.] Swiss Fed Inst Technol, Inst Astron, CH-8093 Zurich, Switzerland. [Meyer, Michael R.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Bastian, N (reprint author), Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. EM bastian@ast.cam.ac.uk; kcovey@astro.cornell.edu; mmeyer@phys.ethz.ch OI Covey, Kevin/0000-0001-6914-7797 NR 326 TC 386 Z9 387 U1 2 U2 18 PU ANNUAL REVIEWS PI PALO ALTO PA 4139 EL CAMINO WAY, PO BOX 10139, PALO ALTO, CA 94303-0897 USA SN 0066-4146 BN 978-0-8243-0948-0 J9 ANNU REV ASTRON ASTR JI Annu. Rev. Astron. Astrophys. PY 2010 VL 48 BP 339 EP 389 DI 10.1146/annurev-astro-082708-101642 PG 51 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BRK23 UT WOS:000282902900010 ER PT J AU Kurtz, MJ Bollen, J AF Kurtz, Michael J. Bollen, Johan TI Usage Bibliometrics SO ANNUAL REVIEW OF INFORMATION SCIENCE AND TECHNOLOGY LA English DT Article ID ASTROPHYSICS DATA SYSTEM; ELECTRONIC JOURNAL USAGE; OPEN-ACCESS ARTICLES; CITATION ANALYSIS; HALF-LIFE; INFORMATION-RETRIEVAL; SCIENTIFIC WORKFLOWS; DIGITAL LIBRARY; SCIENCE POLICY; SEARCH PROCESS C1 [Kurtz, Michael J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bollen, Johan] Los Alamos Natl Lab, Res Lib, Digital Lib Res & Prototyping Team, Los Alamos, NM USA. RP Kurtz, MJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM kurtz@cfa.harvard.edu; jbollen@lanl.gov RI KURTZ, Michael /B-3890-2009; OI Kurtz, Michael/0000-0002-6949-0090 FU NASA [NCC5-189]; Andrew W. Mellon Foundation; Digital Library Research and Prototyping Team at the Research Library of the Los Alamos National Laboratory FX Michael Kurtz would like to acknowledge the long term collaboration with the Astrophysics Data System (ADS) group at the Smithsonian Astrophysical Observatory, especially Guenther Eichhorn, Alberto Accomazzi, and Edwin Henneken. The ADS is supported by NASA grant NCC5-189. Johan Bollen would like to thank Herbert Van de Sompel and the Digital Library Research and Prototyping Team at the Research Library of the Los Alamos National Laboratory for their support in developing many of the ideas and much of the research presented in this paper. The Andrew W. Mellon Foundation supported the MESUR project to develop usage-based impact metrics from 2006 to 2008. NR 170 TC 36 Z9 36 U1 7 U2 50 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0066-4200 J9 ANNU REV INFORM SCI JI Annu. Rev. Inform. Sci. Technol. PY 2010 VL 44 BP 3 EP 64 PG 62 WC Computer Science, Information Systems; Information Science & Library Science SC Computer Science; Information Science & Library Science GA 818XK UT WOS:000294789800002 ER PT J AU Erlandson, JM Rick, TC AF Erlandson, Jon M. Rick, Torben C. TI Archaeology Meets Marine Ecology: The Antiquity of Maritime Cultures and Human Impacts on Marine Fisheries and Ecosystems SO ANNUAL REVIEW OF MARINE SCIENCE SE Annual Review of Marine Science LA English DT Review; Book Chapter DE fishing; deep history; hunter-gatherers; agriculturalists; shifting timelines ID MIDDLE STONE-AGE; CALIFORNIA CHANNEL-ISLANDS; KELP FOREST ECOSYSTEMS; SOUTH-AFRICA; EASTER-ISLAND; ANTHROPOGENIC IMPACTS; AUSTRALIAN MEGAFAUNA; RESOURCE DEPRESSION; HUMAN EXPLOITATION; NORTH-ATLANTIC AB Interdisciplinary study of coastal archaeological sites provides a wealth of information on the ecology and evolution of ancient marine animal populations, the structure of past marine ecosystems, and the history of human impacts on coastal fisheries. In this paper, we review recent methodological developments in the archaeology and historical ecology of coastal regions around the world. Using two case studies, we examine (a) a deep history of anthropogenic effects on the marine ecosystems of California's Channel Islands through the past 12,000 years and (b) geographic variation in the effects of human fishing on Pacific Island peoples who spread through Oceania during the late Holocene. These case studies-the first focused on hunter-gatherers, die second on maritime horticulturalists-provide evidence for shifting baselines and timelines, documenting a much deeper anthropogenic influence oil many coastal ecosystems and fisheries than considered by most ecologists, conservation biologists, and fisheries managers. C1 [Erlandson, Jon M.] Univ Oregon, Dept Anthropol, Eugene, OR 97403 USA. [Erlandson, Jon M.] Univ Oregon, Museum Nat & Cultural Hist, Eugene, OR 97403 USA. [Rick, Torben C.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Archaeobiol Program, Washington, DC 20013 USA. RP Erlandson, JM (reprint author), Univ Oregon, Dept Anthropol, Eugene, OR 97403 USA. EM jerland@uoregon.edu; rickt@si.edu OI Erlandson, Jon/0000-0002-4705-4319 NR 114 TC 46 Z9 46 U1 68 U2 206 PU ANNUAL REVIEWS PI PALO ALTO PA 4139 EL CAMINO WAY, PO BOX 10139, PALO ALTO, CA 94303-0139 USA SN 1941-1405 EI 1941-0611 J9 ANNU REV MAR SCI JI Annu. Rev. Mar. Sci. PY 2010 VL 2 BP 231 EP 251 DI 10.1146/annurev.marine.010908.163749 PG 21 WC Geochemistry & Geophysics; Marine & Freshwater Biology; Oceanography SC Geochemistry & Geophysics; Marine & Freshwater Biology; Oceanography GA 548SA UT WOS:000273985300009 PM 21141664 ER PT J AU Feller, IC Lovelock, CE Berger, U McKee, KL Joye, SB Ball, MC AF Feller, I. C. Lovelock, C. E. Berger, U. McKee, K. L. Joye, S. B. Ball, M. C. TI Biocomplexity in Mangrove Ecosystems SO ANNUAL REVIEW OF MARINE SCIENCE SE Annual Review of Marine Science LA English DT Review; Book Chapter DE emergent properties; collective properties; trait plasticity; habitat stability; nutrient cycling; individual-based models ID INDIVIDUAL-BASED MODELS; SALINITY TOLERANCE; RHIZOPHORA-MANGLE; AVICENNIA-MARINA; FOREST STRUCTURE; CLIMATE-CHANGE; AEGICERAS-CORNICULATUM; NUTRIENT AVAILABILITY; CONCEPTUAL-FRAMEWORK; FIELD CONDITIONS AB Mangroves are an ecological assemblage of trees and shrubs adapted to grow in intertidal environments along tropical coasts. Despite repeated demonstration of their economic and societal value, more than 50% of the world's mangroves have been destroyed, 35% in the past two decades to aquaculture and coastal development, altered hydrology, sea-level rise, and nutrient overenrichment. Variations in the structure and function of mangrove ecosystems have generally been described solely on the basis of a hierarchical classification of the physical characteristics of the intertidal environment, including climate, geomorphology, topography, and hydrology. Here, we use the concept of emergent properties at multiple levels within a hierarchical framework to review how the interplay between specialized adaptations and extreme trait plasticity that characterizes mangroves and intertidal environments gives rise to the biocomplexity that distinguishes mangrove ecosystems. The traits that allow mangroves to tolerate variable salinity, flooding, and nutrient availability influence ecosystem processes and ultimately the services they provide. We conclude that an integrated research strategy using emergent properties in empirical and theoretical studies provides a holistic approach for understanding and managing mangrove ecosystems. C1 [Feller, I. C.] Smithsonian Inst, Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Lovelock, C. E.] Univ Queensland, Ctr Marine Studies, St Lucia, Qld 4072, Australia. [Lovelock, C. E.] Univ Queensland, Sch Biol Sci, St Lucia, Qld 4072, Australia. [Berger, U.] Tech Univ Dresden, Inst Forest Growth & Comp Sci, D-01737 Tharandt, Germany. [McKee, K. L.] US Geol Survey, Natl Wetlands Res Ctr, Lafayette, LA 70506 USA. [Joye, S. B.] Univ Georgia, Dept Marine Sci, Athens, GA 30602 USA. [Ball, M. C.] Australian Natl Univ, Res Sch Biol Sci, Canberra, ACT 0200, Australia. RP Feller, IC (reprint author), Smithsonian Inst, Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. EM felleri@si.edu; c.lovelock@uq.edu.au; uta.berger@forst.tu-dresden.de; mckeek@usgs.gov; mjoye@uga.edu; marilyn.ball@anu.edu.au RI Ball, Marilyn/D-1180-2009; Lovelock, Catherine/G-7370-2012; McKee, Karen/D-1365-2014; OI Lovelock, Catherine/0000-0002-2219-6855; McKee, Karen/0000-0001-7042-670X; Joye, Samantha/0000-0003-1610-451X; Feller, Ilka/0000-0002-6391-1608 FU National Science Foundation [DEB-9981535]; Smithsonian Institution's Marine Science Network; Australian Research Council [DP0774491, LP0776680] FX We apologize in advance to all the investigators whose research we could not appropriately cite owing to space limitations. If important references were included in recent reviews, we cited the reviews. We thank Rainer Feller, Anne Chamberlain, and the editorial reviewers of the Annual Review of Marine Science for helpful edits and comments. This research was funded by the National Science Foundation (DEB-9981535), the Smithsonian Institution's Marine Science Network, and Australian Research Council awards DP0774491 and LP0776680. NR 145 TC 83 Z9 85 U1 14 U2 128 PU ANNUAL REVIEWS PI PALO ALTO PA 4139 EL CAMINO WAY, PO BOX 10139, PALO ALTO, CA 94303-0139 USA SN 1941-1405 EI 1941-0611 J9 ANNU REV MAR SCI JI Annu. Rev. Mar. Sci. PY 2010 VL 2 BP 395 EP 417 DI 10.1146/annurev.marine.010908.163809 PG 23 WC Geochemistry & Geophysics; Marine & Freshwater Biology; Oceanography SC Geochemistry & Geophysics; Marine & Freshwater Biology; Oceanography GA 548SA UT WOS:000273985300015 PM 21141670 ER PT J AU Davidson, IC Zabin, CJ Chang, AL Brown, CW Sytsma, MD Ruiz, GM AF Davidson, Ian C. Zabin, Chela J. Chang, Andrew L. Brown, Christopher W. Sytsma, Mark D. Ruiz, Gregory M. TI Recreational boats as potential vectors of marine organisms at an invasion hotspot SO AQUATIC BIOLOGY LA English DT Article DE Biofouling; Bioinvasions; Nonindigenous species; Recreational boats; Vector ID NEW-ZEALAND; INTRODUCTIONS; TRANSPORT; VESSELS AB With more than 200 aquatic nonindigenous species (NIS), San Francisco Bay (California, USA) is among the world's most invaded harbors. Hard-substratum benthic (biofouling) organisms, which dominate NIS richness, have arrived primarily as a result of shipping and aquaculture activity over past centuries. To date there has been no assessment of the leisure craft vector in the Bay. We aimed to characterize (1) biofouling on boats' submerged surfaces and (2) boater behavior likely to affect the risk of NIS transfers. We used an underwater pole-cam, specimen collections, and a boater questionnaire to quantify the extent and composition of biofouling on recreational boats and to evaluate boater behavior at a subset of the Bay's marinas. Several NIS, already established within the Bay, were recorded from vessel hulls, including the bryozoans Bugula neritina, Membranipora chesapeakensis and Watersipora sp., the ascidians Botrylloides violaceus, Styela clava and Ciona intestinalis, the polychaete Ficopomatus enigmaticus, and the sponge Clathria prolifera. Only 16% of questionnaire respondents had traveled to sites outside the Bay in the previous 12 mo. Frequency of hull painting and cleaning varied substantially, but we did not find strong patterns of biofouling extent associated with hull husbandry or boat usage. The potential for within-Bay and coastwise regional spread of NIS is high, and recreational boats probably interact in close proximity to other vectors (e. g. commercial ships), causing a ratchet effect of vector events; however, there remains a gap in understanding the levels and condition of biofouling on transient boats. Transient vessels from San Francisco Bay and other West Coast sites should be the focus of future studies to evaluate the extent to which organisms are being transferred among bays and how vector management could be applied to prevent NIS transfers and impacts. C1 [Davidson, Ian C.; Sytsma, Mark D.] Portland State Univ, Aquat Bioinvas Res & Policy Inst, Portland, OR 97207 USA. [Zabin, Chela J.; Chang, Andrew L.; Brown, Christopher W.] Romberg Tiburon Ctr Environm Studies, Smithsonian Environm Res Ctr, Marine Invas Lab, Tiburon, CA 94920 USA. [Ruiz, Gregory M.] Smithsonian Environm Res Ctr, Marine Invas Lab, Edgewater, MD 21037 USA. [Davidson, Ian C.; Sytsma, Mark D.] Smithsonian Environm Res Ctr, Portland, OR 97207 USA. RP Davidson, IC (reprint author), Portland State Univ, Aquat Bioinvas Res & Policy Inst, POB 751, Portland, OR 97207 USA. EM idavidso@pdx.edu RI Sytsma, Mark/B-2746-2013; Chang, Andrew/J-8058-2016; OI Chang, Andrew/0000-0002-7870-285X; Ruiz, Gregory/0000-0003-2499-441X; Davidson, Ian/0000-0002-8729-6048 FU US Fish & Wildlife Service through the Western Regional Panel on Aquatic Invasive Species FX We are grateful to R. Draheim and C. Simkanin for their contributions to project initiation and development. We thank J. Leonard of the Hawaii Department of Lands and Natural Resources and S. Altman for helpful discussions and assistance in the field. We also thank B. Proctor of the US Fish & Wildlife Service for helpful advice and comments. The Human Subjects Research Review Committee at Portland State University provided a timely review and approval of our questionnaire for this project. This project was funded by the US Fish & Wildlife Service through the Western Regional Panel on Aquatic Invasive Species. NR 45 TC 25 Z9 25 U1 0 U2 41 PU INTER-RESEARCH PI OLDENDORF LUHE PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY SN 1864-7790 EI 1864-7782 J9 AQUAT BIOL JI Aquat. Biol. PY 2010 VL 11 IS 2 BP 179 EP 191 DI 10.3354/ab00302 PG 13 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 697NA UT WOS:000285519100009 ER PT J AU Fridlund, M Eiroa, C Henning, T Herbst, T Lammer, H Leger, A Liseau, R Paresce, F Penny, A Quirrenbach, A Rottgering, H Selsis, F White, GJ Absil, O Defrere, D Hanot, C Stam, D Schneider, J Tinetti, G Karlsson, A Gondoin, P den Hartog, R D'Arcio, L Stankov, AM Kilter, M Erd, C Beichman, C Coulter, D Danchi, W Devirian, M Johnston, KJ Lawson, P Lay, OP Lunine, J Kaltenegger, L AF Fridlund, Malcolm Eiroa, Carlos Henning, Thomas Herbst, Tom Lammer, Helmut Leger, Alain Liseau, Rene Paresce, Francesco Penny, Alan Quirrenbach, Andreas Rottgering, Huub Selsis, Franck White, Glenn J. Absil, Olivier Defrere, Denis Hanot, C. Stam, Daphne Schneider, Jean Tinetti, Giovanna Karlsson, Anders Gondoin, Phillipe den Hartog, Roland D'Arcio, Luigi Stankov, Anna-Maria Kilter, Mikael Erd, Christian Beichman, Charles Coulter, Daniel Danchi, William Devirian, Michael Johnston, Kenneth J. Lawson, Peter Lay, Oliver P. Lunine, Jonathan Kaltenegger, Lisa TI The Search for Worlds Like Our Own SO ASTROBIOLOGY LA English DT Article DE Terrestrial exoplanets; Habitability; Planet-detection methods; Bioastronomy ID EXTRA-SOLAR PLANETS; GIANT PLANETS; NULLING INTERFEROMETER; DARWIN PROJECT; COMPANION; MISSION; SYSTEMS; SPACE; STARS; DISK AB The direct detection of Earth-like exoplanets orbiting nearby stars and the characterization of such planets particularly, their evolution, their atmospheres, and their ability to host life-constitute a significant problem. The quest for other worlds as abodes of life has been one of mankind's great questions for several millennia. For instance, as stated by Epicurus similar to 300 BC: "Other worlds, with plants and other living things, some of them similar and some of them different from ours, must exist.'' Demokritos from Abdera (460-370 BC), the man who invented the concept of indivisible small parts-atoms-also held the belief that other worlds exist around the stars and that some of these worlds may be inhabited by life-forms. The idea of the plurality of worlds and of life on them has since been held by scientists like Johannes Kepler and William Herschel, among many others. Here, one must also mention Giordano Bruno. Born in 1548, Bruno studied in France and came into contact with the teachings of Nicolas Copernicus. He wrote the book De l'Infinito, Universo e Mondi in 1584, in which he claimed that the Universe was infinite, that it contained an infinite amount of worlds like Earth, and that these worlds were inhabited by intelligent beings. At the time, this was extremely controversial, and eventually Bruno was arrested by the church and burned at the stake in Rome in 1600, as a heretic, for promoting this and other equally confrontational issues (though it is unclear exactly which idea was the one that ultimately brought him to his end). In all the aforementioned cases, the opinions and results were arrived at through reasoning-not by experiment. We have only recently acquired the technological capability to observe planets orbiting stars other than our Sun; acquisition of this capability has been a remarkable feat of our time. We show in this introduction to the Habitability Primer that mankind is at the dawning of an age when, by way of the scientific method and 21(st)-century technology, we will be able to answer this fascinating controversial issue that has persisted for at least 2500 years. C1 [Fridlund, Malcolm] European Space Agcy, European Space Res & Technol Ctr, Estec, Res & Sci Support Dept, NL-2200 AG Noordwijk, Netherlands. [Eiroa, Carlos] Univ Autonoma Madrid, Madrid, Spain. [Henning, Thomas; Herbst, Tom] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Lammer, Helmut] Austrian Acad Sci, Space Res Inst, A-8010 Graz, Austria. [Leger, Alain] Univ Paris 11, Orsay, France. [Liseau, Rene] Chalmers, Dept Radio & Space Sci, Onsala, Sweden. [Paresce, Francesco] Ist Nazl Astrofis, Rome, Italy. [Penny, Alan] Royal Observ, Edinburgh, Blackford Hill, Scotland. [Penny, Alan; White, Glenn J.] CCLRC Rutherford Appleton Lab, Space Sci & Technol Dept, Didcot, Oxon, England. [Quirrenbach, Andreas] Landessternwarte Heidelberg, Heidelberg, Germany. [Rottgering, Huub] Leiden Observ, NL-2300 RA Leiden, Netherlands. [Selsis, Franck] Univ Bordeaux 1, Bordeaux, France. [White, Glenn J.] Open Univ, Milton Keynes MK7 6AA, Bucks, England. [Absil, Olivier] Observ Grenoble, Astrophys Lab, St Martin Dheres, France. [Absil, Olivier; Defrere, Denis; Hanot, C.] Inst Astrophys & Geophys, Liege, Belgium. [Stam, Daphne] SRON, Netherlands Inst Space Res, Utrecht, Netherlands. [Schneider, Jean] Observ Paris, Lab Univers & Theories, Meudon, France. [Tinetti, Giovanna] UCL, Dept Phys & Astron, London, England. [Karlsson, Anders; Gondoin, Phillipe; den Hartog, Roland; D'Arcio, Luigi; Stankov, Anna-Maria; Kilter, Mikael; Erd, Christian] ESA, European Space Res & Technol Ctr, Payload & Adv Concepts Div, Noordwijk, Netherlands. [Beichman, Charles] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Beichman, Charles; Coulter, Daniel; Devirian, Michael; Lawson, Peter; Lay, Oliver P.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Danchi, William] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Johnston, Kenneth J.] USN Observ, Washington, DC 20392 USA. [Lunine, Jonathan] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Kaltenegger, Lisa] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Fridlund, M (reprint author), European Space Agcy, European Space Res & Technol Ctr, Estec, Res & Sci Support Dept, NL-2200 AG Noordwijk, Netherlands. EM malcolm.fridlund@esa.int OI Tinetti, Giovanna/0000-0001-6058-6654; Absil, Olivier/0000-0002-4006-6237 NR 62 TC 10 Z9 10 U1 2 U2 11 PU MARY ANN LIEBERT INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 J9 ASTROBIOLOGY JI Astrobiology PD JAN-FEB PY 2010 VL 10 IS 1 BP 5 EP 17 DI 10.1089/ast.2009.0380 PG 13 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 572NG UT WOS:000275838900002 PM 20307179 ER PT J AU Alibert, Y Broeg, C Benz, W Wuchterl, G Grasset, O Sotin, C Eiroa, C Henning, T Herbst, T Kaltenegger, L Leger, A Liseau, R Lammer, H Beichman, C Danchi, W Fridlund, M Lunine, J Paresce, F Penny, A Quirrenbach, A Rottgering, H Selsis, F Schneider, J Stam, D Tinetti, G White, GJ AF Alibert, Y. Broeg, C. Benz, W. Wuchterl, G. Grasset, O. Sotin, C. Eiroa, Carlos Henning, Thomas Herbst, Tom Kaltenegger, Lisa Leger, Alain Liseau, Rene Lammer, Helmut Beichman, Charles Danchi, William Fridlund, Malcolm Lunine, Jonathan Paresce, Francesco Penny, Alan Quirrenbach, Andreas Rottgering, Huub Selsis, Frank Schneider, Jean Stam, Daphne Tinetti, Giovanna White, Glenn J. TI Origin and Formation of Planetary Systems SO ASTROBIOLOGY LA English DT Article DE Planet formation; Gas giants; Ice giants; Terrestrial exoplanets; Habitability ID STELLAR X-RAY; GIANT PLANETS; PROTOPLANETARY DISKS; MASS PLANETS; ORBITAL MIGRATION; OCEAN-PLANETS; SOLAR NEBULA; EVOLUTION; EARTH; ACCRETION AB To estimate the occurrence of terrestrial exoplanets and maximize the chance of finding them, it is crucial to understand the formation of planetary systems in general and that of terrestrial planets in particular. We show that a reliable formation theory should not only explain the formation of the Solar System, with small terrestrial planets within a few AU and gas giants farther out, but also the newly discovered exoplanetary systems with close-in giant planets. Regarding the presently known exoplanets, we stress that our current knowledge is strongly biased by the sensitivity limits of current detection techniques (mainly the radial velocity method). With time and improved detection methods, the diversity of planets and orbits in exoplanetary systems will definitely increase and help to constrain the formation theory further. In this work, we review the latest state of planetary formation in relation to the origin and evolution of habitable terrestrial planets. C1 [Alibert, Y.] Observ Besancon, Inst UTINAM, Besancon, France. [Alibert, Y.; Broeg, C.; Benz, W.] Univ Bern, Inst Phys, Bern, Switzerland. [Wuchterl, G.] Thuringer Landessternwarte Tautenburg, Sternwarte, Tautenburg, Germany. [Grasset, O.; Sotin, C.] CNRS, UMR, Lab Planetol & Geodynam, Nantes, France. [Eiroa, Carlos] Univ Autonoma Madrid, Madrid, Spain. [Henning, Thomas; Herbst, Tom] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Kaltenegger, Lisa] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Leger, Alain] Univ Paris 11, Inst Astrophys Spatiale, Orsay, France. [Liseau, Rene] Chalmers, Dept Radio & Space Sci, Onsala, Sweden. [Lammer, Helmut] Austrian Acad Sci, Space Res Inst, A-8010 Graz, Austria. [Beichman, Charles] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Beichman, Charles] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Danchi, William] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Fridlund, Malcolm] European Space Agcy, European Space Res & Technol Ctr, Res & Sci Support Dept, NL-2200 AG Noordwijk, Netherlands. [Lunine, Jonathan] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Paresce, Francesco] Ist Nazl Astrofis, Rome, Italy. [Penny, Alan; White, Glenn J.] CCLRC Rutherford Appleton Lab, Space Sci & Technol Dept, Didcot, Oxon, England. [Penny, Alan] Royal Observ, Edinburgh, Blackford Hill, Scotland. [Quirrenbach, Andreas] Landessternwarte Heidelberg, Heidelberg, Germany. [Rottgering, Huub] Leiden Observ, NL-2300 RA Leiden, Netherlands. [Selsis, Frank] Univ Bordeaux 1, Bordeaux, France. [Schneider, Jean] Observ Paris, Lab Univers & Ses Theories, Meudon, France. [Stam, Daphne] SRON, Netherlands Inst Space Res, Utrecht, Netherlands. [Tinetti, Giovanna] UCL, Dept Phys & Astron, London, England. [White, Glenn J.] Open Univ, Milton Keynes MK7 6AA, Bucks, England. RP Alibert, Y (reprint author), Observ Besancon, Inst UTINAM, Besancon, France. EM alibert@obs-besancon.fr OI Tinetti, Giovanna/0000-0001-6058-6654 NR 84 TC 9 Z9 11 U1 1 U2 9 PU MARY ANN LIEBERT INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 J9 ASTROBIOLOGY JI Astrobiology PD JAN-FEB PY 2010 VL 10 IS 1 BP 19 EP 32 DI 10.1089/ast.2009.0372 PG 14 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 572NG UT WOS:000275838900003 PM 20307180 ER PT J AU Dvorak, R Pilat-Lohinger, E Bois, E Schwarz, R Funk, B Beichman, C Danchi, W Eiroa, C Fridlund, M Henning, T Herbst, T Kaltenegger, L Lammer, H Leger, A Liseau, R Lunine, J Paresce, F Penny, A Quirrenbach, A Rottgering, H Selsis, F Schneider, J Stam, D Tinetti, G White, GJ AF Dvorak, Rudolf Pilat-Lohinger, Elke Bois, Eric Schwarz, Richard Funk, Barbara Beichman, Charles Danchi, William Eiroa, Carlos Fridlund, Malcolm Henning, Thomas Herbst, Tom Kaltenegger, Lisa Lammer, Helmut Leger, Alain Liseau, Rene Lunine, Jonathan Paresce, Francesco Penny, Alan Quirrenbach, Andreas Rottgering, Huub Selsis, Frank Schneider, Jean Stam, Daphne Tinetti, Giovanna White, Glenn J. TI Dynamical Habitability of Planetary Systems SO ASTROBIOLOGY LA English DT Article DE Orbital dynamics; Habitability; Terrestrial exoplanets ID EXTRA-SOLAR PLANETS; GLOBAL DYNAMICS; TERRESTRIAL PLANETS; PREDICTING PLANETS; APSIDAL RESONANCE; STABILITY LIMITS; DOUBLE STARS; ORBITS; ZONES; MOTION AB The problem of the stability of planetary systems, a question that concerns only multiplanetary systems that host at least two planets, is discussed. The problem of mean motion resonances is addressed prior to discussion of the dynamical structure of the more than 350 known planets. The difference with regard to our own Solar System with eight planets on low eccentricity is evident in that 60% of the known extrasolar planets have orbits with eccentricity e > 0.2. We theoretically highlight the studies concerning possible terrestrial planets in systems with a Jupiter-like planet. We emphasize that an orbit of a particular nature only will keep a planet within the habitable zone around a host star with respect to the semimajor axis and its eccentricity. In addition, some results are given for individual systems (e.g., Gl777A) with regard to the stability of orbits within habitable zones. We also review what is known about the orbits of planets in double-star systems around only one component ( e. g., gamma Cephei) and around both stars (e.g., eclipsing binaries). C1 [Dvorak, Rudolf; Pilat-Lohinger, Elke; Schwarz, Richard; Funk, Barbara] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. [Bois, Eric] Observ Cote Azur, F-06003 Nice, France. [Schwarz, Richard; Funk, Barbara] Univ Budapest, Dept Astron, Budapest, Hungary. [Beichman, Charles] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Beichman, Charles] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Danchi, William] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Eiroa, Carlos] Univ Autonoma Madrid, Madrid, Spain. [Fridlund, Malcolm] European Space Agcy, European Space Res & Technol Ctr, Res & Sci Support Dept, NL-2200 AG Noordwijk, Netherlands. [Henning, Thomas; Herbst, Tom] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Kaltenegger, Lisa] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lammer, Helmut] Austrian Acad Sci, Space Res Inst, A-8010 Graz, Austria. [Leger, Alain] Univ Paris 11, Orsay, France. [Liseau, Rene] Chalmers, Dept Radio & Space Sci, Onsala, Sweden. [Lunine, Jonathan] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Paresce, Francesco] Ist Nazl Astrofis, Rome, Italy. [Penny, Alan; White, Glenn J.] CCLRC Rutherford Appleton Lab, Space Sci & Technol Dept, Didcot, Oxon, England. [Quirrenbach, Andreas] Landessternwarte Heidelberg, Heidelberg, Germany. [Rottgering, Huub] Leiden Observ, NL-2300 RA Leiden, Netherlands. [Selsis, Frank] Univ Bordeaux 1, Bordeaux, France. [Schneider, Jean] Observ Paris, Lab Univers & Ses Theories, Meudon, France. [Stam, Daphne] SRON, Netherlands Inst Space Res, Utrecht, Netherlands. [Tinetti, Giovanna] UCL, Dept Phys & Astron, London, England. [White, Glenn J.] Open Univ, Milton Keynes MK7 6AA, Bucks, England. RP Dvorak, R (reprint author), Univ Vienna, Inst Astron, Turkenschanzstr 17, A-1180 Vienna, Austria. EM dvorak@astro.univie.ac.at OI Tinetti, Giovanna/0000-0001-6058-6654; Funk, Barbara/0000-0001-7233-9730 FU Austrian science foundation FWF [P18930-N16, P19569-N16, J2892-N16]; Osterreichische Forschungsgesellschaft [MOEL 309] FX R.D. (project P18930-N16), E. P.-L. (project P19569-N16), and B. F. (Erwin Schrodinger grant J2892-N16) wish to acknowledge support by the Austrian science foundation FWF. R. S. wishes to acknowledge the support of the Osterreichische Forschungsgesellschaft (project MOEL 309). NR 57 TC 8 Z9 8 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 J9 ASTROBIOLOGY JI Astrobiology PD JAN-FEB PY 2010 VL 10 IS 1 BP 33 EP 43 DI 10.1089/ast.2009.0379 PG 11 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 572NG UT WOS:000275838900004 PM 20307181 ER PT J AU Brack, A Horneck, G Cockell, CS Berces, A Belisheva, NK Eiroa, C Henning, T Herbst, T Kaltenegger, L Leger, A Liseau, R Lammer, H Selsis, F Beichman, C Danchi, W Fridlund, M Lunine, J Paresce, F Penny, A Quirrenbach, A Rottgering, H Schneider, J Stam, D Tinetti, G White, GJ AF Brack, A. Horneck, G. Cockell, C. S. Berces, A. Belisheva, N. K. Eiroa, Carlos Henning, Thomas Herbst, Tom Kaltenegger, Lisa Leger, Alain Liseau, Rene Lammer, Helmut Selsis, Franck Beichman, Charles Danchi, William Fridlund, Malcolm Lunine, Jonathan Paresce, Francesco Penny, Alan Quirrenbach, Andreas Rottgering, Huub Schneider, Jean Stam, Daphne Tinetti, Giovanna White, Glenn J. TI Origin and Evolution of Life on Terrestrial Planets SO ASTROBIOLOGY LA English DT Article DE Organic molecules; Origin of life; Astrobiology; Radiation ID EARTH-LIKE PLANETS; GALACTIC HABITABLE ZONE; AMINO-ACIDS; ULTRAVIOLET-RADIATION; HYDROTHERMAL VENTS; BACTERIA; STARS; PERMAFROST; BIOSPHERE; SEDIMENTS AB The ultimate goal of terrestrial planet-finding missions is not only to discover terrestrial exoplanets inside the habitable zone (HZ) of their host stars but also to address the major question as to whether life may have evolved on a habitable Earth-like exoplanet outside our Solar System. We note that the chemical evolution that finally led to the origin of life on Earth must be studied if we hope to understand the principles of how life might evolve on other terrestrial planets in the Universe. This is not just an anthropocentric point of view: the basic ingredients of terrestrial life, that is, reduced carbon-based molecules and liquid H2O, have very specific properties. We discuss the origin of life from the chemical evolution of its precursors to the earliest life-forms and the biological implications of the stellar radiation and energetic particle environments. Likewise, the study of the biological evolution that has generated the various life-forms on Earth provides clues toward the understanding of the interconnectedness of life with its environment. C1 [Brack, A.] CNRS, Ctr Biophys Mol, F-45071 Orleans 2, France. [Horneck, G.] DLR, Inst Aerosp Med, Cologne, Germany. [Cockell, C. S.] Open Univ, Geochem Res Grp, Milton Keynes MK7 6AA, Bucks, England. [Berces, A.] Hungarian Acad Sci, MTA SE Res Grp Biophys, Budapest, Hungary. [Belisheva, N. K.] Russian Acad Sci, Kola Sci Ctr, Polar Alpine Bot Garden Inst, Apatity, Russia. [Eiroa, Carlos] Univ Autonoma Madrid, Madrid, Spain. [Henning, Thomas; Herbst, Tom] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Kaltenegger, Lisa] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Leger, Alain] Univ Paris 11, Inst Astrophys Spatiale, Orsay, France. [Liseau, Rene] Chalmers, Dept Radio & Space Sci, Onsala, Sweden. [Lammer, Helmut] Austrian Acad Sci, Space Res Inst, A-8010 Graz, Austria. [Selsis, Franck] Univ Bordeaux 1, Bordeaux, France. [Beichman, Charles] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Beichman, Charles] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Danchi, William] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Fridlund, Malcolm] European Space Agcy, European Space Res & Technol Ctr, Res & Sci Support Dept, NL-2200 AG Noordwijk, Netherlands. [Lunine, Jonathan] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Paresce, Francesco] Ist Nazl Astrofis, Rome, Italy. [Penny, Alan; White, Glenn J.] CCLRC Rutherford Appleton Lab, Space Sci & Technol Dept, Didcot, Oxon, England. [Quirrenbach, Andreas] Landessternwarte Heidelberg, Heidelberg, Germany. [Rottgering, Huub] Leiden Observ, NL-2300 RA Leiden, Netherlands. [Schneider, Jean] Observ Paris, Lab Univers & Ses Theories, Meudon, France. [Stam, Daphne] SRON, Netherlands Inst Space Res, Utrecht, Netherlands. [Tinetti, Giovanna] UCL, Dept Phys & Astron, London, England. [White, Glenn J.] Open Univ, Milton Keynes MK7 6AA, Bucks, England. RP Brack, A (reprint author), CNRS, Ctr Biophys Mol, Rue Charles Sadron, F-45071 Orleans 2, France. EM brack@cnrs-orleans.fr RI Berces, Attila/K-1180-2013; OI Berces, Attila/0000-0002-7234-5660; Tinetti, Giovanna/0000-0001-6058-6654 NR 66 TC 18 Z9 18 U1 3 U2 37 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 JAN-FEB PY 2010 VL 10 IS 1 BP 69 EP 76 DI 10.1089/ast.2009.0374 PG 8 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 572NG UT WOS:000275838900005 PM 20307183 ER PT J AU Grenfell, JL Rauer, H Selsis, F Kaltenegger, L Beichman, C Danchi, W Eiroa, C Fridlund, M Henning, T Herbst, T Lammer, H Leger, A Liseau, R Lunine, J Paresce, F Penny, A Quirrenbach, A Rottgering, H Schneider, J Stam, D Tinetti, G White, GJ AF Grenfell, J. Lee Rauer, Heike Selsis, Franck Kaltenegger, Lisa Beichman, Charles Danchi, William Eiroa, Carlos Fridlund, Malcolm Henning, Thomas Herbst, Tom Lammer, Helmut Leger, Alain Liseau, Rene Lunine, Jonathan Paresce, Francesco Penny, Alan Quirrenbach, Andreas Rottgering, Huub Schneider, Jean Stam, Daphne Tinetti, Giovanna White, Glenn J. TI Co-Evolution of Atmospheres, Life, and Climate SO ASTROBIOLOGY LA English DT Article DE Early Earth; Biomarker; Atmospheres; Climate; Exoplanets ID HALOGEN OCCULTATION EXPERIMENT; EARTH-LIKE PLANETS; MIDDLE-ATMOSPHERE; HABITABLE ZONES; LONG-TERM; 2-DIMENSIONAL MODEL; OZONE; EVOLUTION; METHANE; HYDROGEN AB After Earth's origin, our host star, the Sun, was shining 20-25% less brightly than today. Without greenhouse-like conditions to warm the atmosphere, our early planet would have been an ice ball, and life may never have evolved. But life did evolve, which indicates that greenhouse gases must have been present on early Earth to warm the planet. Evidence from the geological record indicates an abundance of the greenhouse gas CO2. CH4 was probably present as well; and, in this regard, methanogenic bacteria, which belong to a diverse group of anaerobic prokaryotes that ferment CO2 plus H-2 to CH4, may have contributed to modification of the early atmosphere. Molecular oxygen was not present, as is indicated by the study of rocks from that era, which contain iron carbonate rather than iron oxide. Multicellular organisms originated as cells within colonies that became increasingly specialized. The development of photosynthesis allowed the Sun's energy to be harvested directly by life-forms. The resultant oxygen accumulated in the atmosphere and formed the ozone layer in the upper atmosphere. Aided by the absorption of harmful UV radiation in the ozone layer, life colonized Earth's surface. Our own planet is a very good example of how life-forms modified the atmosphere over the planets' lifetime. We show that these facts have to be taken into account when we discover and characterize atmospheres of Earth-like exoplanets. If life has originated and evolved on a planet, then it should be expected that a strong co-evolution occurred between life and the atmosphere, the result of which is the planet's climate. C1 [Grenfell, J. Lee; Rauer, Heike] DLR, German Aerosp Ctr, Inst Planetary Res, Berlin, Germany. [Rauer, Heike] Tech Univ Berlin, Berlin, Germany. [Selsis, Franck] Univ Bordeaux 1, Bordeaux, France. [Kaltenegger, Lisa] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Beichman, Charles] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Beichman, Charles] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Danchi, William] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Eiroa, Carlos] Univ Autonoma Madrid, Madrid, Spain. [Fridlund, Malcolm] European Space Agcy, European Space Res & Technol Ctr, Res & Sci Support Dept, NL-2200 AG Noordwijk, Netherlands. [Henning, Thomas; Herbst, Tom] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Lammer, Helmut] Austrian Acad Sci, Space Res Inst, A-8010 Graz, Austria. [Leger, Alain] Univ Paris 11, Orsay, France. [Liseau, Rene] Chalmers, Dept Radio & Space Sci, Onsala, Sweden. [Lunine, Jonathan] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Paresce, Francesco] Ist Nazl Astrofis, Rome, Italy. [Penny, Alan; White, Glenn J.] CCLRC Rutherford Appleton Lab, Space Sci & Technol Dept, Didcot, Oxon, England. [Quirrenbach, Andreas] Landessternwarte Heidelberg, Heidelberg, Germany. [Rottgering, Huub] Leiden Observ, NL-2300 RA Leiden, Netherlands. [Schneider, Jean] Observ Paris, Lab Univers & Ses Theories, Meudon, France. [Stam, Daphne] SRON, Netherlands Inst Space Res, Utrecht, Netherlands. [Tinetti, Giovanna] UCL, Dept Phys & Astron, London, England. [White, Glenn J.] Open Univ, Milton Keynes MK7 6AA, Bucks, England. RP Grenfell, JL (reprint author), Tech Univ Berlin, Zentrum Astron & Astrophys, Hardenbergstr 36, D-10623 Berlin, Germany. EM lee.Grenfell@dlr.de OI Tinetti, Giovanna/0000-0001-6058-6654 FU Helmholtz Association; International Space Science Institute (ISSI, Bern, Switzerland); Evolution of Habitable Planets'; Evolution of Exoplanet Atmospheres and Their Characterization FX The authors acknowledge the Helmholtz-Gemeinschaft, as this research has been supported by the Helmholtz Association through the research alliance "Planetary Evolution and Life,'' the International Space Science Institute (ISSI, Bern, Switzerland) and the ISSI teams "Evolution of Habitable Planets'' and "Evolution of Exoplanet Atmospheres and Their Characterization.'' NR 66 TC 8 Z9 8 U1 5 U2 21 PU MARY ANN LIEBERT INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 J9 ASTROBIOLOGY JI Astrobiology PD JAN-FEB PY 2010 VL 10 IS 1 BP 77 EP 88 DI 10.1089/ast.2009.0375 PG 12 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 572NG UT WOS:000275838900006 PM 20307184 ER PT J AU Kaltenegger, L Selsis, F Fridlund, M Lammer, H Beichman, C Danchi, W Eiroa, C Henning, T Herbst, T Leger, A Liseau, R Lunine, J Paresce, F Penny, A Quirrenbach, A Rottgering, H Schneider, J Stam, D Tinetti, G White, GJ AF Kaltenegger, Lisa Selsis, Frank Fridlund, Malcolm Lammer, Helmut Beichman, Charles Danchi, William Eiroa, Carlos Henning, Thomas Herbst, Tom Leger, Alain Liseau, Rene Lunine, Jonathan Paresce, Francesco Penny, Alan Quirrenbach, Andreas Rottgering, Huub Schneider, Jean Stam, Daphne Tinetti, Giovanna White, Glenn J. TI Deciphering Spectral Fingerprints of Habitable Exoplanets SO ASTROBIOLOGY LA English DT Article DE Habitable planets; Exoplanet search; Biomarkers; Planetary atmospheres ID EARTH-LIKE PLANETS; EXTRASOLAR TERRESTRIAL PLANETS; INFRARED RADIATION; THERMAL EMISSION; HD 189733B; RED-EDGE; LIFE; SEARCH; STARS; ATMOSPHERES AB We discuss how to read a planet's spectrum to assess its habitability and search for the signatures of a biosphere. After a decade rich in giant exoplanet detections, observation techniques have advanced to a level where we now have the capability to find planets of less than 10 Earth masses (M-Earth) (so-called "super Earths''), which may be habitable. How can we characterize those planets and assess whether they are habitable? This new field of exoplanet search has shown an extraordinary capacity to combine research in astrophysics, chemistry, biology, and geophysics into a new and exciting interdisciplinary approach to understanding our place in the Universe. The results of a first-generation mission will most likely generate an amazing scope of diverse planets that will set planet formation, evolution, and our planet into an overall context. C1 [Kaltenegger, Lisa] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. [Selsis, Frank] Univ Bordeaux 1, Bordeaux, France. [Fridlund, Malcolm] European Space Agcy, European Space Res & Technol Ctr, Res & Sci Support Dept, NL-2200 AG Noordwijk, Netherlands. [Lammer, Helmut] Austrian Acad Sci, Space Res Inst, A-8010 Graz, Austria. [Beichman, Charles] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Beichman, Charles] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Danchi, William] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Eiroa, Carlos] Univ Autonoma Madrid, Madrid, Spain. [Henning, Thomas; Herbst, Tom] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Leger, Alain] Univ Paris 11, Orsay, France. [Liseau, Rene] Chalmers, Dept Radio & Space Sci, Onsala, Sweden. [Lunine, Jonathan] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Paresce, Francesco] Ist Nazl Astrofis, Rome, Italy. [Penny, Alan; White, Glenn J.] CCLRC Rutherford Appleton Lab, Space Sci & Technol Dept, Didcot, Oxon, England. [Quirrenbach, Andreas] Landessternwarte Heidelberg, Heidelberg, Germany. [Rottgering, Huub] Leiden Observ, NL-2300 RA Leiden, Netherlands. [Schneider, Jean] Observ Paris, Lab Univers & Ses Theories, Meudon, France. [Stam, Daphne] SRON, Netherlands Inst Space Res, Utrecht, Netherlands. [Tinetti, Giovanna] UCL, Dept Phys & Astron, London, England. [White, Glenn J.] Open Univ, Milton Keynes MK7 6AA, Bucks, England. RP Kaltenegger, L (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-20, Cambridge, MA USA. EM lkaltene@cfa.harvard.edu OI Tinetti, Giovanna/0000-0001-6058-6654 FU Harvard Origins of Life Initiative; NASA Astrobiology Institute FX L. Kaltenegger acknowledges the support of the Harvard Origins of Life Initiative and the NASA Astrobiology Institute. NR 63 TC 36 Z9 37 U1 3 U2 20 PU MARY ANN LIEBERT INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 J9 ASTROBIOLOGY JI Astrobiology PD JAN-FEB PY 2010 VL 10 IS 1 BP 89 EP 102 DI 10.1089/ast.2009.0381 PG 14 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 572NG UT WOS:000275838900007 PM 20307185 ER PT J AU Kaltenegger, L Eiroa, C Ribas, I Paresce, F Leitzinger, M Odert, P Hanslmeier, A Fridlund, M Lammer, H Beichman, C Danchi, W Henning, T Herbst, T Leger, A Liseau, R Lunine, J Penny, A Quirrenbach, A Rottgering, H Selsis, F Schneider, J Stam, D Tinetti, G White, GJ AF Kaltenegger, Lisa Eiroa, Carlos Ribas, Ignasi Paresce, Francesco Leitzinger, Martin Odert, Petra Hanslmeier, Arnold Fridlund, Malcolm Lammer, Helmut Beichman, Charles Danchi, William Henning, Thomas Herbst, Tom Leger, Alain Liseau, Rene Lunine, Jonathan Penny, Alan Quirrenbach, Andreas Rottgering, Huub Selsis, Frank Schneider, Jean Stam, Daphne Tinetti, Giovanna White, Glenn J. TI Stellar Aspects of Habitability-Characterizing Target Stars for Terrestrial Planet-Finding Missions SO ASTROBIOLOGY LA English DT Article DE Darwin/TPF; Nearby stars; Habitability; Exoplanet search ID EXTRA-SOLAR PLANETS; M-CIRCLE-PLUS; EARTH-LIKE EXOPLANETS; EJECTION CME ACTIVITY; LATE-TYPE DWARFS; X-RAY-EMISSION; MASS M-STARS; HARPS SEARCH; SUPER-EARTH; MAIN-SEQUENCE AB We present and discuss the criteria for selecting potential target stars suitable for the search for Earth-like planets, with a special emphasis on the stellar aspects of habitability. Missions that search for terrestrial exoplanets will explore the presence and habitability of Earth-like exoplanets around several hundred nearby stars, mainly F, G, K, and M stars. The evaluation of the list of potential target systems is essential in order to develop mission concepts for a search for terrestrial exoplanets. Using the Darwin All Sky Star Catalogue (DASSC), we discuss the selection criteria, configuration-dependent subcatalogues, and the implication of stellar activity for habitability. C1 [Kaltenegger, Lisa] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Eiroa, Carlos] Univ Autonoma Madrid, Madrid, Spain. [Ribas, Ignasi] CSIC, IEEC, Inst Ciencies Espai, Barcelona, Spain. [Paresce, Francesco] Ist Nazl Astrofis, Rome, Italy. [Leitzinger, Martin; Hanslmeier, Arnold] Graz Univ, Graz, Austria. [Odert, Petra; Fridlund, Malcolm] European Space Agcy, European Space Res & Technol Ctr, Res & Sci Support Dept, NL-2200 AG Noordwijk, Netherlands. [Lammer, Helmut] Austrian Acad Sci, Space Res Inst, A-8010 Graz, Austria. [Beichman, Charles] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Beichman, Charles] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Danchi, William] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Henning, Thomas; Herbst, Tom] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Leger, Alain] Univ Paris 11, Orsay, France. [Liseau, Rene] Chalmers, Dept Radio & Space Sci, Onsala, Sweden. [Lunine, Jonathan] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Penny, Alan; White, Glenn J.] CCLRC Rutherford Appleton Lab, Space Sci & Technol Dept, Didcot, Oxon, England. [Quirrenbach, Andreas] Landessternwarte Heidelberg, Heidelberg, Germany. [Rottgering, Huub] Leiden Observ, NL-2300 RA Leiden, Netherlands. [Selsis, Frank] Univ Bordeaux 1, Bordeaux, France. [Schneider, Jean] Observ Paris, Lab Univers & Ses Theories, Meudon, France. [Stam, Daphne] SRON, Netherlands Inst Space Res, Utrecht, Netherlands. [Tinetti, Giovanna] UCL, Dept Phys & Astron, London, England. [White, Glenn J.] Open Univ, Milton Keynes MK7 6AA, Bucks, England. RP Kaltenegger, L (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-20, Cambridge, MA 02138 USA. EM lkaltene@cfa.harvard.edu RI Ribas, Ignasi/M-2134-2014; OI Ribas, Ignasi/0000-0002-6689-0312; Tinetti, Giovanna/0000-0001-6058-6654 FU Harvard Origins of Life Initiative; NASA; NSF; Austrian FWF (Wissenschaftsfond) [P19446] FX L.K. gratefully acknowledges support from the Harvard Origins of Life Initiative. We thank ISSI. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France; NASA's Astrophysics Data System; and data products from the Two Micron All Sky Survey, which is a joint project of the UMass and IPAC, funded by NASA and NSF. M.L., P.O., and A. H. acknowledge the Austrian FWF (Wissenschaftsfond), grant P19446, for supporting this project. NR 71 TC 11 Z9 11 U1 0 U2 8 PU MARY ANN LIEBERT INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 J9 ASTROBIOLOGY JI Astrobiology PD JAN-FEB PY 2010 VL 10 IS 1 BP 103 EP 112 DI 10.1089/ast.2009.0367 PG 10 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 572NG UT WOS:000275838900008 PM 20307186 ER PT J AU Fridlund, M Eiroa, C Henning, T Herbst, T Kaltenegger, L Leger, A Liseau, R Lammer, H Selsis, F Beichman, C Danchi, W Lunine, J Paresce, F Penny, A Quirrenbach, A Rottgering, H Schneider, J Stam, D Tinetti, G White, GJ AF Fridlund, Malcolm Eiroa, Carlos Henning, Thomas Herbst, Tom Kaltenegger, Lisa Leger, Alain Liseau, Rene Lammer, Helmut Selsis, Franck Beichman, Charles Danchi, William Lunine, Jonathan Paresce, Francesco Penny, Alan Quirrenbach, Andreas Rottgering, Huub Schneider, Jean Stam, Daphne Tinetti, Giovanna White, Glenn J. TI A Roadmap for the Detection and Characterization of Other Earths SO ASTROBIOLOGY LA English DT Article DE Exoplanets; Life in the Universe; Space missions; Biomarkers AB The European Space Agency and other space agencies such as NASA recognize that the question with regard to life beyond Earth in general, and the associated issue of the existence and study of exoplanets in particular, is of paramount importance for the 21(st) century. The new Cosmic Vision science plan, Cosmic Vision 2015-2025, which is built around four major themes, has as its first theme: "What are the conditions for planet formation and the emergence of life?'' This main theme is addressed through further questions: (1) How do gas and dust give rise to stars and planets? (2) How will the search for and study of exoplanets eventually lead to the detection of life outside Earth (biomarkers*)? (3) How did life in the Solar System arise and evolve? Although ESA has busied itself with these issues since the beginning of the Darwin study in 1996, it has become abundantly clear that, as these topics have evolved, only a very large effort, addressed from the ground and from space with the utilization of different instruments and space missions, can provide the empirical results required for a complete understanding. The good news is that the problems can be addressed and solved within a not-too-distant future. In this short essay, we present the present status of a roadmap related to projects that are related to the key long-term goal of understanding and characterizing exoplanets, in particular Earthlike planets. C1 [Fridlund, Malcolm] European Space Agcy, European Space Res & Technol Ctr, Estec, Res & Sci Support Dept, NL-2200 AG Noordwijk, Netherlands. [Eiroa, Carlos] Univ Autonoma Madrid, Madrid, Spain. [Henning, Thomas; Herbst, Tom] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Kaltenegger, Lisa] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Leger, Alain] Univ Paris 11, Inst Astrophys Spatiale, Orsay, France. [Liseau, Rene] Chalmers, Dept Radio & Space Sci, Onsala, Sweden. [Lammer, Helmut] Austrian Acad Sci, Space Res Inst, A-8010 Graz, Austria. [Selsis, Franck] Univ Bordeaux 1, Bordeaux, France. [Beichman, Charles] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Beichman, Charles] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Danchi, William] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Lunine, Jonathan] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Paresce, Francesco] Ist Nazl Astrofis, Rome, Italy. [Penny, Alan; White, Glenn J.] CCLRC Rutherford Appleton Lab, Space Sci & Technol Dept, Didcot, Oxon, England. [Quirrenbach, Andreas] Landessternwarte Heidelberg, Heidelberg, Germany. [Rottgering, Huub] Leiden Observ, NL-2300 RA Leiden, Netherlands. [Schneider, Jean] Observ Paris, Lab Univers & Ses Theories, Meudon, France. [Stam, Daphne] SRON, Netherlands Inst Space Res, Utrecht, Netherlands. [Tinetti, Giovanna] UCL, Dept Phys & Astron, London, England. [White, Glenn J.] Open Univ, Milton Keynes MK7 6AA, Bucks, England. RP Fridlund, M (reprint author), European Space Agcy, European Space Res & Technol Ctr, Estec, Res & Sci Support Dept, NL-2200 AG Noordwijk, Netherlands. EM malcolm.fridlund@esa.int OI Tinetti, Giovanna/0000-0001-6058-6654 NR 1 TC 2 Z9 2 U1 2 U2 10 PU MARY ANN LIEBERT INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 J9 ASTROBIOLOGY JI Astrobiology PD JAN-FEB PY 2010 VL 10 IS 1 BP 113 EP 119 DI 10.1089/ast.2009.0391 PG 7 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 572NG UT WOS:000275838900009 PM 20307187 ER PT J AU Schneider, J Leger, A Fridlund, M White, GJ Eiroa, C Henning, T Herbst, T Lammer, H Liseau, R Paresce, F Penny, A Quirrenbach, A Rottgering, H Selsis, F Beichman, C Danchi, W Kaltenegger, L Lunine, J Stam, D Tinetti, G AF Schneider, Jean Leger, Alain Fridlund, Malcolm White, Glenn J. Eiroa, Carlos Henning, Thomas Herbst, Tom Lammer, Helmut Liseau, Rene Paresce, Francesco Penny, Alan Quirrenbach, Andreas Rottgering, Huub Selsis, Franck Beichman, Charles Danchi, William Kaltenegger, Lisa Lunine, Jonathan Stam, Daphne Tinetti, Giovanna TI The Far Future of Exoplanet Direct Characterization SO ASTROBIOLOGY LA English DT Article DE Far future missions; Direct imaging; High-resolution spectroscopy; Habitable exoplanets; Exo-moons; Surface features ID EXTRA-SOLAR PLANETS; SIGNATURES; SEARCH; IMAGER AB We describe future steps in the direct characterization of habitable exoplanets subsequent to medium and large mission projects currently underway and investigate the benefits of spectroscopic and direct imaging approaches. We show that, after third- and fourth-generation missions have been conducted over the course of the next 100 years, a significant amount of time will lapse before we will have the capability to observe directly the morphology of extrasolar organisms. C1 [Schneider, Jean] Observ Paris, Lab Univers & Ses Theories, Meudon, France. [Leger, Alain] Univ Paris 11, Inst Astrophys Spatiale, Orsay, France. [Fridlund, Malcolm] European Space Agcy, European Space Res & Technol Ctr, Res & Sci Support Dept, NL-2200 AG Noordwijk, Netherlands. [White, Glenn J.] Open Univ, Milton Keynes MK7 6AA, Bucks, England. [White, Glenn J.; Penny, Alan] CCLRC Rutherford Appleton Lab, Space Sci & Technol Dept, Didcot, Oxon, England. [Eiroa, Carlos] Univ Autonoma Madrid, Madrid, Spain. [Henning, Thomas; Herbst, Tom] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Lammer, Helmut] Austrian Acad Sci, Space Res Inst, A-8010 Graz, Austria. [Liseau, Rene] Chalmers, Dept Radio & Space Sci, Onsala, Sweden. [Paresce, Francesco] Ist Nazl Astrofis, Rome, Italy. [Penny, Alan] Royal Observ, Edinburgh, Blackford Hill, Scotland. [Quirrenbach, Andreas] Landessternwarte Heidelberg, Heidelberg, Germany. [Rottgering, Huub] Leiden Observ, NL-2300 RA Leiden, Netherlands. [Selsis, Franck] Univ Bordeaux 1, Bordeaux, France. [Beichman, Charles] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Beichman, Charles] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Danchi, William] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kaltenegger, Lisa] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lunine, Jonathan] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Stam, Daphne] SRON, Netherlands Inst Space Res, Utrecht, Netherlands. [Tinetti, Giovanna] UCL, Dept Phys & Astron, London, England. RP Schneider, J (reprint author), Observ Paris, Lab Univers & Ses Theories, Meudon, France. EM Jean.Schneider@obspm.fr OI Tinetti, Giovanna/0000-0001-6058-6654 NR 25 TC 9 Z9 9 U1 1 U2 10 PU MARY ANN LIEBERT INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 J9 ASTROBIOLOGY JI Astrobiology PD JAN-FEB PY 2010 VL 10 IS 1 BP 121 EP 126 DI 10.1089/ast.2009.0371 PG 6 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 572NG UT WOS:000275838900010 PM 20307188 ER PT B AU Rots, AH AF Rots, Arnold H. BE Mizumoto, Y Morita, KI Ohishi, M TI When Time Is of the Essence SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS XIX SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 19th Annual Conference on Astronomical Data Analysis Software and Systems CY OCT 04-08, 2009 CL Sapporo, JAPAN AB When dealing with (or preserving) time series data, one does well to consider the circumstances under which the data were taken and the uses they may be put to. The higher the timing accuracy that is required, the more stringent will be the requirements for complete and accurate metadata. This paper presents a brief tutorial on time scales, time standards, and time metadata requirements. This includes issues like the difference between dynamic and coordinate time scales, relativistic effects, the connection with spatial coordinate information and barycenter corrections. We also refer to the Virtual Observatory time standards and the proposed FITS Time standard: WCS Paper V. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Rots, AH (reprint author), Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. NR 4 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-748-3 J9 ASTR SOC P PY 2010 VL 434 BP 107 EP 111 PG 5 WC Astronomy & Astrophysics; Computer Science, Interdisciplinary Applications SC Astronomy & Astrophysics; Computer Science GA BUU27 UT WOS:000290361300016 ER PT B AU Kurtz, MJ Accomazzi, A Henneken, E Di Milia, G Grant, CS AF Kurtz, Michael J. Accomazzi, Alberto Henneken, Edwin Di Milia, Giovanni Grant, Carolyn S. BE Mizumoto, Y Morita, KI Ohishi, M TI Using Multipartite Graphs for Recommendation and Discovery SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS XIX SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 19th Annual Conference on Astronomical Data Analysis Software and Systems CY OCT 04-08, 2009 CL Sapporo, JAPAN ID ASTROPHYSICS DATA SYSTEM AB The Smithsonian/NASA Astrophysics Data System exists at the nexus of a dense system of interacting and interlinked information networks. The syntactic and the semantic content of this multipartite graph structure can be combined to provide very specific research recommendations to the scientist/user. C1 [Kurtz, Michael J.; Accomazzi, Alberto; Henneken, Edwin; Di Milia, Giovanni; Grant, Carolyn S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kurtz, MJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 9 TC 2 Z9 2 U1 0 U2 1 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-748-3 J9 ASTR SOC P PY 2010 VL 434 BP 155 EP 158 PG 4 WC Astronomy & Astrophysics; Computer Science, Interdisciplinary Applications SC Astronomy & Astrophysics; Computer Science GA BUU27 UT WOS:000290361300028 ER PT B AU Mitschang, AW Huenemoerder, DP Nichols, JS AF Mitschang, Arik W. Huenemoerder, David P. Nichols, Joy S. BE Mizumoto, Y Morita, KI Ohishi, M TI TGCat, The Chandra Transmission Grating Catalog and Archive: Systems, Design and Accessibility SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS XIX SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 19th Annual Conference on Astronomical Data Analysis Software and Systems CY OCT 04-08, 2009 CL Sapporo, JAPAN AB The recently released Chandra Transmission Grating Catalog and Archive, TGCat, presents a fully dynamic on-line catalog allowing users to browse and categorize Chandra gratings observations quickly and easily, generate custom plots of resulting response corrected spectra on-line without the need for special software and to download analysis ready products from multiple observations in one convenient operation. TGCat has been registered as a VO resource with the NVO providing direct access to the catalogs interface. Catalog processing is automated in order to consistently have the latest available products, and is massively scalable allowing rapid reprocessing of catalog data. A unique feature of the catalog is that all of the high level functions used to retrieve inputs from the Chandra archive and to generate the final data products are available to the user in an ISIS written library with detailed documentation. Here we present a structural overview of the Systems, Design, and Accessibility features of the catalog and archive. C1 [Mitschang, Arik W.; Nichols, Joy S.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Huenemoerder, David P.] MIT, Kavli Inst Space Res, Cambridge, MA 02138 USA. RP Mitschang, AW (reprint author), Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. NR 4 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-748-3 J9 ASTR SOC P PY 2010 VL 434 BP 329 EP + PG 2 WC Astronomy & Astrophysics; Computer Science, Interdisciplinary Applications SC Astronomy & Astrophysics; Computer Science GA BUU27 UT WOS:000290361300072 ER PT J AU Brown, WR Geller, MJ Kenyon, SJ Diaferio, A AF Brown, Warren R. Geller, Margaret J. Kenyon, Scott J. Diaferio, Antonaldo TI VELOCITY DISPERSION PROFILE OF THE MILKY WAY HALO SO ASTRONOMICAL JOURNAL LA English DT Article DE Galaxy: halo; Galaxy: kinematics and dynamics ID HORIZONTAL-BRANCH STARS; SURVEY GALACTIC HALO; A-TYPE STARS; MAIN-SEQUENCE STARS; METAL-POOR GALAXIES; DIGITAL SKY SURVEY; MASS WHITE-DWARF; HYPERVELOCITY STARS; THEORETICAL ISOCHRONES; PHOTOMETRIC SYSTEMS AB We present a spectroscopic sample of 910 distant halo stars from the Hypervelocity Star survey from which we derive the velocity dispersion profile of the Milky Way halo. The sample is a mix of 74% evolved horizontal branch stars and 26% blue stragglers. We estimate distances to the stars using observed colors, metallicities, and stellar evolution tracks. Our sample contains twice as many objects with R > 50 kpc as previous surveys. We compute the velocity dispersion profile in two ways: with a parametric method based on a Milky Way potential model and with a non-parametric method based on the caustic technique originally developed to measure galaxy cluster mass profiles. The resulting velocity dispersion profiles are remarkably consistent with those found by two independent surveys based on other stellar populations: the Milky Way halo exhibits a mean decline in radial velocity dispersion of -0.38 +/- 0.12 km s(-1) kpc(-1) over 15 < R < 75 kpc. This measurement is a useful basis for calculating the total mass and mass distribution of the Milky Way halo. C1 [Brown, Warren R.; Geller, Margaret J.; Kenyon, Scott J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Diaferio, Antonaldo] Univ Torino, Dipartimento Fis Gen Amedeo Avogadro, I-10125 Turin, Italy. [Diaferio, Antonaldo] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy. RP Brown, WR (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM wbrown@cfa.harvard.edu; mgeller@cfa.harvard.edu; skenyon@cfa.harvard.edu; diaferio@ph.unito.it OI Kenyon, Scott/0000-0003-0214-609X NR 60 TC 49 Z9 50 U1 2 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD JAN PY 2010 VL 139 IS 1 BP 59 EP 67 DI 10.1088/0004-6256/139/1/59 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 530RO UT WOS:000272610200006 ER PT J AU van Loon, JT Oliveira, JM Gordon, KD Meixner, M Shiao, B Boyer, ML Kemper, F Woods, PM Tielens, AGGM Marengo, M Indebetouw, R Sloan, GC Chen, CHR AF van Loon, Jacco Th. Oliveira, Joana M. Gordon, Karl D. Meixner, Margaret Shiao, Bernie Boyer, Martha L. Kemper, F. Woods, Paul M. Tielens, A. G. G. M. Marengo, Massimo Indebetouw, Remy Sloan, G. C. Chen, C. -H. Rosie TI A SPITZER SPACE TELESCOPE FAR-INFRARED SPECTRAL ATLAS OF COMPACT SOURCES IN THE MAGELLANIC CLOUDS. I. THE LARGE MAGELLANIC CLOUD SO ASTRONOMICAL JOURNAL LA English DT Review DE circumstellar matter; Magellanic Clouds; stars: AGB and post-AGB; stars: formation; supergiants; supernova remnants ID GIANT BRANCH STARS; LUMINOUS BLUE VARIABLES; SUPERNOVA REMNANT N49; H-II REGIONS; ISO-LWS OBSERVATIONS; SEST KEY PROGRAM; MASS-LOSS RATES; MULTIBAND IMAGING PHOTOMETER; CORONAE-BOREALIS STARS; YOUNG STELLAR OBJECTS AB We present far-infrared spectra, lambda = 52-93 mu m, obtained with the Spitzer Space Telescope in the spectral energy distribution mode of its MIPS instrument, of a representative sample of the most luminous compact far-infrared sources in the Large Magellanic Cloud (LMC). These include carbon stars, OH/IR asymptotic giant branch (AGB) stars, post-AGB objects and planetary nebulae, the R CrB-type star HV 2671, the OH/IR red supergiants (RSGs) WOH G064 and IRAS 05280-6910, the three B[e] stars IRAS 04530-6916, R 66 and R 126, the Wolf-Rayet star Brey 3a, the luminous blue variable (LBV) R 71, the supernova remnant N 49, a large number of young stellar objects (YSOs), compact Hii regions and molecular cores, and a background galaxy at a redshift z similar or equal to 0.175. We use the spectra to constrain the presence and temperature of cold dust and the excitation conditions and shocks within the neutral and ionized gas, in the circumstellar environments and interfaces with the surrounding interstellar medium (ISM). First, we introduce a spectral classification scheme. Then, we measure line strengths, dust temperatures, and IR luminosities. Objects associated with star formation are readily distinguished from evolved stars by their cold dust and/or fine-structure lines. Evolved stars, including the LBV R 71, lack cold dust except in some cases where we argue that this is swept-up ISM. This leads to an estimate of the duration of the prolific dust-producing phase ("superwind") of several thousand years for both RSGs and massive AGB stars, with a similar fractional mass loss experienced despite the different masses. We tentatively detect line emission from neutral oxygen in the extreme RSG WOH G064, which suggests a large dust-free cavity with implications for wind driving. In N 49, the shock between the supernova ejecta and ISM is revealed in spectacular fashion by its strong [O I] lambda 63 mu m emission and possibly water vapor; we estimate that 0.2 M(circle dot) of ISM dust was swept up. On the other hand, some of the compact Hii regions display pronounced [O III] lambda 88 mu m emission. The efficiency of photoelectric heating in the interfaces of ionized gas and molecular clouds is estimated at 0.1%-0.3%. We confirm earlier indications of a low nitrogen content in the LMC. Evidence for solid state emission features is found in both young and evolved objects, but the carriers of these features remain elusive; some of the YSOs are found to contain crystalline water ice. The spectra constitute a valuable resource for the planning and interpretation of observations with the Herschel Space Observatory and the Stratospheric Observatory For Infrared Astronomy. C1 [van Loon, Jacco Th.; Oliveira, Joana M.] Univ Keele, Astrophys Grp, Lennard Jones Labs, Keele ST5 5BG, Staffs, England. [Gordon, Karl D.; Meixner, Margaret; Shiao, Bernie; Boyer, Martha L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Kemper, F.; Woods, Paul M.] Univ Manchester, Jodrell Bank, Sch Phys & Astron, Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Tielens, A. G. G. M.] Leiden Observ, NL-2300 RA Leiden, Netherlands. [Marengo, Massimo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Marengo, Massimo] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Indebetouw, Remy; Chen, C. -H. Rosie] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Indebetouw, Remy] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Sloan, G. C.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. RP van Loon, JT (reprint author), Univ Keele, Astrophys Grp, Lennard Jones Labs, Keele ST5 5BG, Staffs, England. EM jacco@astro.keele.ac.uk RI Woods, Paul/E-6926-2011; Kemper, Francisca/D-8688-2011 OI Woods, Paul/0000-0003-4340-3590; Kemper, Francisca/0000-0003-2743-8240 NR 357 TC 40 Z9 40 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD JAN PY 2010 VL 139 IS 1 BP 68 EP 95 DI 10.1088/0004-6256/139/1/68 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 530RO UT WOS:000272610200007 ER PT J AU Pietrukowicz, P Minniti, D Diaz, RF Fernandez, JM Zoccali, M Gieren, W Pietrzynski, G Ruiz, MT Udalski, A Szeifert, T Hempel, M AF Pietrukowicz, P. Minniti, D. Diaz, R. F. Fernandez, J. M. Zoccali, M. Gieren, W. Pietrzynski, G. Ruiz, M. T. Udalski, A. Szeifert, T. Hempel, M. TI Millimagnitude photometry for transiting extrasolar planetary candidates V. Follow-up of 30 OGLE transits. New candidates SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: individual: OGLE-TR-109, OGLE-TR-111, OGLE-TR-113; planetary systems; binaries: eclipsing ID GRAVITATIONAL LENSING EXPERIMENT; LUMINOSITY OBJECT TRANSITS; ACCURATE RADIUS; GALACTIC DISK; GIANT PLANET; STAR; EXOPLANET; PERIOD; MASS; ATMOSPHERES AB Aims. We used VLT/VIMOS images in the V band to obtain light curves of the extrasolar planetary transits OGLE-TR-111 and OGLE-TR-113 and the candidate planetary transits: OGLE-TR-82, OGLE-TR-86, OGLE-TR-91, OGLE-TR-106, OGLE-TR-109, OGLE-TR-110, OGLE-TR-159, OGLE-TR-167, OGLE-TR-170, OGLE-TR-171. Methods. Using difference imaging photometry, we were able to achieve millimagnitude errors in the individual data points. We present the analysis of the data and the light curves by measuring transit amplitudes and ephemerides and by calculating geometrical parameters for some of the systems. Results. We observed nine OGLE objects at the predicted transit moments. Two other transits were shifted in time by a few hours. For another seven objects we expected to observe transits during the VIMOS run, but they were not detected. Conclusions. The stars OGLE-TR-111 and OGLE-TR-113 are probably the only OGLE objects in the observed sample to host planets, with the other objects being very likely eclipsing binaries or multiple systems. In this paper we also report on four new transiting candidates which we have found in the data. C1 [Pietrukowicz, P.; Minniti, D.; Fernandez, J. M.; Zoccali, M.; Hempel, M.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile. [Pietrukowicz, P.] Nicolaus Copernicus Astron Ctr, PL-00716 Warsaw, Poland. [Minniti, D.] Vatican Observ, I-00120 Vatican City, Vatican. [Diaz, R. F.] UBA, CONICET, Inst Astron & Fis Espacio, Buenos Aires, DF, Argentina. [Fernandez, J. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gieren, W.; Pietrzynski, G.] Univ Concepcion, Dept Astron, Concepcion, Chile. [Pietrzynski, G.; Udalski, A.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. [Ruiz, M. T.] Univ Chile, Dept Astron, Santiago, Chile. [Szeifert, T.] European So Observ, Santiago 19, Chile. RP Pietrukowicz, P (reprint author), Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Av Vicuna MacKenna 4860,Casilla 306, Santiago 22, Chile. EM pietruk@astro.puc.cl RI Diaz, Rodrigo/H-1487-2011; Ruiz, Maria Teresa/I-5770-2016; OI Ruiz, Maria Teresa/0000-0002-6799-1537; Diaz, Rodrigo/0000-0001-9289-5160 FU FONDAP Center for Astrophysics [15010003]; BASAL Center for Astrophysics and Associated Technologies; Foundation for Polish Science; Polish Ministry of Science and Higher Education [N N203 301335]; FONDECYT [1085278]; Polish MNiSW [N20303032/4275] FX P. P., D. M., J.M.F., G. P., M.Z., M. T. R., W. G., M. H. are supported by FONDAP Center for Astrophysics No. 15010003 and the BASAL Center for Astrophysics and Associated Technologies. P. P. was also supported by the Foundation for Polish Science through program MISTRZ and the Polish Ministry of Science and Higher Education through the grant N N203 301335. M.Z. acknowledges support by Proyecto FONDECYT Regular No. 1085278. The OGLE project is partially supported by the Polish MNiSW grant N20303032/4275. D. M. also thanks the John Simon Guggenheim Foundation. A. U. acknowledges support from the grant "Subsydium Profesorskie" from the Foundation for Polish Science. We thank the ESO staff at Paranal Observatory. NR 41 TC 8 Z9 8 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 JAN PY 2010 VL 509 DI 10.1051/0004-6361/200912141 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 550VM UT WOS:000274159400016 ER PT J AU Fong, W Berger, E Fox, DB AF Fong, W. Berger, E. Fox, D. B. TI HUBBLE SPACE TELESCOPE OBSERVATIONS OF SHORT GAMMA-RAY BURST HOST GALAXIES: MORPHOLOGIES, OFFSETS, AND LOCAL ENVIRONMENTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays: bursts ID CORE-COLLAPSE SUPERNOVAE; EXTENDED EMISSION; ELLIPTIC-GALAXY; FORMATION RATES; AFTERGLOW; PROGENITORS; REDSHIFT; SPECTROSCOPY; CONSTRAINTS; POPULATIONS AB We present the first comprehensive analysis of Hubble Space Telescope (HST) observations of short-duration gamma-ray burst (GRB) host galaxies. These observations allow us to characterize the galactic and local environments of short GRBs as a powerful constraint on the nature of their progenitors. Using the HST data for 10 short GRB hosts, we determine the host morphological properties, measure precise physical and host-normalized offsets relative to the galaxy centers, and study the locations of short GRBs relative to their host light distributions. We find that most short GRB hosts have exponential disk profiles, characteristic of late-type galaxies, but with a median size that is twice as large as that of long GRB hosts, commensurate with their higher luminosities. The observed distribution of projected physical offsets, supplemented by ground-based measurements, has a median of approximate to 5 kpc, about five times larger than that for long GRBs, and in good agreement with predicted offset distributions for neutron star-neutron star (NS-NS) binary mergers. For the short GRB population as a whole, we find the following robust constraints: (1) greater than or similar to 25% have projected offsets of less than or similar to 10 kpc; and (2) greater than or similar to 5% have projected offsets of greater than or similar to 20 kpc. We find no clear systematic trends for the offset distribution of short GRBs with and without extended soft emission. While the physical offsets are larger than those for long GRBs, the distribution of host-normalized offsets is nearly identical due to the larger size of short GRB hosts. Finally, unlike long GRBs, which are concentrated in the brightest regions of their host galaxies, short GRBs appear to under-represent the light distribution of their hosts; this is true even in comparison to core-collapse and Type Ia supernovae. Based on these results, we conclude that short GRBs are consistent with a progenitor population of NS-NS binaries, but partial contribution from prompt or delayed magnetar formation is also consistent with the data. Our study underscores the importance of future HST observations of the larger existing and growing sample of short GRB hosts, which will allow us to delineate the properties of the progenitor population. C1 [Fong, W.; Berger, E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fox, D. B.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. RP Fong, W (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 55 TC 115 Z9 117 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 JAN 1 PY 2010 VL 708 IS 1 BP 9 EP 25 DI 10.1088/0004-637X/708/1/9 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 532ZM UT WOS:000272790400002 ER PT J AU Nagel, E D'Alessio, P Calvet, N Espaillat, C Sargent, B Hernandez, J Forrest, WJ AF Nagel, Erick D'Alessio, Paola Calvet, Nuria Espaillat, Catherine Sargent, Ben Hernandez, Jesus Forrest, William J. TI WALL EMISSION IN CIRCUMBINARY DISKS: THE CASE OF CoKu TAU/4 SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; infrared: stars; stars: pre-main sequence ID T-TAURI STARS; ECCENTRIC STELLAR BINARIES; ACCRETION DISKS; YOUNG OBJECTS; PROTOPLANETARY DISKS; INTERSTELLAR GRAINS; INNER RIM; DUST; EVOLUTION; DISCS AB A few years ago, the mid-IR spectrum of a Weak Line T Tauri Star, CoKu Tau/4, was explained as emission from the inner wall of a circumstellar disk, with the inner disk truncated at similar to 10 AU. Based on the spectral energy distribution (SED) shape and the assumption that it was produced by a single star and its disk, CoKu Tau/4 was classified as a prototypical transitional disk, with a clean inner hole possibly carved out by a planet, some other orbiting body, or by photodissociation. However, recently it has been discovered that CoKu Tau/4 is a close binary system. This implies that the observed mid-IR SED is probably produced by the circumbinary disk. The aim of the present paper is to model the SED of CoKu Tau/4 as arising from the inner wall of a circumbinary disk, with parameters constrained by what is known about the central stars and by a dynamical model for the interaction between these stars and their surrounding disk. We lack a physical prescription for the shape of the wall, thus, here we use a simplified and unrealistic assumption: the wall is vertical. In order to fit the Spitzer IRS SED, the binary orbit should be almost circular, implying a small mid-IR variability (10%) related to the variable distances of the stars to the inner wall of the circumbinary disk. In the context of the present model, higher eccentricities would imply that the stars are farther from the wall, the latter being too cold to explain the observed SED. Our models suggest that the inner wall of CoKu Tau/4 is located at 1.7a, where a is the semi-major axis of the binary system (a similar to 8 AU). A small amount of optically thin dust in the hole (less than or similar to 0.01 lunar masses) helps to improve the fit to the 10 mu m silicate band. Also, we find that water ice should be absent or have a very small abundance (a dust to gas mass ratio less than or similar to 5.6 x 10(-5)). In general, for a binary system with eccentricity e > 0, the model predicts mid-IR variability with periods similar to orbital timescales, assuming that thermal equilibrium is reached instantaneously. C1 [Nagel, Erick; D'Alessio, Paola] UNAM, Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico. [Nagel, Erick] Univ Guanajuato, Dept Astron, Guanajuato 36240, Mexico. [Calvet, Nuria] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Espaillat, Catherine] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Sargent, Ben] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Hernandez, Jesus] Ctr Invest Astron, Merida 5101A, Venezuela. [Forrest, William J.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. RP Nagel, E (reprint author), UNAM, Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico. EM erick@astro.ugto.mx FU NASA [NNX08AH94G]; CONACyT, Mexico; UNAM; National Science Foundation [0901947] 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. We are indebted with Adam Kraus for the opportunity to exchange ideas with him. P.D. acknowledges a grant from CONACyT, Mexico. E.N.appreciates postdoctoral fellowships from UNAM and CONACyT, Mexico. C.E. was supported by the National Science Foundation under Award No. 0901947. N.C. acknowledges support from NASA grant NNX08AH94G. NR 51 TC 21 Z9 21 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 JAN 1 PY 2010 VL 708 IS 1 BP 38 EP 50 DI 10.1088/0004-637X/708/1/38 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 532ZM UT WOS:000272790400004 ER PT J AU Yoon, J Peterson, DM Kurucz, RL Zagarello, RJ AF Yoon, Jinmi Peterson, Deane M. Kurucz, Robert L. Zagarello, Robert J. TI A NEW VIEW OF VEGA'S COMPOSITION, MASS, AND AGE SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: chemically peculiar; stars: evolution; stars: fundamental parameters (metallicity, mass, age); stars: individual (Vega); stars: rotation ID LAMBDA-BOOTIS STARS; RAPIDLY ROTATING STAR; A-TYPE STARS; CHEMICAL-COMPOSITION; CHARA ARRAY; POLE-ON; ABUNDANCES; PHOTOMETRY AB We present estimates of Vega's composition, mass, and age based on a simultaneous fit of high-resolution metal line profiles, the wings of the Balmer lines, the absolute visible/near-IR fluxes, and high angular resolution triple phase data from the Navy Prototype Optical Interferometer to gravity-darkened Roche models. This substantially expands our earlier analysis. We determine that Vega has a much lower mass, 2.135 +/- 0.074M(circle dot), than generally assumed. This strongly supports the contention that Vega is metal-poor throughout (Z similar to 0.008), suggesting it was formed that way. Assuming a uniform composition equal to that derived for the surface, and the luminosity and radius obtained here, we derive a best estimate of Vega's age, 455 +/- 13 Myr, and mass, 2.157 +/- 0.017M(circle dot), by fitting to standard isochrones. We continue to argue that Vega is much too old to be coeval with other members of the Castor moving group and is thus unlikely to be a member. The updated chemical abundances continue to support the conclusion that Vega is a lambda Boo star. C1 [Yoon, Jinmi; Peterson, Deane M.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA. [Kurucz, Robert L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Zagarello, Robert J.] PCPION, S Setauket, NY 11720 USA. RP Yoon, J (reprint author), SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA. EM jyoon@grad.physics.sunysb.edu; dpeterson@astro.sunysb.edu; rkurucz@cfa.harvard.edu; rzagarello@mail.astro.sunysb.edu OI Yoon, Jinmi/0000-0002-4168-239X FU Naval Research Laboratory; NSF AST [06-07612] FX This research was supported in part by a grant from the Naval Research Laboratory to D.M.P. and in part by NSF AST grant 06-07612 to Dr. Michal Simon. NR 38 TC 26 Z9 27 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 JAN 1 PY 2010 VL 708 IS 1 BP 71 EP 79 DI 10.1088/0004-637X/708/1/71 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 532ZM UT WOS:000272790400007 ER PT J AU Matthews, LD Greenhill, LJ Goddi, C Chandler, CJ Humphreys, EML Kunz, MW AF Matthews, L. D. Greenhill, L. J. Goddi, C. Chandler, C. J. Humphreys, E. M. L. Kunz, M. W. TI A FEATURE MOVIE OF SiO EMISSION 20-100 AU FROM THE MASSIVE YOUNG STELLAR OBJECT ORION SOURCE I SO ASTROPHYSICAL JOURNAL LA English DT Article DE masers; radio lines: stars; stars: formation ID BECKLIN-NEUGEBAUER/KLEINMANN-LOW; STAR-FORMING REGIONS; MASER EMISSION; MAGNETIC-FIELD; NUMERICAL-CALCULATIONS; VLBA OBSERVATIONS; ACCRETION DISKS; BN/KL REGION; 86 GHZ; KL AB We present multi-epoch Very Long Baseline Array imaging of the (28)SiO nu = 1 and nu = 2, J = 1-0 maser emission toward the massive young stellar object (YSO) Orion Source I. Both SiO transitions were observed simultaneously with an angular resolution of similar to 0.5 mas (similar to 0.2 AU for d = 414 pc) and a spectral resolution of similar to 0.2 km s(-1). Here we explore the global properties and kinematics of the emission through two 19-epoch animated movies spanning 21 months (from 2001 March 19 to 2002 December 10). These movies provide the most detailed view to date of the dynamics and temporal evolution of molecular material within similar to 20-100 AU of a massive (greater than or similar to 8 M(circle dot)) YSO. As in previous studies, we find that the bulk of the SiO masers surrounding Source I lie in an X-shaped locus; the emission in the south and east arms is predominantly blueshifted, and emission in the north and west is predominantly redshifted. In addition, bridges of intermediate-velocity emission are observed connecting the red and blue sides of the emission distribution. We have measured proper motions of over 1000 individual maser features and found that these motions are characterized by a combination of radially outward migrations along the four main maser-emitting arms and motions tangent to the intermediate-velocity bridges. We interpret the SiO masers as arising from a wide-angle bipolar wind emanating from a rotating, edge-on disk. The detection of maser features along extended, curved filaments suggests that magnetic fields may play a role in launching and/or shaping the wind. Our observations appear to support a picture in which stars with masses as high as at least 8M(circle dot) form via disk-mediated accretion. However, we cannot yet rule out that the Source I disk may have been formed or altered following a recent close encounter. C1 [Matthews, L. D.; Greenhill, L. J.; Goddi, C.; Humphreys, E. M. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Matthews, L. D.] MIT, Haystack Observ, Westford, MA 01886 USA. [Chandler, C. J.; Kunz, M. W.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Kunz, M. W.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA. RP Matthews, LD (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU NSF [0507478]; NRAO [BG118, BG129] FX We thank Mark Reid for valuable technical discussions and for supplying his fit_rates code. We also acknowledge helpful discussions with Mark Krumholz and comments from our anonymous referee that have helped to improve our presentation. This project has been supported by NSF grant 0507478 and a Visiting Scientist appointment to L.D.M. from the Smithsonian Astrophysical Observatory. The data presented here were part of NRAO programs BG118 and BG129. NR 57 TC 53 Z9 53 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 JAN 1 PY 2010 VL 708 IS 1 BP 80 EP 92 DI 10.1088/0004-637X/708/1/80 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 532ZM UT WOS:000272790400008 ER PT J AU Belczynski, K Holz, DE Fryer, CL Berger, E Hartmann, DH O'Shea, B AF Belczynski, Krzysztof Holz, Daniel E. Fryer, Chris L. Berger, Edo Hartmann, Dieter H. O'Shea, Brian TI ON THE ORIGIN OF THE HIGHEST REDSHIFT GAMMA-RAY BURSTS SO ASTROPHYSICAL JOURNAL LA English DT Review DE binaries: general; gamma rays: bursts; stars: formation ID MASS-METALLICITY RELATION; COMPACT OBJECT MERGERS; POPULATION-III STARS; NEUTRON-STARS; BLACK-HOLES; LUMINOSITY EVOLUTION; MILLISECOND PULSARS; EARLY UNIVERSE; GRB 080913; AFTERGLOW AB GRB 080913 and GRB 090423 are the most distant gamma-ray bursts (GRBs) known to date, with spectroscopically determined redshifts of z = 6.7 and z = 8.1, respectively. The detection of bursts at this early epoch of the universe significantly constrains the nature of GRBs and their progenitors. We perform population synthesis studies of the formation and evolution of early stars, and calculate the resulting formation rates of short- and long-duration GRBs at high redshift. The peak of the GRB rate from Population II stars occurs at z similar to 7 for a model with efficient/fast mixing of metals, while it is found at z similar to 3 for an inefficient/slow metallicity evolution model. We show that in the redshift range 6 less than or similar to z less than or similar to 10, essentially all GRBs originate from Population II stars, regardless of the metallicity evolution model. These stars (having small, but non-zero metallicity) are the most likely progenitors for both long GRBs (collapsars) and short GRBs (neutron star-neutron star or blackhole-neutron star mergers) at this epoch. Although the predicted intrinsic rates of long and short GRBs are similar at these high redshifts, observational selection effects lead to higher (a factor of similar to 10) observed rates for long GRBs. We conclude that the two recently observed high-z GRB events are most likely long GRBs originating from Population II collapsars. C1 [Belczynski, Krzysztof; Holz, Daniel E.; Fryer, Chris L.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Belczynski, Krzysztof] Univ Warsaw, Astron Observ, PL-00478 Warsaw, Poland. [Berger, Edo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hartmann, Dieter H.] Clemson Univ, Dept Phys & Astron, Clemson, SC 29634 USA. [O'Shea, Brian] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. RP Belczynski, K (reprint author), Los Alamos Natl Lab, POB 1663, Los Alamos, NM 87545 USA. EM kbelczyn@nmsu.edu; daniel@restmass.com; clfreyer@lanl.gov; eberger@astro.princeton.edu; hdieter@CLEMSON.EDU; oshea@msu.edu FU KBN [N203 302835.] FX We thank the anonymous referee and Duncan Lorimer, Thomas Maccarone, and Ardrzej Zdziarski. K.B. acknowledges support from KBN grant N N203 302835. NR 103 TC 27 Z9 27 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 JAN 1 PY 2010 VL 708 IS 1 BP 117 EP 126 DI 10.1088/0004-637X/708/1/117 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 532ZM UT WOS:000272790400012 ER PT J AU Schnee, S Enoch, M Noriega-Crespo, A Sayers, J Terebey, S Caselli, P Foster, J Goodman, A Kauffmann, J Padgett, D Rebull, L Sargent, A Shetty, R AF Schnee, Scott Enoch, Melissa Noriega-Crespo, Alberto Sayers, Jack Terebey, Susan Caselli, Paola Foster, Jonathan Goodman, Alyssa Kauffmann, Jens Padgett, Deborah Rebull, Luisa Sargent, Anneila Shetty, Rahul TI THE DUST EMISSIVITY SPECTRAL INDEX IN THE STARLESS CORE TMC-1C SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; stars: formation ID TEMPERATURE-DEPENDENCE; ABSORPTION-COEFFICIENT; INITIAL CONDITIONS; SILICATE GRAINS; MOLECULAR CLOUD; MU-M; CONTINUUM; SPITZER; PERSEUS; TAURUS AB In this paper, we present a dust emission map of the starless core TMC-1C taken at 2100 mu m. Along with maps at 160, 450, 850, and 1200 mu m, we study the dust emissivity spectral index from the (sub)millimeter spectral energy distribution, and find that it is close to the typically assumed value of beta = 2. We also map the dust temperature and column density in TMC-1C, and find that at the position of the dust peak (A(V) similar to 50) the line-of-sight-averaged temperature is similar to 7 K. Employing simple Monte Carlo modeling, we show that the data are consistent with a constant value for the emissivity spectral index over the whole map of TMC-1C. C1 [Schnee, Scott; Shetty, Rahul] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Enoch, Melissa] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Noriega-Crespo, Alberto; Padgett, Deborah; Rebull, Luisa] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Sayers, Jack] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Terebey, Susan] Calif State Univ Los Angeles, Dept Phys & Astron PS315, Los Angeles, CA 90032 USA. [Caselli, Paola] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Foster, Jonathan; Goodman, Alyssa; Kauffmann, Jens; Shetty, Rahul] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Schnee, S (reprint author), NRC HIA, 5071 W Saanich Rd, Victoria, BC V9E 2E7, Canada. EM scott.schnee@nrc-cnrc.gc.ca RI Goodman, Alyssa/A-6007-2010; OI Goodman, Alyssa/0000-0003-1312-0477; Rebull, Luisa/0000-0001-6381-515X FU National Science Foundation [AST 05-40399]; NASA Postdoctoral Program; Spitzer Space Telescope; INSU/CNRS (France); MPG (Germany); IGN (Spain); NSF [AST 02-29008] FX We thank our referee, Yancy Shirley, for comments that improved the clarity of this paper. S.S. acknowledges support from the Owens Valley Radio Observatory, which is supported by the National Science Foundation through grant AST 05-40399. J.S. was partially supported by a NASA Postdoctoral Program Fellowship. Support was provided to M.E. by NASA through the Spitzer Space Telescope Fellowship Program. The JCMT is operated by the Joint Astronomy Centre on behalf of the Particle Physics and Astronomy Research Council of the United Kingdom, the Netherlands Organisation for Scientific Research, and the National Research Council of Canada. IRAM is supported by INSU/CNRS (France), MPG (Germany), and IGN (Spain). The CSO is supported by the NSF fund under contract AST 02-29008. NR 43 TC 33 Z9 33 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 JAN 1 PY 2010 VL 708 IS 1 BP 127 EP 136 DI 10.1088/0004-637X/708/1/127 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 532ZM UT WOS:000272790400013 ER PT J AU Merloni, A Bongiorno, A Bolzonella, M Brusa, M Civano, F Comastri, A Elvis, M Fiore, F Gilli, R Hao, H Jahnke, K Koekemoer, AM Lusso, E Mainieri, V Mignoli, M Miyaji, T Renzini, A Salvato, M Silverman, J Trump, J Vignali, C Zamorani, G Capak, P Lilly, SJ Sanders, D Taniguchi, Y Bardelli, S Carollo, CM Caputi, K Contini, T Coppa, G Cucciati, O de la Torre, S de Ravel, L Franzetti, P Garilli, B Hasinger, G Impey, C Iovino, A Iwasawa, K Kampczyk, P Kneib, JP Knobel, C Kovac, K Lamareille, F Le Borgne, JF Le Brun, V Le Fevre, O Maier, C Pello, R Peng, Y Montero, EP Ricciardelli, E Scodeggio, M Tanaka, M Tasca, LAM Tresse, L Vergani, D Zucca, E AF Merloni, A. Bongiorno, A. Bolzonella, M. Brusa, M. Civano, F. Comastri, A. Elvis, M. Fiore, F. Gilli, R. Hao, H. Jahnke, K. Koekemoer, A. M. Lusso, E. Mainieri, V. Mignoli, M. Miyaji, T. Renzini, A. Salvato, M. Silverman, J. Trump, J. Vignali, C. Zamorani, G. Capak, P. Lilly, S. J. Sanders, D. Taniguchi, Y. Bardelli, S. Carollo, C. M. Caputi, K. Contini, T. Coppa, G. Cucciati, O. de la Torre, S. de Ravel, L. Franzetti, P. Garilli, B. Hasinger, G. Impey, C. Iovino, A. Iwasawa, K. Kampczyk, P. Kneib, J. -P. Knobel, C. Kovac, K. Lamareille, F. Le Borgne, J. -F. Le Brun, V. Le Fevre, O. Maier, C. Pello, R. Peng, Y. Perez Montero, E. Ricciardelli, E. Scodeggio, M. Tanaka, M. Tasca, L. A. M. Tresse, L. Vergani, D. Zucca, E. TI ON THE COSMIC EVOLUTION OF THE SCALING RELATIONS BETWEEN BLACK HOLES AND THEIR HOST GALAXIES: BROAD-LINE ACTIVE GALACTIC NUCLEI IN THE ZCOSMOS SURVEY SO ASTROPHYSICAL JOURNAL LA English DT Review DE cosmology: observations; galaxies: active; galaxies: evolution; quasars: emission lines ID BH-SIGMA RELATION; SPECTRAL ENERGY-DISTRIBUTIONS; QUASI-STELLAR OBJECTS; HIGH-REDSHIFT QUASARS; RADIUS-LUMINOSITY RELATIONSHIP; STAR-FORMING GALAXIES; BULGE MASS RELATION; X-RAY; SEYFERT-1 GALAXIES; ELLIPTIC GALAXIES AB We report on the measurement of the physical properties (rest-frame K-band luminosity and total stellar mass) of the hosts of 89 broad-line (type-1) active galactic nuclei (AGNs) detected in the ZCOSMOS survey in the redshift range 1 < z < 2.2. The unprecedented multi-wavelength coverage of the survey field allows us to disentangle the emission of the host galaxy from that of the nuclear black hole in their spectral energy distributions (SEDs). We derive an estimate of black hole masses through the analysis of the broad Mg II emission lines observed in the medium-resolution spectra taken with VIMOS/VLT as part of the ZCOSMOS project. We found that, as compared to the local value, the average black hole to host-galaxy mass ratio appears to evolve positively with redshift, with a best-fit evolution of the form (1+ z)(0.68 +/- 0.12)(+0.6)(-0.3), where the large asymmetric systematic errors stem from the uncertainties in the choice of initial mass function, in the calibration of the virial relation used to estimate BH masses and in the mean QSO SED adopted. On the other hand, if we consider the observed rest-frame K-band luminosity, objects tend to be brighter, for a given black hole mass, than those on the local M(BH)-M(K) relation. This fact, together with more indirect evidence from the SED fitting itself, suggests that the AGN hosts are likely actively star-forming galaxies. A thorough analysis of observational biases induced by intrinsic scatter in the scaling relations reinforces the conclusion that an evolution of the M(BH)-M(*) relation must ensue for actively growing black holes at early times: either its overall normalization, or its intrinsic scatter (or both) appear to increase with redshift. This can be interpreted as signature of either a more rapid growth of supermassive black holes at high redshift, a change of structural properties of AGN hosts at earlier times, or a significant mismatch between the typical growth times of nuclear black holes and host galaxies. In any case, our results provide important clues on the nature of the early co-evolution of black holes and galaxies and challenging tests for models of AGN feedback and self-regulated growth of structures. C1 [Merloni, A.] TUM, Excellence Cluster Universe, D-85748 Garching, Germany. [Merloni, A.; Bongiorno, A.; Brusa, M.; Hasinger, G.] Max Planck Inst Extraterr Phys, D-85471 Garching, Germany. [Bongiorno, A.] Univ Maryland, Baltimore, MD 21250 USA. [Bolzonella, M.; Comastri, A.; Gilli, R.; Lusso, E.; Mignoli, M.; Zamorani, G.; Bardelli, S.; Coppa, G.; Iwasawa, K.; Vergani, D.; Zucca, E.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy. [Civano, F.; Elvis, M.; Hao, H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fiore, F.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Rm, Italy. [Jahnke, K.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Koekemoer, A. M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Mainieri, V.; Tanaka, M.] ESO, D-85748 Garching, Germany. [Miyaji, T.] UNAM, Inst Astron, Ensenada 22860, Baja California, Mexico. [Miyaji, T.] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. [Renzini, A.] INAF Osservatorio Astron Padova, Padua, Italy. [Salvato, M.; Capak, P.] CALTECH, Pasadena, CA 91125 USA. [Salvato, M.; Hasinger, G.] Max Planck Inst Plasma Phys, D-85748 Garching, Germany. [Silverman, J.; Lilly, S. J.; Carollo, C. M.; Caputi, K.; Kampczyk, P.; Knobel, C.; Kovac, K.; Maier, C.; Peng, Y.] ETH, Dept Phys, CH-8093 Zurich, Switzerland. [Trump, J.; Impey, C.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Vignali, C.; Coppa, G.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. [Capak, P.] 314 6 Caltech, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Sanders, D.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Taniguchi, Y.] Ehime Univ, Res Ctr Space & Cosm Evolut, Matsuyama, Ehime 7908577, Japan. [Contini, T.; Lamareille, F.; Le Borgne, J. -F.; Pello, R.; Perez Montero, E.] Univ Toulouse, CNRS, Lab Astrophys Toulouse Tarbes, F-31400 Toulouse, France. [Cucciati, O.; de la Torre, S.; de Ravel, L.; Kneib, J. -P.; Le Brun, V.; Le Fevre, O.; Tasca, L. A. M.; Tresse, L.] Univ Aix Marseille, CNRS, Lab Astrophys Marseille, F-13388 Marseille 13, France. [de la Torre, S.; Franzetti, P.; Garilli, B.; Iovino, A.; Scodeggio, M.; Tasca, L. A. M.] INAF IASF, I-20133 Milan, Italy. [de la Torre, S.] INAF Osservatorio Astron Brera, I-20121 Milan, Italy. [Perez Montero, E.] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. [Ricciardelli, E.] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy. RP Merloni, A (reprint author), TUM, Excellence Cluster Universe, Boltzmannstr 2, D-85748 Garching, Germany. RI Pello, Roser/G-4754-2010; Le Fevre, Olivier/G-7389-2011; Vignali, Cristian/J-4974-2012; Kneib, Jean-Paul/A-7919-2015; Zucca, Elena/O-9396-2015; Bardelli, Sandro/O-9369-2015; Mignoli, Marco/O-9426-2015; Bolzonella, Micol/O-9495-2015; Comastri, Andrea/O-9543-2015; Gilli, Roberto/P-1110-2015; OI Zamorani, Giovanni/0000-0002-2318-301X; Koekemoer, Anton/0000-0002-6610-2048; Perez Montero, E/0000-0003-3985-4882; Brusa, Marcella/0000-0002-5059-6848; Fiore, Fabrizio/0000-0002-4031-4157; Bongiorno, Angela/0000-0002-0101-6624; Scodeggio, Marco/0000-0002-2282-5850; Franzetti, Paolo/0000-0002-6986-0127; Vergani, Daniela/0000-0003-0898-2216; Jahnke, Knud/0000-0003-3804-2137; Maier, Christian/0000-0001-6405-2182; Garilli, Bianca/0000-0001-7455-8750; Vignali, Cristian/0000-0002-8853-9611; Kneib, Jean-Paul/0000-0002-4616-4989; Zucca, Elena/0000-0002-5845-8132; Bardelli, Sandro/0000-0002-8900-0298; Mignoli, Marco/0000-0002-9087-2835; Bolzonella, Micol/0000-0003-3278-4607; Comastri, Andrea/0000-0003-3451-9970; Gilli, Roberto/0000-0001-8121-6177; Iovino, Angela/0000-0001-6958-0304 FU NASA [HST-GO-09822]; INAF [PRIN/2007/1.06.10.08]; ASI [ASI/COFIS/WP3110 I/026/07/0]; CONACyT [83564]; PAPIIT [IN110209] FX This research was supported by the DFG cluster of excellence "Origin and Structure of the Universe." We thank the anonymous referee for carefully reading the manuscript and providing us with insightful and constructive remarks. We also thank R. Decarli, F. Fontanot, O. Gerhard, J. Greiner, P. Hopkins, S. Komossa, N. Menci, P. Monaco, H. Netzer, R. Saglia, L. Wisotzki, J.-H. Woo for their useful comments and suggestions. The HST COSMOS Treasury program was supported through NASA grant HST-GO-09822. We thank Tony Roman, Denise Taylor, and David Soderblom for their assistance in planning and scheduling of the extensive COSMOS observations. We gratefully acknowledge the contributions of the entire COSMOS collaboration consisting of more than 80 scientists. More information on the COSMOS survey is available at http://www.astro.caltech.edu/similar to cosmos. It is a pleasure to acknowledge the excellent services provided by the NASA IPAC/IRSA staff (Anastasia Laity, Anastasia Alexov, Bruce Berriman, and John Good) in providing online archive and server capabilities for the COSMOS data sets. In Italy, this work was partly supported by an INAF contract PRIN/2007/1.06.10.08 and an ASI grant ASI/COFIS/WP3110 I/026/07/0; in Mexico by the CONACyT grant program 83564 and PAPIIT IN110209; in Germany by the Bundesministerium fur Bildung und Forschung/Deutsches Zentrum fur Luft und Raumfahrt and the Max Planck Society. NR 146 TC 174 Z9 174 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 JAN 1 PY 2010 VL 708 IS 1 BP 137 EP 157 DI 10.1088/0004-637X/708/1/137 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 532ZM UT WOS:000272790400014 ER PT J AU Aulanier, G Torok, T Demoulin, P DeLuca, EE AF Aulanier, G. Toeroek, T. Demoulin, P. DeLuca, E. E. TI FORMATION OF TORUS-UNSTABLE FLUX ROPES AND ELECTRIC CURRENTS IN ERUPTING SIGMOIDS SO ASTROPHYSICAL JOURNAL LA English DT Review DE instabilities; methods: numerical; MHD; Sun: coronal mass ejections (CMEs); Sun: magnetic fields ID CORONAL MASS EJECTIONS; FREE MAGNETIC-FIELDS; QUASI-SEPARATRIX LAYERS; SOLAR ACTIVE-REGION; FORCE-FREE FIELDS; CURRENT SHEETS; EMERGING FLUX; NUMERICAL SIMULATIONS; DRIVEN EVOLUTION; KINK INSTABILITY AB We analyze the physical mechanisms that form a three-dimensional coronal flux rope and later cause its eruption. This is achieved by a zero-beta magnetohydrodynamic (MHD) simulation of an initially potential, asymmetric bipolar field, which evolves by means of simultaneous slow magnetic field diffusion and sub-Alfvenic, line-tied shearing motions in the photosphere. As in similarmodels, flux-cancellation-driven photospheric reconnection in a bald-patch (BP) separatrix transforms the sheared arcades into a slowly rising and stable flux rope. A bifurcation from a BP to a quasi-separatrix layer (QSL) topology occurs later on in the evolution, while the flux rope keeps growing and slowly rising, now due to shear-driven coronal slip-running reconnection, which is of tether-cutting type and takes place in the QSL. As the flux rope reaches the altitude at which the decay index -partial derivative ln B/partial derivative in z of the potential field exceeds similar to 3/2, it rapidly accelerates upward, while the overlying arcade eventually develops an inverse tear-drop shape, as observed in coronal mass ejections (CMEs). This transition to eruption is in accordance with the onset criterion of the torus instability. Thus, we find that photospheric flux-cancellation and tether-cutting coronal reconnection do not trigger CMEs in bipolar magnetic fields, but are key pre-eruptive mechanisms for flux ropes to build up and to rise to the critical height above the photosphere at which the torus instability causes the eruption. In order to interpret recent Hinode X-Ray Telescope observations of an erupting sigmoid, we produce simplified synthetic soft X-ray images from the distribution of the electric currents in the simulation. We find that a bright sigmoidal envelope is formed by pairs of J-shaped field lines in the pre-eruptive stage. These field lines form through the BP reconnection and merge later on into S-shaped loops through the tether-cutting reconnection. During the eruption, the central part of the sigmoid brightens due to the formation of a vertical current layer in the wake of the erupting flux rope. Slip-running reconnection in this layer yields the formation of flare loops. A rapid decrease of currents due to field line expansion, together with the increase of narrow currents in the reconnecting QSL, yields the sigmoid hooks to thin in the early stages of the eruption. Finally, a slightly rotating erupting loop-like feature (ELLF) detaches from the center of the sigmoid. Most of this ELLF is not associated with the erupting flux rope, but with a current shell that develops within expanding field lines above the rope. Only the short, curved end of the ELLF corresponds to a part of the flux rope. We argue that the features found in the simulation are generic for the formation and eruption of soft X-ray sigmoids. C1 [Aulanier, G.; Toeroek, T.; Demoulin, P.] Univ Paris Diderot, UPMC, Observ Paris, CNRS,LESIA, F-92190 Meudon, France. [DeLuca, E. E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02139 USA. RP Aulanier, G (reprint author), Univ Paris Diderot, UPMC, Observ Paris, CNRS,LESIA, 5 Pl Jules Janssen, F-92190 Meudon, France. RI DeLuca, Edward/L-7534-2013; OI DeLuca, Edward/0000-0001-7416-2895; Demoulin, Pascal/0000-0001-8215-6532 FU European Commission [MTRN-CT-2006-035484]; FP7 SOTERIA project [218816]; NASA [NNM07AB07C] FX The authors thank L. Golub and the referee for their helpful comments which improved the clarity of the paper. G. A. also thanks T. Amari for stimulating questions and discussions. The MHD calculations were done on the quadri-core bi-Xeon computers of the Cluster of the Service Informatique of Paris Observatory. 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). Financial supports by the European Commission through the FP6 SOLAIRE Network (MTRN-CT-2006-035484) and through the FP7 SOTERIA project (Grant Agreement No. 218816) are gratefully acknowledged. E.E.D. was supported by NASA contract NNM07AB07C. NR 119 TC 192 Z9 192 U1 0 U2 11 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JAN 1 PY 2010 VL 708 IS 1 BP 314 EP 333 DI 10.1088/0004-637X/708/1/314 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 532ZM UT WOS:000272790400028 ER PT J AU Kilic, M Brown, WR McLeod, B AF Kilic, Mukremin Brown, Warren R. McLeod, B. TI A SPITZER SEARCH FOR SUBSTELLAR COMPANIONS TO LOW-MASS WHITE DWARFS SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared: stars; planetary systems; stars: low-mass; brown dwarfs; white dwarfs ID STELLAR EVOLUTION; BROWN DWARFS; SOLAR NEIGHBORHOOD; CLOSE BINARIES; DODO SURVEY; GIANT STAR; PLANETS; MODELS; LIMITS; IA AB The formation scenarios for single low-mass (M < 0.45 M(circle dot)) white dwarfs (WDs) include enhanced mass loss from a metal-rich progenitor star or a common envelope phase of a solar-like star with a close-in massive planet or a brown dwarf. Both scenarios suggest that low-mass WDs may have planets. Here, we present a Spitzer IRAC search for substellar and planetary mass companions to 14 low-mass WDs. One of our targets, HS 1653+7753, displays near- and mid-infrared flux excess. However, follow-up MMT observations show that this excess is due to a nearby resolved source, which is mostly likely a background object. Another target, PG 2257+162, shows flux excess compatible with a late-type stellar companion. We do not detect substellar companions to any of the remaining targets. In addition, eight of these stars do not show any radial velocity variations, ruling out stellar mass companions including other WDs. We conclude that a significant fraction of the low-mass WDs in our sample do not have stellar or massive brown dwarf companions. C1 [Kilic, Mukremin; Brown, Warren R.; McLeod, B.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Kilic, M (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM mkilic@cfa.harvard.edu FU NASA FX Support for this work was provided by NASA through the Spitzer Space Telescope Fellowship Program, under an award from Caltech. We thank the MMIRS commissioning team for obtaining the observations, and T. von Hippel for a careful reading of an earlier version of this manuscript. We also thank an anonymous referee for useful suggestions. NR 51 TC 11 Z9 11 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 JAN 1 PY 2010 VL 708 IS 1 BP 411 EP 418 DI 10.1088/0004-637X/708/1/411 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 532ZM UT WOS:000272790400036 ER PT J AU Rau, A Roelofs, GHA Groot, PJ Marsh, TR Nelemans, G Steeghs, D Salvato, M Kasliwal, MM AF Rau, A. Roelofs, G. H. A. Groot, P. J. Marsh, T. R. Nelemans, G. Steeghs, D. Salvato, M. Kasliwal, M. M. TI A CENSUS OF AM CVn STARS: THREE NEW CANDIDATES AND ONE CONFIRMED 48.3-MINUTE BINARY SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; binaries: close; novae, cataclysmic variables; stars: individual (SDSS J090221.34+381941.9, SDSS J152509.57+360054.5, SDSS J164228.06+193410.0, SDSS J172102.48+273301.2); white dwarfs ID CANUM-VENATICORUM BINARIES; DIGITAL SKY SURVEY; DOUBLE-DEGENERATE BINARY; ORBITAL PERIOD; LOW-RESOLUTION; WHITE-DWARFS; GP COM; SYSTEMS; POPULATION; KINEMATICS AB We present three new candidate AM CVn binaries, and one confirmed new system, from a spectroscopic survey of color-selected objects from the Sloan Digital Sky Survey (SDSS). All four systems were found from their helium emission lines in low-resolution spectra taken on the Hale telescope at Palomar, the Nordic Optical Telescope, and the William Herschel Telescope on La Palma. The ultra-compact binary nature of SDSS J090221.35+381941.9 was confirmed using phase-resolved spectroscopy at the Keck-I telescope. From the characteristic radial velocity "S-wave" observed in the helium emission lines, we measure an orbital period of 48.31 +/- 0.08 minutes. The continuum emission can be described with a blackbody or a helium white dwarf atmosphere of T(eff) similar to 15,000 K, in agreement with theoretical cooling models for relatively massive accretors and/or donors. The absence in the spectrum of broad helium absorption lines from the accreting white dwarf suggests that the accreting white dwarf cannot be much hotter than 15,000 K, or that an additional component such as the accretion disk contributes substantially to the optical flux. Two of the candidate systems, SDSS J152509.57+360054.5 and SDSS J172102.48+273301.2, do show helium absorption in the blue part of their spectra in addition to the characteristic helium emission lines. This in combination with the high effective temperatures of similar to 18,000 K and similar to 16,000 K suggests both to be at orbital periods below similar to 40 minutes. The third candidate, SDSS J164228.06+193410.0, exhibits remarkably strong helium emission on top of a relatively cool (T(eff) similar to 12,000 K) continuum, indicating an orbital period above similar to 50 minutes. C1 [Rau, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Rau, A.; Salvato, M.; Kasliwal, M. M.] CALTECH, Opt Observ, Pasadena, CA 91125 USA. [Roelofs, G. H. A.; Steeghs, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Groot, P. J.; Nelemans, G.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands. [Marsh, T. R.; Steeghs, D.] Univ Warwick, Dept Phys, Coventry CV4 7A1, W Midlands, England. [Salvato, M.] Max Planck Inst Plasma Phys, D-85748 Garching, Germany. RP Rau, A (reprint author), Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85748 Garching, Germany. EM arau@mpe.mpg.de RI Nelemans, Gijs/D-3177-2012; Steeghs, Danny/C-5468-2009; Groot, Paul/K-4391-2016 OI Nelemans, Gijs/0000-0002-0752-2974; Steeghs, Danny/0000-0003-0771-4746; Groot, Paul/0000-0002-4488-726X FU NASA [NNX08AK66G]; NWO [680.50.0610]; California Institute of Technology, the University of California; National Aeronautics and Space Administration (NASA); W.M. Keck Foundation FX A.R. acknowledges support through NASA grant NNX08AK66G. G.H. A.R. is supported by NWO Rubicon grant 680.50.0610. D. S. acknowledges a STFC Advanced Fellowship. This paper is based on data obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration (NASA). The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. We also acknowledge use of the Palomar Hale-5 m telescope operated by the California Institute of Technology and Palomar Observatory; the Nordic Optical Telescope and the William Herschel Telescope, La Palma; and the GALEX public archive. We are grateful to D. Koester for kindly making available his white dwarf atmosphere models. NR 33 TC 32 Z9 32 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 JAN 1 PY 2010 VL 708 IS 1 BP 456 EP 461 DI 10.1088/0004-637X/708/1/456 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 532ZM UT WOS:000272790400042 ER PT J AU Todorov, K Deming, D Harrington, J Stevenson, KB Bowman, WC Nymeyer, S Fortney, JJ Bakos, GA AF Todorov, Kamen Deming, Drake Harrington, Jospeph Stevenson, Kevin B. Bowman, William C. Nymeyer, Sarah Fortney, Jonathan J. Bakos, Gaspar A. TI SPITZER IRAC SECONDARY ECLIPSE PHOTOMETRY OF THE TRANSITING EXTRASOLAR PLANET HAT-P-1b SO ASTROPHYSICAL JOURNAL LA English DT Article DE eclipses; planetary systems; techniques: photometric ID INFRARED-EMISSION SPECTRUM; EXOPLANET HD 189733B; THERMAL EMISSION; TEMPERATURE INVERSION; HOT JUPITERS; GIANT PLANETS; LIGHT CURVES; ATMOSPHERES; 209458B; SEARCH AB We report Spitzer/IRAC photometry of the transiting giant exoplanet HAT-P-1b during its secondary eclipse. This planet lies near the postulated boundary between the pM and pL-class of hot Jupiters, and is important as a test of models for temperature inversions in hot Jupiter atmospheres. We derive eclipse depths for HAT-P-1b, in units of the stellar flux, that are: 0.080%+/- 0.008% [3.6 mu m], 0.135%+/- 0.022% [4.5 mu m], 0.203%+/- 0.031% [5.8 mu m], and 0.238%+/- 0.040% [8.0 mu m]. These values are best fit using an atmosphere with a modest temperature inversion, intermediate between the archetype inverted atmosphere (HD 209458b) and a model without an inversion. The observations also suggest that this planet is radiating a large fraction of the available stellar irradiance on its dayside, with little available for redistribution by circulation. This planet has sometimes been speculated to be inflated by tidal dissipation, based on its large radius in discovery observations, and on a non-zero orbital eccentricity allowed by the radial velocity data. The timing of the secondary eclipse is very sensitive to orbital eccentricity, and we find that the central phase of the eclipse is 0.4999 +/- 0.0005. The difference between the expected and observed phase indicates that the orbit is close to circular, with a 3 sigma limit of vertical bar e cos omega vertical bar < 0.002. C1 [Todorov, Kamen; Deming, Drake] Goddard Space Flight Ctr, Goddard Ctr Astrobiol, Greenbelt, MD 20771 USA. [Harrington, Jospeph; Stevenson, Kevin B.; Bowman, William C.; Nymeyer, Sarah] Univ Cent Florida, Dept Phys, Planetary Sci Grp, Orlando, FL 32816 USA. [Fortney, Jonathan J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Bakos, Gaspar A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Todorov, Kamen] Connecticut Coll, Dept Phys Astron & Geophys, New London, CT 06320 USA. RP Todorov, K (reprint author), Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. RI Harrington, Joseph/E-6250-2011; OI Fortney, Jonathan/0000-0002-9843-4354; Todorov, Kamen/0000-0002-9276-8118; Stevenson, Kevin/0000-0002-7352-7941; Harrington, Joseph/0000-0002-8955-8531 FU NASA 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. We are grateful to the anonymous referee for thoughtful comments that improved this paper. NR 32 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 JAN 1 PY 2010 VL 708 IS 1 BP 498 EP 504 DI 10.1088/0004-637X/708/1/498 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 532ZM UT WOS:000272790400047 ER PT J AU Westra, E Geller, MJ Kurtz, MJ Fabricant, DG Dell'Antonio, I AF Westra, Eduard Geller, Margaret J. Kurtz, Michael J. Fabricant, Daniel G. Dell'Antonio, Ian TI EVOLUTION OF THE H alpha LUMINOSITY FUNCTION SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: interactions; galaxies: luminosity function, mass function; galaxies: starburst ID STAR-FORMATION RATE; DIGITAL SKY SURVEY; GALAXY REDSHIFT SURVEY; FIBER-FED SPECTROGRAPH; FORMATION RATE DENSITY; SUBARU DEEP FIELD; FORMING GALAXIES; FORMATION HISTORY; METALLICITY RELATION; EMITTING GALAXIES AB The Smithsonian Hectospec Lensing Survey (SHELS) is a window on the star formation history over the last 4 Gyr. SHELS is a spectroscopically complete survey for R(tot) < 20.3 over 4 square degrees. We use the 10k spectra to select a sample of pure star-forming galaxies based on their Ha emission line. We use the spectroscopy to determine extinction corrections for individual galaxies and to remove active galaxies in order to reduce systematic uncertainties. We use the large volume of SHELS with the depth of a narrowband survey for H alpha galaxies at z similar to 0.24 to make a combined determination of the H alpha luminosity function at z similar to 0.24. The large area covered by SHELS yields a survey volume big enough to determine the bright end of the H alpha luminosity function from redshift 0.100 to 0.377 for an assumed fixed faint-end slope alpha = -1.20. The bright end evolves: the characteristic luminosity L* increases by 0.84 dex over this redshift range. Similarly, the star formation density increases by 0.11 dex. The fraction of galaxies with a close neighbor increases by a factor of 2-5 for LH alpha greater than or similar to L* in each of the redshift bins. We conclude that triggered star formation is an important influence for star-forming galaxies with H alpha emission. C1 [Westra, Eduard; Geller, Margaret J.; Kurtz, Michael J.; Fabricant, Daniel G.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Dell'Antonio, Ian] Brown Univ, Dept Phys, Providence, RI 02912 USA. RP Westra, E (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM ewestra@cfa.harvard.edu RI KURTZ, Michael /B-3890-2009 NR 70 TC 27 Z9 27 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 JAN 1 PY 2010 VL 708 IS 1 BP 534 EP 549 DI 10.1088/0004-637X/708/1/534 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 532ZM UT WOS:000272790400049 ER PT J AU Frebel, A Simon, JD Geha, M Willman, B AF Frebel, Anna Simon, Joshua D. Geha, Marla Willman, Beth TI HIGH-RESOLUTION SPECTROSCOPY OF EXTREMELY METAL-POOR STARS IN THE LEAST EVOLVED GALAXIES: URSA MAJOR II and COMA BERENICES SO ASTROPHYSICAL JOURNAL LA English DT Review DE early universe; galaxies: dwarf; Galaxy: halo; Local Group; stars: abundances; stars: Population II ID DWARF SPHEROIDAL GALAXY; NEUTRON-CAPTURE ELEMENTS; MILKY-WAY SATELLITES; HIGH-DISPERSION-SPECTROGRAPH; GALACTIC CHEMICAL EVOLUTION; CORE-COLLAPSE SUPERNOVAE; 1ST STARS; METALLICITY DISTRIBUTION; GIANT STARS; LOCAL GROUP AB We present spectra of six metal-poor stars in two of the ultra-faint dwarf galaxies orbiting the Milky Way (MW), Ursa Major II, and Coma Berenices obtained with the Keck/High Resolution Echelle Spectrometer (HIRES). These observations include the first high-resolution spectroscopic observations of extremely metal-poor ([Fe/H] < -3.0) stars not belonging to the MW halo field star population. We obtain abundance measurements and upper limits for 26 elements between carbon and europium. The entire sample of stars spans a range of -3.2 < [Fe/H] < -2.3, and we confirm that each galaxy contains a large intrinsic spread of Fe abundances. A comparison with MW halo stars of similar metallicities reveals substantial agreement between the abundance patterns of the ultra-faint dwarf galaxies and the MW halo for the light, alpha, and iron-peak elements (C to Zn). This agreement contrasts with the results of earlier studies of more metal-rich stars (-2.5 less than or similar to [Fe/H] less than or similar to -1.0) in more luminous dwarf spheroidal galaxies, which found significant abundance discrepancies with respect to the MW halo data. The abundances of neutron-capture elements (Sr to Eu) in the ultra-faint dwarf galaxies are extremely low, consistent with the most metal-poor halo stars, but not with the typical halo abundance pattern at [Fe/H] greater than or similar to -3.0. Not only are our results broadly consistent with a galaxy formation model that predicts that massive dwarf galaxies are the source of the metal-rich component ([Fe/H] > -2.5) of the MW halo, but they also suggest that the faintest known dwarfs may be the primary contributors to the metal-poor end of the MW halo metallicity distribution. C1 [Frebel, Anna] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Frebel, Anna] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA. [Simon, Joshua D.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [Geha, Marla] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Willman, Beth] Haverford Coll, Haverford, PA 19041 USA. RP Frebel, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM afrebel@cfa.harvard.edu; jsimon@ociw.edu; marla.geha@yale.edu; bwillman@haverford.edu NR 114 TC 132 Z9 132 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 JAN 1 PY 2010 VL 708 IS 1 BP 560 EP 583 DI 10.1088/0004-637X/708/1/560 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 532ZM UT WOS:000272790400051 ER PT J AU Goodger, JL Hardcastle, MJ Croston, JH Kraft, RP Birkinshaw, M Evans, DA Jordan, A Nulsen, PEJ Sivakoff, GR Worrall, DM Brassington, NJ Forman, WR Gilfanov, M Jones, C Murray, SS Raychaudhury, S Sarazin, CL Voss, R Woodley, KA AF Goodger, J. L. Hardcastle, M. J. Croston, J. H. Kraft, R. P. Birkinshaw, M. Evans, D. A. Jordan, A. Nulsen, P. E. J. Sivakoff, G. R. Worrall, D. M. Brassington, N. J. Forman, W. R. Gilfanov, M. Jones, C. Murray, S. S. Raychaudhury, S. Sarazin, C. L. Voss, R. Woodley, K. A. TI LONG-TERM MONITORING OF THE DYNAMICS AND PARTICLE ACCELERATION OF KNOTS IN THE JET OF CENTAURUS A SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: individual (Centaurus A, NGC 5128); galaxies: jets; X-rays: galaxies ID X-RAY-EMISSION; ACTIVE GALACTIC NUCLEI; M87 JET; CHANDRA OBSERVATIONS; GLOBULAR-CLUSTERS; SPITZER OBSERVATIONS; HOT-SPOTS; RADIO; HST-1; LOBES AB We present new and archival multi-frequency radio and X-ray data for Centaurus A obtained over almost 20 years at the Very Large Array and with Chandra, with which we measure the X-ray and radio spectral indices of jet knots, flux density variations in the jet knots, polarization variations, and proper motions. We compare the observed properties with current knot formation models and particle acceleration mechanisms. We rule out impulsive particle acceleration as a formation mechanism for all of the knots as we detect the same population of knots in all of the observations, and we find no evidence of extreme variability in the X-ray knots. We find that the most likely mechanism for all the stationary knots is a collision resulting in a local shock followed by a steady state of prolonged, stable particle acceleration, and X-ray synchrotron emission. In this scenario, the X-ray-only knots have radio counterparts that are too faint to be detected, while the radio-only knots are due to weak shocks where no particles are accelerated to X-ray emitting energies. Although the base knots are prime candidates for reconfinement shocks, the presence of a moving knot in this vicinity and the fact that there are two base knots are hard to explain in this model. We detect apparent motion in three knots; however, their velocities and locations provide no conclusive evidence for or against a faster moving "spine" within the jet. The radio-only knots, both stationary and moving, may be due to compression of the fluid. C1 [Goodger, J. L.; Hardcastle, M. J.] Univ Hertfordshire, Sch Phys Astron & Math, Hatfield AL10 9AB, Herts, England. [Croston, J. H.] Univ Southampton, Southampton SO17 1BJ, Hants, England. [Kraft, R. P.; Birkinshaw, M.; Jordan, A.; Nulsen, P. E. J.; Worrall, D. M.; Brassington, N. J.; Forman, W. R.; Jones, C.; Murray, S. S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Birkinshaw, M.; Worrall, D. M.] Univ Bristol, Dept Phys, Bristol BS8 ITL, Avon, England. [Evans, D. A.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Jordan, A.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 7820436, Chile. [Sivakoff, G. R.; Sarazin, C. L.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Gilfanov, M.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Raychaudhury, S.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Voss, R.] Excellence Cluster Universe Tech Univ Munchen, D-85748 Garching, Germany. [Woodley, K. A.] McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1, Canada. European So Observ, D-85748 Garching, Germany. RP Goodger, JL (reprint author), Univ Hertfordshire, Sch Phys Astron & Math, Coll Lane, Hatfield AL10 9AB, Herts, England. EM j.l.goodger@herts.ac.uk; m.j.hardcastle@herts.ac.uk; J.Croston@soton.ac.uk; kraft@head.cfa.harvard.edu; mark.birkinshaw@bristol.ac.uk; devans@space.mit.edu; ajordan@astro.puc.cl; pnulsen@cfa.harvard.edu; grs8g@virginia.edu; d.m.worrall@bristol.ac.uk; nbrassington@cfa.harvard.edu; wforman@cfa.harvard.edu; gilfanov@MPA-Garching.mpg.de; cjones@cfa.harvard.edu; ssm@cfa.harvard.edu; somak@star.sr.bham.ac.uk; sarazin@virginia.edu; rvoss@mpe.mpg.de; woodleka@physics.mcmaster.ca RI Hardcastle, Martin/E-2264-2012; Sivakoff, Gregory/G-9602-2011 OI Goodger, Joanna/0000-0002-5738-4768; Jordan, Andres/0000-0002-5389-3944; Nulsen, Paul/0000-0003-0297-4493; Forman, William/0000-0002-9478-1682; Hardcastle, Martin/0000-0003-4223-1117; Sivakoff, Gregory/0000-0001-6682-916X FU STFC; Royal Society; NASA [GO7-8105X]; Associated Universities, Inc. FX We gratefully acknowledge financial support for this work from the STFC (research studentship for J. L. G.), the Royal Society (research fellowship for M. J. H.), and NASA (grant GO7-8105X to R. P. K.). The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. We acknowledge helpful comments from an anonymous referee. NR 49 TC 20 Z9 20 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 JAN 1 PY 2010 VL 708 IS 1 BP 675 EP 697 DI 10.1088/0004-637X/708/1/675 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 532ZM UT WOS:000272790400060 ER PT J AU Bartko, H Martins, F Trippe, S Fritz, TK Genzel, R Ott, T Eisenhauer, F Gillessen, S Paumard, T Alexander, T Dodds-Eden, K Gerhard, O Levin, Y Mascetti, L Nayakshin, S Perets, HB Perrin, G Pfuhl, O Reid, MJ Rouan, D Zilka, M Sternberg, A AF Bartko, H. Martins, F. Trippe, S. Fritz, T. K. Genzel, R. Ott, T. Eisenhauer, F. Gillessen, S. Paumard, T. Alexander, T. Dodds-Eden, K. Gerhard, O. Levin, Y. Mascetti, L. Nayakshin, S. Perets, H. B. Perrin, G. Pfuhl, O. Reid, M. J. Rouan, D. Zilka, M. Sternberg, A. TI AN EXTREMELY TOP-HEAVY INITIAL MASS FUNCTION IN THE GALACTIC CENTER STELLAR DISKS SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy: center; stars: early-type; stars: luminosity function, mass function ID SUPERMASSIVE BLACK-HOLES; CENTRAL PARSEC; STAR-FORMATION; YOUNG STARS; MILKY-WAY; VELOCITY DISPERSION; DYNAMICAL FRICTION; GLOBULAR CLUSTER; NUCLEAR CLUSTER; ACCRETION DISK AB We present new observations of the nuclear star cluster in the central parsec of the Galaxy with the adaptive optics assisted, integral field spectrograph SINFONI on the ESO/VLT. Our work allows the spectroscopic detection of early- and late-type stars to m(K) >= 16, more than 2 mag deeper than our previous data sets. Our observations result in a total sample of 177 bona fide early- type stars. We find that most of these Wolf Rayet (WR), O-, and B-stars reside in two strongly warped disks between 0 ''.8 and 12 '' from Sgr A*, as well as a central compact concentration (the S-star cluster) centered on Sgr A*. The later type B-stars (m(K) > 15) in the radial interval between 0 ''.8 and 12 '' seem to be in a more isotropic distribution outside the disks. The observed dearth of late-type stars in the central few arcseconds is puzzling, even when allowing for stellar collisions. The stellar mass function of the disk stars is extremely top heavy with a best-fit power law of dN/dm alpha m(-0.45 +/- 0.3). WR/O-stars were formed in situ in a single star formation event similar to 6 Myr ago, this mass function probably reflects the initial mass function (IMF). The mass functions of the S-stars inside 0 ''.8 and of the early- type stars at distances beyond 12 '' are compatible with a standard Salpeter/Kroupa IMF (best-fit power law of dN/dm alpha m(-2.15 +/- 0.3)). C1 [Bartko, H.; Martins, F.; Fritz, T. K.; Genzel, R.; Ott, T.; Eisenhauer, F.; Gillessen, S.; Dodds-Eden, K.; Gerhard, O.; Mascetti, L.; Pfuhl, O.] Max Planck Inst Extraterr Phys, D-37075 Garching, Germany. [Martins, F.] Univ Montpellier 2, CNRS, GRAAL, UMR5024, F-34095 Montpellier, France. [Trippe, S.] IRAM Grenoble, F-38406 St Martin Dheres, France. [Genzel, R.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Paumard, T.; Perrin, G.; Rouan, D.] Univ Paris Direrot, UPMC, CNRS, Observ Paris,LESIA, Meudon, France. [Alexander, T.; Perets, H. B.] Weizmann Inst Sci, Fac Phys, IL-76100 Rehovot, Israel. [Levin, Y.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Levin, Y.] Leiden Univ, Inst Lorentz, NL-2300 RA Leiden, Netherlands. [Nayakshin, S.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Reid, M. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. [Zilka, M.; Sternberg, A.] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. RP Bartko, H (reprint author), Max Planck Inst Extraterr Phys, D-37075 Garching, Germany. EM hbartko@mpe.mpg.de; fabrice.martins@graal.univ-montp2.fr RI Perets, Hagai/K-9605-2015 OI Perets, Hagai/0000-0002-5004-199X FU DFG [STE1869/1-1.GE625/15-1] FX We thank all the ESO staff for their help during the various observing runs, and Melvyn Davies for a discussion on his work on stellar collisions. We thank the DFG for support via German-Israeli Project Cooperation grant STE1869/1-1.GE625/15-1. We thank the referee, Don Figer, for his comments and suggestions. NR 73 TC 161 Z9 161 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 JAN 1 PY 2010 VL 708 IS 1 BP 834 EP 840 DI 10.1088/0004-637X/708/1/834 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 532ZM UT WOS:000272790400071 ER PT J AU Smolcic, V Zamorani, G Schinnerer, E Bardelli, S Bondi, M Birzan, L Carilli, CL Ciliegi, P Elvis, M Impey, CD Koekemoer, AM Merloni, A Paglione, T Salvato, M Scodeggio, M Scoville, N Trump, JR AF Smolcic, V. Zamorani, G. Schinnerer, E. Bardelli, S. Bondi, M. Birzan, L. Carilli, C. L. Ciliegi, P. Elvis, M. Impey, C. D. Koekemoer, A. M. Merloni, A. Paglione, T. Salvato, M. Scodeggio, M. Scoville, N. Trump, J. R. TI COSMIC EVOLUTION OF RADIO SELECTED ACTIVE GALACTIC NUCLEI IN THE COSMOS FIELD (vol 696, pg 24, 2009) SO ASTROPHYSICAL JOURNAL LA English DT Correction C1 [Smolcic, V.; Salvato, M.; Scoville, N.] CALTECH, Pasadena, CA 91125 USA. [Zamorani, G.; Bardelli, S.; Ciliegi, P.] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy. [Schinnerer, E.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Bondi, M.] Inst Radioastron, INAF, I-40129 Bologna, Italy. [Birzan, L.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Birzan, L.] Ohio Univ, Dept Phys & Astron, Clippinger Labs, Athens, OH 45701 USA. [Carilli, C. L.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Elvis, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Impey, C. D.; Trump, J. R.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Koekemoer, A. M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Merloni, A.] Tech Univ Munich, D-85748 Garching, Germany. [Merloni, A.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Paglione, T.] CUNY York Coll, Jamaica, NY 11451 USA. [Paglione, T.] Amer Museum Nat Hist, New York, NY 10024 USA. [Scodeggio, M.] IASF Milano INAF, I-20133 Milan, Italy. RP Smolcic, V (reprint author), CALTECH, MC 105-24,1200 E Calif Blvd, Pasadena, CA 91125 USA. RI Bardelli, Sandro/O-9369-2015 OI Bardelli, Sandro/0000-0002-8900-0298 NR 1 TC 2 Z9 2 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 JAN 1 PY 2010 VL 708 IS 1 BP 909 EP 909 DI 10.1088/0004-637X/708/1/909 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 532ZM UT WOS:000272790400075 ER PT J AU Foley, RJ Brown, PJ Rest, A Challis, PJ Kirshner, RP Wood-Vasey, WM AF Foley, Ryan J. Brown, Peter J. Rest, Armin Challis, Peter J. Kirshner, Robert P. Wood-Vasey, W. Michael TI EARLY- AND LATE-TIME OBSERVATIONS OF SN 2008ha: ADDITIONAL CONSTRAINTS FOR THE PROGENITOR AND EXPLOSION SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE supernovae: general; supernovae: individual (SN 2008ha) ID THERMONUCLEAR SUPERNOVAE; IA SUPERNOVAE; 2005HK; SPECTROGRAPH; 2002CX; PHASE AB We present a new maximum-light optical spectrum of the extremely low luminosity and exceptionally low-energy Type Ia supernova (SN Ia) 2008ha, obtained one week before the earliest published spectrum. Previous observations of SN 2008ha were unable to distinguish between a massive star and white dwarf (WD) origin for the SN. The new maximum-light spectrum, obtained one week before the earliest previously published spectrum, unambiguously shows features corresponding to intermediate mass elements, including silicon, sulfur, and carbon. Although strong silicon features are seen in some core-collapse SNe, sulfur features, which are a signature of carbon/oxygen burning, have always been observed to be weak in such events. It is therefore likely that SN 2008ha was the result of a thermonuclear explosion of a carbon-oxygen WD. Carbon features at maximum light show that unburned material is present to significant depths in the SN ejecta, strengthening the case that SN 2008ha was a failed deflagration. We also present late-time imaging and spectroscopy that are consistent with this scenario. C1 [Foley, Ryan J.; Challis, Peter J.; Kirshner, Robert P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Brown, Peter J.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Rest, Armin] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Wood-Vasey, W. Michael] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. RP Foley, RJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rfoley@cfa.harvard.edu FU Clay Fellowship; NSF [AST09-07903]; US National Science Foundation on behalf of the Gemini partnership; Science and Technology Facilities Council (United Kingdom); National Research Council (Canada); CONICYT (Chile); Australian Research Council (Australia); Ministerio da Ciencia e Tecnologia (Brazil); Ministerio de Ciencia, Tecnologia e Innovacion Productiva (Argentina) FX Based in part on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the US National Science Foundation on behalf of the Gemini partnership: the NSF (United States), the Science and Technology Facilities Council (United Kingdom), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministerio da Ciencia e Tecnologia (Brazil), and Ministerio de Ciencia, Tecnologia e Innovacion Productiva (Argentina). The HET is a joint project of the University of Texas at Austin, the Pennsylvania State University, Stanford University, Ludwig-Maximilians-Universitat Munchen, and Georg-August-Universitat Gottingen. The HET is named in honor of its principal benefactors, William P. Hobby and Robert E. Eberly. The Marcario LRS is named for Mike Marcario of High Lonesome Optics who fabricated several optics for the instrument but died before its completion. The LRS is a joint project of the HET partnership and the Instituto de Astronomia de la Universidad Nacional Autonoma de Mexico. NR 24 TC 49 Z9 49 U1 2 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JAN 1 PY 2010 VL 708 IS 1 BP L61 EP L65 DI 10.1088/2041-8205/708/1/L61 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 540BX UT WOS:000273306700014 ER PT J AU Kotochigova, S Linnik, M Kirby, KP Brickhouse, NS AF Kotochigova, S. Linnik, M. Kirby, K. P. Brickhouse, N. S. TI RADIATIVE L-SHELL TRANSITIONS IN Fe XIX AND Fe XX IONS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE atomic data; atomic processes; line: identification; X-rays: general ID PERTURBATION-THEORY; CHANDRA; CAPELLA; EMISSION; GRATINGS; RATIOS; XVIII AB We compute the wavelengths and oscillator strengths for the 3s, 3d -> 2p, and 3p -> 2s emission lines in Fe XIX and Fe XX ions by using a configuration interaction Dirac-Fock and Dirac-Fock-Sturm method combined with second-order Brillouin-Wigner perturbation theory. We provide a complete list of computed wavelengths and oscillator strengths in both the velocity and length gauge for these transitions, many of which have never previously been reported. A comparison of our data with laboratory measurements and other theoretical predictions allows us to estimate an uncertainty of similar to 2 m angstrom in the wavelengths and an uncertainty of 2%-3% in the oscillator strengths. We expect that our calculations will provide a means of identifying emission lines from astrophysical sources and improve the ability to detect blending in X-ray grating spectra from Chandra and XMM-Newton. As an example, we present a simulated emission spectrum of Capella and find improved agreement between the observations and our calculations, compared with previous data sets. C1 [Kotochigova, S.; Linnik, M.] Temple Univ, Dept Phys, Philadelphia, PA 19122 USA. [Kirby, K. P.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys, Cambridge, MA 02138 USA. RP Kotochigova, S (reprint author), Temple Univ, Dept Phys, Philadelphia, PA 19122 USA. OI Brickhouse, Nancy/0000-0002-8704-4473 FU Smithsonian Institution; NASA [NAS8-03060] FX S. K. and M. L. acknowledge partial support from the Smithsonian Institution Atherton Seidell Fund through the Smithsonian Astrophysical Observatory. N. S. B. acknowledges support from NASA contract NAS8-03060 to the Chandra X-ray Center. NR 19 TC 6 Z9 6 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD JAN PY 2010 VL 186 IS 1 BP 85 EP 93 DI 10.1088/0067-0049/186/1/85 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 538JH UT WOS:000273179900005 ER PT J AU Croft, B Lohmann, U Martin, RV Stier, P Wurzler, S Feichter, J Hoose, C Heikkila, U van Donkelaar, A Ferrachat, S AF Croft, B. Lohmann, U. Martin, R. V. Stier, P. Wurzler, S. Feichter, J. Hoose, C. Heikkila, U. van Donkelaar, A. Ferrachat, S. TI Influences of in-cloud aerosol scavenging parameterizations on aerosol concentrations and wet deposition in ECHAM5-HAM SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID GENERAL-CIRCULATION MODEL; CHEMICAL TRACER MODEL; GLOBAL CLIMATE MODEL; ICE CRYSTAL PLATES; THEORETICAL DETERMINATION; SIZE DISTRIBUTIONS; CIRRUS CLOUDS; TRANSPORT; PB-210; BE-7 AB A diagnostic cloud nucleation scavenging scheme, which determines stratiform cloud scavenging ratios for both aerosol mass and number distributions, based on cloud droplet, and ice crystal number concentrations, is introduced into the ECHAM5-HAM global climate model. This scheme is coupled with a size-dependent in-cloud impaction scavenging parameterization for both cloud droplet-aerosol, and ice crystal-aerosol collisions. The aerosol mass scavenged in stratiform clouds is found to be primarily (>90%) scavenged by cloud nucleation processes for all aerosol species, except for dust (50%). The aerosol number scavenged is primarily (>90%) attributed to impaction. 99% of this impaction scavenging occurs in clouds with temperatures less than 273 K. Sensitivity studies are presented, which compare aerosol concentrations, burdens, and deposition for a variety of incloud scavenging approaches: prescribed fractions, a more computationally expensive prognostic aerosol cloud processing treatment, and the new diagnostic scheme, also with modified assumptions about in-cloud impaction and nucleation scavenging. Our results show that while uncertainties in the representation of in-cloud scavenging processes can lead to differences in the range of 20-30% for the predicted annual, global mean aerosol mass burdens, and near to 50% for accumulation mode aerosol number burden, the differences in predicted aerosol mass concentrations can be up to one order of magnitude, particularly for regions of the middle troposphere with temperatures below 273K where mixed and ice phase clouds exist. Different parameterizations for impaction scavenging changed the predicted global, annual mean number removal attributed to ice clouds by seven-fold, and the global, annual dust mass removal attributed to impaction by two orders of magnitude. Closer agreement with observations of black carbon profiles from aircraft (increases near to one order of magnitude for mixed phase clouds), mid-troposphere Pb-210 vertical profiles, and the geographic distribution of aerosol optical depth is found for the new diagnostic scavenging scheme compared to the prescribed scavenging fraction scheme of the standard ECHAM5-HAM. The diagnostic and prognostic schemes represent the variability of scavenged fractions particularly for submicron size aerosols, and for mixed and ice phase clouds, and are recommended in preference to the prescribed scavenging fractions method. C1 [Croft, B.; Martin, R. V.; van Donkelaar, A.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS, Canada. [Lohmann, U.; Ferrachat, S.] ETH, Inst Atmospher & Climate Sci, Zurich, Switzerland. [Martin, R. V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Stier, P.] Univ Oxford, Oxford, England. [Wurzler, S.] LANUV, Recklinghausen, Germany. [Feichter, J.] Max Planck Inst Meteorol, Hamburg, Germany. [Hoose, C.] Univ Oslo, Dept Geosci, Oslo, Norway. [Heikkila, U.] Bjerknes Ctr Climate Res, Bergen, Norway. RP Croft, B (reprint author), Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS, Canada. EM croft@mathstat.dal.ca RI Hoose, Corinna/A-4295-2009; Stier, Philip/B-2258-2008; Martin, Randall/C-1205-2014; Lohmann, Ulrike/B-6153-2009 OI Hoose, Corinna/0000-0003-2827-5789; Stier, Philip/0000-0002-1191-0128; Martin, Randall/0000-0003-2632-8402; Lohmann, Ulrike/0000-0001-8885-3785 FU National Science and Engineering Research Council of Canada; Killam Trusts Foundation of Canada FX The authors are grateful to the National Science and Engineering Research Council of Canada and Killam Trusts Foundation of Canada for financial support. We thank D. Koch, and the following groups associated with providing aircraft data: NOAA at UC Boulder (David Fahey), University of Tokyo (Y. Kondo), and University of Hawaii (T. Clarke). Thanks also to CSCS for computing time. NR 55 TC 32 Z9 32 U1 2 U2 19 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1680-7316 EI 1680-7324 J9 ATMOS CHEM PHYS JI Atmos. Chem. Phys. PY 2010 VL 10 IS 4 BP 1511 EP 1543 PG 33 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 559TS UT WOS:000274851500003 ER PT J AU Liu, X Bhartia, PK Chance, K Spurr, RJD Kurosu, TP AF Liu, X. Bhartia, P. K. Chance, K. Spurr, R. J. D. Kurosu, T. P. TI Ozone profile retrievals from the Ozone Monitoring Instrument SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID ROTATIONAL RAMAN-SCATTERING; TROPOSPHERIC OZONE; TROPICAL ATLANTIC; SATELLITE; POLLUTION; ALGORITHM; VALIDATION; DERIVATION; RADIANCES; TRANSPORT AB Ozone profiles from the surface to about 60 km are retrieved from Ozone Monitoring Instrument (OMI) ultraviolet radiances using the optimal estimation technique. OMI provides daily ozone profiles for the entire sunlit portion of the earth at a horizontal resolution of 13 kmx48 km for the nadir position. The retrieved profiles have sufficient accuracy in the troposphere to see ozone perturbations caused by convection, biomass burning and anthropogenic pollution, and to track their spatiotemporal transport. However, to achieve such accuracy it has been necessary to calibrate OMI radiances carefully (using two days of Aura/Microwave Limb Sounder data taken in the tropics). The retrieved profiles contain similar to 6-7 degrees of freedom for signal, with 5-7 in the stratosphere and 0-1.5 in the troposphere. Vertical resolution varies from 7-11 km in the stratosphere to 10-14 km in the troposphere. Retrieval precisions range from 1% in the middle stratosphere to 10% in the lower stratosphere and troposphere. Solution errors (i.e., root sum square of precisions and smoothing errors) vary from 1-6% in the middle stratosphere to 6-35% in the troposphere, and are dominated by smoothing errors. Total, stratospheric, and tropospheric ozone columns can be retrieved with solution errors typically in the few Dobson unit range at solar zenith angles less than 80 degrees. C1 [Liu, X.] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. [Liu, X.; Chance, K.; Kurosu, T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Liu, X.; Bhartia, P. K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Spurr, R. J. D.] RT Solut Inc, Cambridge, MA USA. RP Liu, X (reprint author), Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. EM xliu@cfa.harvard.edu RI Liu, Xiong/P-7186-2014; Bhartia, Pawan/A-4209-2016; OI Liu, Xiong/0000-0003-2939-574X; Bhartia, Pawan/0000-0001-8307-9137; Chance, Kelly/0000-0002-7339-7577 FU NASA [NNG06GH99G]; New Investigator Program in Earth Science [NNX08AN98G]; Smithsonian Institution FX This study was supported by the NASA Atmospheric Composition Program (NNG06GH99G), the New Investigator Program in Earth Science (NNX08AN98G), and the Smithsonian Institution. The Dutch-Finnish OMI instrument is part of the NASA EOS Aura satellite payload. The OMI Project is managed by NIVR and KNMI in the Netherlands. We acknowledge the OMI International Science Team and MLS science team for providing satellite data used in this study. NCEP Reanalysis data are provided by NOAA/OAR/ESRL PSD, Boulder, CO, USA, from their Web site at http://www.cdc.noaa.gov. We also thank J. Joiner, S. Taylor, and G. Jaross for discussions on OMI radiance calibration. NR 60 TC 81 Z9 83 U1 6 U2 29 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1680-7316 EI 1680-7324 J9 ATMOS CHEM PHYS JI Atmos. Chem. Phys. PY 2010 VL 10 IS 5 BP 2521 EP 2537 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 568ER UT WOS:000275505500029 ER PT J AU Liu, X Bhartia, PK Chance, K Froidevaux, L Spurr, RJD Kurosu, TP AF Liu, X. Bhartia, P. K. Chance, K. Froidevaux, L. Spurr, R. J. D. Kurosu, T. P. TI Validation of Ozone Monitoring Instrument (OMI) ozone profiles and stratospheric ozone columns with Microwave Limb Sounder (MLS) measurements SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article AB We validate OMI ozone profiles between 0.22-215 hPa and stratospheric ozone columns down to 215 hPa (SOC215) against v2.2 MLS data from 2006. The validation demonstrates convincingly that SOC can be derived accurately from OMI data alone, with errors comparable to or smaller than those from current MLS retrievals, and it demonstrates implicitly that tropospheric ozone column can be retrieved accurately from OMI or similar nadir-viewing ultraviolet measurements alone. The global mean biases are within 2.5% above 100 hPa and 5-10% below 100 hPa; the standard deviations of the differences (1 sigma) are 3.5-5% between 1-50 hPa, 6-9% above 1 hPa and 8-15% below 50 hPa. OMI shows some latitude and solar zenith angle dependent biases, but the mean biases are mostly within 5% and the standard deviations are mostly within 2-5% except for low altitudes and high latitudes. The excellent agreement with MLS data shows that OMI retrievals can be used to augment the validation of MLS and other stratospheric ozone measurements made with even higher vertical resolution than that for OMI. OMI SOC215 shows a small bias of -0.6% with a standard deviation of 2.8%. When compared as a function of latitude and solar zenith angle, the mean biases are within 2% and the standard deviations range from 2.1 to 3.4%. Assuming 2% precision for MLS SOC215, we deduce that the upper limits of random-noise and smoothing errors for OMI SOC215 range from 0.6% in the southern tropics to 2.8% at northern middle latitudes. C1 [Liu, X.] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. [Liu, X.; Chance, K.; Kurosu, T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Liu, X.; Bhartia, P. K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Froidevaux, L.] NASA, Jet Prop Lab, Pasadena, CA USA. [Spurr, R. J. D.] RT Solut Inc, Cambridge, MA USA. RP Liu, X (reprint author), Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. EM xliu@cfa.harvard.edu RI Liu, Xiong/P-7186-2014; Bhartia, Pawan/A-4209-2016; OI Liu, Xiong/0000-0003-2939-574X; Bhartia, Pawan/0000-0001-8307-9137; Chance, Kelly/0000-0002-7339-7577 FU NASA Atmospheric Composition Program [NNG06GH99G]; Smithsonian Institution FX This study was supported by the NASA Atmospheric Composition Program (NNG06GH99G) and by the Smithsonian Institution. The Dutch-Finnish OMI instrument is part of the NASA EOS Aura satellite payload. The OMI Project is managed by NIVR and KNMI in the Netherlands. We acknowledge the OMI International Science Team and MLS science team for the satellite data used in this study. NR 14 TC 27 Z9 28 U1 0 U2 6 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1680-7316 J9 ATMOS CHEM PHYS JI Atmos. Chem. Phys. PY 2010 VL 10 IS 5 BP 2539 EP 2549 PG 11 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 568ER UT WOS:000275505500030 ER PT J AU Slowik, JG Stroud, C Bottenheim, JW Brickell, PC Chang, RYW Liggio, J Makar, PA Martin, RV Moran, MD Shantz, NC Sjostedt, SJ van Donkelaar, A Vlasenko, A Wiebe, HA Xia, AG Zhang, J Leaitch, WR Abbatt, JPD AF Slowik, J. G. Stroud, C. Bottenheim, J. W. Brickell, P. C. Chang, R. Y. -W. Liggio, J. Makar, P. A. Martin, R. V. Moran, M. D. Shantz, N. C. Sjostedt, S. J. van Donkelaar, A. Vlasenko, A. Wiebe, H. A. Xia, A. G. Zhang, J. Leaitch, W. R. Abbatt, J. P. D. TI Characterization of a large biogenic secondary organic aerosol event from eastern Canadian forests SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID POSITIVE MATRIX FACTORIZATION; CLOUD CONDENSATION NUCLEI; MULTISCALE GEM MODEL; MASS-SPECTROMETER; MEXICO-CITY; HIGH-RESOLUTION; ALPHA-PINENE; PHOTOCHEMICAL OXIDATION; SOURCE APPORTIONMENT; LIGHT-SCATTERING AB Measurements of aerosol composition, volatile organic compounds, and CO are used to determine biogenic secondary organic aerosol (SOA) concentrations at a rural site 70 km north of Toronto. These biogenic SOA levels are many times higher than past observations and occur during a period of increasing temperatures and outflow from Northern Ontario and Quebec forests in early summer. A regional chemical transport model approximately predicts the event timing and accurately predicts the aerosol loading, identifying the precursors as monoterpene emissions from the coniferous forest. The agreement between the measured and modeled biogenic aerosol concentrations contrasts with model underpredictions for polluted regions. Correlations of the oxygenated organic aerosol mass with tracers such as CO support a secondary aerosol source and distinguish biogenic, pollution, and biomass burning periods during the field campaign. Using the Master Chemical Mechanism, it is shown that the levels of CO observed during the biogenic event are consistent with a photochemical source arising from monoterpene oxidation. The biogenic aerosol mass correlates with satellite measurements of regional aerosol optical depth, indicating that the event extends across the eastern Canadian forest. This regional event correlates with increased temperatures, indicating that temperature-dependent forest emissions can significantly affect climate through enhanced direct optical scattering and higher cloud condensation nuclei numbers. C1 [Slowik, J. G.; Chang, R. Y. -W.; Shantz, N. C.; Sjostedt, S. J.; Vlasenko, A.; Abbatt, J. P. D.] Univ Toronto, Dept Chem, Toronto, ON M5S 1A1, Canada. [Stroud, C.; Bottenheim, J. W.; Brickell, P. C.; Liggio, J.; Makar, P. A.; Moran, M. D.; Shantz, N. C.; Vlasenko, A.; Wiebe, H. A.; Xia, A. G.; Zhang, J.; Leaitch, W. R.] Environm Canada, Sci & Technol Branch, Toronto, ON, Canada. [Martin, R. V.; van Donkelaar, A.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS, Canada. [Martin, R. V.] Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. RP Abbatt, JPD (reprint author), Univ Toronto, Dept Chem, 80 St George St, Toronto, ON M5S 1A1, Canada. EM jabbatt@chem.utoronto.ca RI Vlasenko, Alexander/B-4280-2008; Slowik, Jay/F-4894-2011; Xia, Adam/A-6823-2013; Martin, Randall/C-1205-2014; Sjostedt, Steven/B-5032-2015; OI Slowik, Jay/0000-0001-5682-850X; Martin, Randall/0000-0003-2632-8402; Chang, Rachel/0000-0003-2337-098X FU Canadian Foundation for Climate and Atmospheric Sciences; Natural Science and Engineering Research Council (Canada) FX This work was supported by the Canadian Foundation for Climate and Atmospheric Sciences through the Cloud-Aerosol Feedbacks and Climate Network and by the Natural Science and Engineering Research Council (Canada). Partial infrastructure funding came from CFI and OIT. The authors also thank Dr. Jiannan Li for discussion of the radiative forcing calculations, Prof. Rainer Volkamer for discussion of the SOA yield calculation, and the MODIS team for measurements of aerosol optical depth. NR 105 TC 79 Z9 79 U1 0 U2 39 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1680-7316 EI 1680-7324 J9 ATMOS CHEM PHYS JI Atmos. Chem. Phys. PY 2010 VL 10 IS 6 BP 2825 EP 2845 DI 10.5194/acp-10-2825-2010 PG 21 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 576XA UT WOS:000276182100018 ER PT J AU Zhang, L Jacob, DJ Liu, X Logan, JA Chance, K Eldering, A Bojkov, BR AF Zhang, L. Jacob, D. J. Liu, X. Logan, J. A. Chance, K. Eldering, A. Bojkov, B. R. TI Intercomparison methods for satellite measurements of atmospheric composition: application to tropospheric ozone from TES and OMI SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID UNITED-STATES; MONITORING INSTRUMENT; EMISSION SPECTROMETER; STRATOSPHERIC OZONE; MODEL DESCRIPTION; HIGH-RESOLUTION; AIR-QUALITY; 3-D MODELS; A-PRIORI; DISTRIBUTIONS AB We analyze the theoretical basis of three different methods to validate and intercompare satellite measurements of atmospheric composition, and apply them to tropospheric ozone retrievals from the Tropospheric Emission Spectrometer (TES) and the Ozone Monitoring Instrument (OMI). The first method (in situ method) uses in situ vertical profiles for absolute instrument validation; it is limited by the sparseness of in situ data. The second method (CTM method) uses a chemical transport model (CTM) as an intercomparison platform; it provides a globally complete intercomparison with relatively small noise from model error. The third method (averaging kernel smoothing method) involves smoothing the retrieved profile from one instrument with the averaging kernel matrix of the other; it also provides a global intercomparison but dampens the actual difference between instruments and adds noise from the a priori. We apply the three methods to a full year (2006) of TES and OMI data. Comparison with in situ data from ozonesondes shows mean positive biases of 5.3 parts per billion volume (ppbv) (10%) for TES and 2.8 ppbv (5%) for OMI at 500 hPa. We show that the CTM method (using the GEOS-Chem CTM) closely approximates results from the in situ method while providing global coverage. It reveals that differences between TES and OMI are generally less than 10 ppbv (18%), except at northern mid-latitudes in summer and over tropical continents. The CTM method further allows for CTM evaluation using both satellite observations. We thus find that GEOS-Chem underestimates tropospheric ozone in the tropics due to possible underestimates of biomass burning, soil, and lightning emissions. It overestimates ozone in the northern subtropics and southern mid-latitudes, likely because of excessive stratospheric influx of ozone. C1 [Zhang, L.; Jacob, D. J.] Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. [Jacob, D. J.; Logan, J. A.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. [Liu, X.] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. [Liu, X.; Chance, K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Liu, X.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Eldering, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bojkov, B. R.] European Space Agcy ESA ESRIN, Sci Applicat & Future Technol Dept, I-00044 Frascati, RM, Italy. RP Zhang, L (reprint author), Harvard Univ, Dept Earth & Planetary Sci, 20 Oxford St, Cambridge, MA 02138 USA. EM linzhang@fas.harvard.edu RI Zhang, Lin/A-6729-2008; Zhang, Lin/H-9801-2014; Chem, GEOS/C-5595-2014; Liu, Xiong/P-7186-2014; OI Zhang, Lin/0000-0003-2383-8431; Liu, Xiong/0000-0003-2939-574X; Chance, Kelly/0000-0002-7339-7577 FU NASA [NNX07AN65H, NNX08AN98G, NNG06GH99G]; Smithsonian Institution FX This work was funded by the NASA Atmospheric Composition Modeling and Analysis Program and by NASA Headquarters under the Earth and Space Science Fellowship Program Grant NNX07AN65H to Lin Zhang, and by the New Investigator Program in Earth Science (NNX08AN98G) to Xiong Liu. Xiong Liu and Kelly Chance also acknowledge support from the NASA Atmospheric Composition Program (NNG06GH99G) and the Smithsonian Institution. NR 66 TC 44 Z9 45 U1 1 U2 15 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1680-7316 EI 1680-7324 J9 ATMOS CHEM PHYS JI Atmos. Chem. Phys. PY 2010 VL 10 IS 10 BP 4725 EP 4739 DI 10.5194/acp-10-4725-2010 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 603CE UT WOS:000278184700020 ER PT J AU Curci, G Palmer, PI Kurosu, TP Chance, K Visconti, G AF Curci, G. Palmer, P. I. Kurosu, T. P. Chance, K. Visconti, G. TI Estimating European volatile organic compound emissions using satellite observations of formaldehyde from the Ozone Monitoring Instrument SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID MASTER CHEMICAL MECHANISM; MCM V3 PART; ATMOSPHERIC CHEMISTRY; ISOPRENE EMISSIONS; TROPOSPHERIC DEGRADATION; BIOGENIC EMISSIONS; NORTH-AMERICA; MODEL; INVENTORY; POLLUTION AB Emission of non-methane Volatile Organic Compounds (VOCs) to the atmosphere stems from biogenic and human activities, and their estimation is difficult because of the many and not fully understood processes involved. In order to narrow down the uncertainty related to VOC emissions, which negatively reflects on our ability to simulate the atmospheric composition, we exploit satellite observations of formaldehyde (HCHO), an ubiquitous oxidation product of most VOCs, focusing on Europe. HCHO column observations from the Ozone Monitoring Instrument (OMI) reveal a marked seasonal cycle with a summer maximum and winter minimum. In summer, the oxidation of methane and other long-lived VOCs supply a slowly varying background HCHO column, while HCHO variability is dominated by most reactive VOC, primarily biogenic isoprene followed in importance by biogenic terpenes and anthropogenic VOCs. The chemistry-transport model CHIMERE qualitatively reproduces the temporal and spatial features of the observed HCHO column, but display regional biases which are attributed mainly to incorrect biogenic VOC emissions, calculated with the Model of Emissions of Gases and Aerosol from Nature (MEGAN) algorithm. These "bottom-up" or a-priori emissions are corrected through a Bayesian inversion of the OMI HCHO observations. Resulting "top-down" or a-posteriori isoprene emissions are lower than "bottom-up" by 40% over the Balkans and by 20% over Southern Germany, and higher by 20% over Iberian Peninsula, Greece and Italy. We conclude that OMI satellite observations of HCHO can provide a quantitative "top-down" constraint on the European "bottom-up" VOC inventories. C1 [Curci, G.; Visconti, G.] Univ Aquila, Dipartimento Fis, CETEMPS, I-67100 Laquila, Italy. [Palmer, P. I.] Univ Edinburgh, Sch GeoSci, Edinburgh, Midlothian, Scotland. [Kurosu, T. P.; Chance, K.] Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. RP Curci, G (reprint author), Univ Aquila, Dipartimento Fis, CETEMPS, I-67100 Laquila, Italy. EM gabriele.curci@aquila.infn.it RI Palmer, Paul/F-7008-2010; Curci, Gabriele/A-2020-2011; OI Curci, Gabriele/0000-0001-9871-5570; Chance, Kelly/0000-0002-7339-7577 FU Italian Space Agency (ASI) [I/035/06/0] FX The work is part of the Pilot Project QUIT-SAT, funded by the Italian Space Agency (ASI), contract I/035/06/0 NR 81 TC 27 Z9 27 U1 5 U2 34 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1680-7316 EI 1680-7324 J9 ATMOS CHEM PHYS JI Atmos. Chem. Phys. PY 2010 VL 10 IS 23 BP 11501 EP 11517 DI 10.5194/acp-10-11501-2010 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 694XJ UT WOS:000285334900013 ER PT J AU Lerner, HRL Fleischer, RC AF Lerner, Heather R. L. Fleischer, Robert C. TI PROSPECTS FOR THE USE OF NEXT-GENERATION SEQUENCING METHODS IN ORNITHOLOGY SO AUK LA English DT Review ID COMPLETE MITOCHONDRIAL GENOMES; MICROBIAL DIVERSITY; WOOLLY MAMMOTHS; DARWINS FINCHES; AVIAN GENOMICS; SNP DISCOVERY; DNA; GENE; TRANSCRIPTOME; LIBRARIES C1 [Lerner, Heather R. L.; Fleischer, Robert C.] Smithsonian Inst, Natl Museum Nat Hist, Ctr Conservat & Evolutionary Genet, Washington, DC 20013 USA. RP Lerner, HRL (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Ctr Conservat & Evolutionary Genet, Natl Zool Pk,POB 37012,MRC 5503, Washington, DC 20013 USA. EM hlerner@gmail.com FU NGSMs; National Science Foundation [DEB-0643291] FX We thank M. Meyer, M. Hofreiter, F. Hailer, D. Locke, S. Schuster, and K. Heigen for elucidation and discussion of NGSMs and the National Science Foundation (DEB-0643291) for funding. O. Ryder and A. R. Hoelzel provided valuable comments on all earlier version of the manuscript. Online resources for analysis of next-generation sequencing data are available at the following websites: seqanswers.com/forums/showthread.php?t=43, and http://www.sanger.ac.uk/resources/software/. saiigei-.ac.Lik/i-esources/softxware/. NR 86 TC 27 Z9 30 U1 2 U2 31 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 JAN PY 2010 VL 127 IS 1 BP 4 EP 15 DI 10.1525/auk.2010.127.1.4 PG 12 WC Ornithology SC Zoology GA 554RQ UT WOS:000274452500002 ER PT J AU Smith, ZF James, EA McLean, CB AF Smith, Zoe F. James, Elizabeth A. McLean, Cassandra B. TI Mycorrhizal specificity of Diuris fragrantissima (Orchidaceae) and persistence in a reintroduced population SO AUSTRALIAN JOURNAL OF BOTANY LA English DT Article ID IN-SITU; SYMBIOTIC GERMINATION; TERRESTRIAL ORCHIDS; FUNGI; CONSERVATION; SEEDLINGS; SEED; PROPAGATION; DIVERSITY; BUSHLAND AB This study investigated the diversity and specificity of mycorrhizal fungi associated with five Diuris (Orchidaceae) taxa in south-eastern Australia, as part of a reintroduction program for the endangered species Diuris fragrantissima. We compared fungi isolated from D. fragrantissima occurring naturally in the only remaining population with those from artificially cultivated plants and reintroduced plants 18 months after planting in a new field site west of Melbourne. Genetic similarity of nuclear internal transcribed spacer and nuclear large subunit DNA sequences showed that Diuris taxa associate with a narrow taxonomic range of fungi within the cosmopolitan family Tulasnellaceae in the Rhizoctonia alliance. All fungal isolates induced host seed germination and hence were considered mycorrhizal. Fungal isolates from naturally occurring D. fragrantissima plants showed a higher level of genetic similarity than fungi isolated from cultivated plants. This observation suggests that, historically, the species may have associated with a more genetically variable range of Tulasnella fungi. Artificially cultivated D. fragrantissima were propagated aseptically from seed and spontaneously formed mycorrhizal associations within 6 months of transfer to potting media. Wild collected D. fragrantissima plants maintained in cultivation for over 30 years were found to contain mycorrhizal fungi similar to those isolated from naturally occurring plants in 2004-2006. Mycorrhizal associations in artificially cultivated D. fragrantissima were present in 18 randomly sampled plants 18 months after reintroduction. Further, associations formed between several reintroduced plants and a fungus concurrently inoculated into site soil. We propose that future orchid reintroductions may benefit from the concurrent addition of suitable mycorrhizal fungi to site soil. Maintenance of orchid mycorrhizal relationships after reintroduction is essential to improve long-term viability of reintroduced populations. C1 [Smith, Zoe F.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [James, Elizabeth A.] Royal Bot Gardens Melbourne, S Yarra, Vic 3141, Australia. [McLean, Cassandra B.] Univ Melbourne, Burnley Coll, Fac Land & Food Resources, Sch Resource Management, Richmond, Vic 3121, Australia. RP Smith, ZF (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM smithz@si.edu FU Australian Systematic Botany Society Hansjorg Eichler Scientific Research Fund FX This paper is dedicated to the fond memory of Cassandra B. McLean; a dedicated mycorrhizal ecologist and inspiring and encouraging mentor. We thank the Department of Sustainability and the Environment, Australasian Native Orchid Society Victorian Group, Melbourne Zoo, Parks Victoria and the Threatened Orchid Recovery Team for assistance with fieldwork. This research was supported by an Australian Systematic Botany Society Hansjorg Eichler Scientific Research Fund to Z.S. We also sincerely thank Sally Smith for revising the manuscript and providing valuable comments and discussion, and an anonymous reviewer for constructive feedback. NR 48 TC 4 Z9 6 U1 8 U2 24 PU CSIRO PUBLISHING PI COLLINGWOOD PA 150 OXFORD ST, PO BOX 1139, COLLINGWOOD, VICTORIA 3066, AUSTRALIA SN 0067-1924 EI 1444-9862 J9 AUST J BOT JI Aust. J. Bot. PY 2010 VL 58 IS 2 BP 97 EP 106 DI 10.1071/BT09214 PG 10 WC Plant Sciences SC Plant Sciences GA 574YS UT WOS:000276030700003 ER PT J AU Craddock, RA Hutchinson, MF Stein, JA AF Craddock, R. A. Hutchinson, M. F. Stein, J. A. TI Topographic data reveal a buried fluvial landscape in the Simpson Desert, Australia SO AUSTRALIAN JOURNAL OF EARTH SCIENCES LA English DT Article DE floodouts; groundwater flow; linear dunes; paleodrainage; paleovalleys; playas; Simpson Desert ID DIGITAL ELEVATION MODELS; SHUTTLE RADAR; WIND-RIFT; DUNES; AREAS AB Buried river channels and valleys have proven to be valuable economic and agricultural resources. Often they are ecologically important refugia and in some instances, such as in the Sahara Desert, serve as dramatic reminders of the climatic changes that have taken place. Here we report the determination of a fluvial landscape that is substantially buried under the Simpson Desert using a digital elevation model (DEM) specifically derived for this purpose. The DEM is a grid of ground-level elevation points with a spacing of 9 s in longitude and latitude (similar to 250 m). It was calculated by applying the ANUDEM gridding algorithm to national spot height elevation data taken from 1: 100 000 scale topographic maps. The ANUDEM algorithm includes a drainage enforcement algorithm that has been found to reliably discern drainage structure from minimally sampled point elevation data in central Queensland and broad-scale paleodrainage structure in Western Australia. To avoid erroneously high-elevation information, source elevation data were only selected from between dunes in the Simpson Desert region, providing a more accurate basis for determination of the general surface topography and its underlying paleodrainage structure that existed prior to the development of the dunefields. The DEM reveals the broader, low-frequency topography in the Simpson Desert, reflecting the landscape buried up to 35 m below the sand surface. The paleodrainage analysis is in good agreement with data from the Shuttle Radar Topographic Mission (SRTM). It is now possible to trace a network of topographic lows that are likely to represent paleochannels through the driest desert in Australia and plot the former courses of the world's oldest rivers prior to their burial. C1 [Craddock, R. A.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. [Hutchinson, M. F.; Stein, J. A.] Australian Natl Univ, Fenner Sch Environm & Soc, Canberra, ACT 0200, Australia. RP Craddock, RA (reprint author), Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. EM craddockb@si.edu RI Craddock, Robert/B-3884-2013 FU National Aeronautics and Space Administration [NAG5-12180]; Smithsonian Institution's George F. Becker Endowment FX This paper benefited greatly from meticulous reviews by Pauline English and Colin Pain. We thank T. Farr and Janet Stein for support. We also appreciate help with fieldwork by Alan Howard, Ross Irwin, Ted Maxwell, Stephen Tooth and Sharon Wilson, and reviews by Ted Maxwell and Stephen Tooth prior to submission. This work was supported by grants to RAC from the National Aeronautics and Space Administration (NAG5-12180) and the Smithsonian Institution's George F. Becker Endowment. NR 40 TC 5 Z9 5 U1 1 U2 12 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0812-0099 J9 AUST J EARTH SCI JI Aust. J. Earth Sci. PY 2010 VL 57 IS 1 BP 141 EP 149 DI 10.1080/08120090903416278 PG 9 WC Geosciences, Multidisciplinary SC Geology GA 546AS UT WOS:000273780000007 ER PT J AU Meyer, KM Schiffers, K Munkemuller, T Schadler, M Calabrese, JM Basset, A Breulmann, M Duquesne, S Hidding, B Huth, A Schob, C van de Voorde, TFJ AF Meyer, Katrin M. Schiffers, Katja Muenkemueller, Tamara Schaedler, Martin Calabrese, Justin M. Basset, Alberto Breulmann, Marc Duquesne, Sabine Hidding, Bert Huth, Andreas Schoeb, Christian van de Voorde, Tess F. J. TI Predicting population and community dynamics: The type of aggregation matters SO BASIC AND APPLIED ECOLOGY LA English DT Article DE Scales; Organizational level; Pattern-process relationship; Trophic guild; Functional type; Species; Phenotype; Genotype; Body size class; Study design ID PLANT GENOTYPE; BODY-SIZE; ENVIRONMENTAL-CHANGE; SOIL-MICROORGANISMS; ECOLOGICAL NETWORKS; TRAIT CONVERGENCE; TROPHIC GUILDS; BEWICKS SWANS; BURIAL DEPTH; FOOD WEBS AB When investigating complex ecological dynamics at the population or community level, we necessarily need to abstract and aggregate ecological information. The way in which information is aggregated may be crucial for the outcome of the study. In this paper, we suggest that in addition to the traditional spatial, temporal and organizational levels, we need a more flexible framework linking ecological processes, study objects and types of aggregation. We develop such a framework and exemplify the most commonly used types of aggregation and their potential influence on identifiable drivers of community dynamics. We also illustrate strategies to narrow down the range of possible aggregation types for a particular study. With this approach, we hope (i) to clarify the function of aggregation types as related to traditional ecological levels and (ii) to raise the awareness of how important a deliberate way of aggregating ecological information is for a sound and reliable outcome of any empirical or theoretical ecological study. C1 [Meyer, Katrin M.] Univ Gottingen, Fac Forest Sci & Forest Ecol, D-37077 Gottingen, Germany. [Meyer, Katrin M.; van de Voorde, Tess F. J.] Netherlands Inst Ecol NIOO KNAW, Dept Terr Ecol, NL-6666 GA Heteren, Netherlands. [Schiffers, Katja] Univ Aberdeen, Sch Biol Sci, Aberdeen AB24 2TZ, Scotland. [Schiffers, Katja] Univ Potsdam, Dept Plant Ecol & Nat Conservat, D-14469 Potsdam, Germany. [Muenkemueller, Tamara; Calabrese, Justin M.; Huth, Andreas] UFZ Helmholtz Ctr Environm Res, Dept Ecol Modelling, D-04301 Leipzig, Germany. [Muenkemueller, Tamara] Univ Grenoble 1, Lab Ecol Alpine, CNRS, UMR 5553, FR-38041 Grenoble 9, France. [Schaedler, Martin] Univ Marburg, Dept Anim Ecol, D-35032 Marburg, Germany. [Basset, Alberto] Univ Salento, Dept Biol & Environm Sci & Technol, I-73100 Lecce, Italy. [Breulmann, Marc] UFZ Helmholtz Ctr Environm Res, Dept Soil Ecol, D-06120 Halle, Germany. [Duquesne, Sabine] UFZ Helmholtz Ctr Environm Res, Dept Conservat Biol, D-04318 Leipzig, Germany. [Duquesne, Sabine] UFZ Helmholtz Ctr Environm Res, Dept Syst Ecotoxicol, D-04318 Leipzig, Germany. [Hidding, Bert] Netherlands Inst Ecol NIOO KNAW, Dept Aquat Ecol, NL-3631 AC Nieuwersluis, Netherlands. [Schoeb, Christian] Univ Bern, Inst Geog, CH-3012 Bern, Switzerland. [van de Voorde, Tess F. J.] Univ Wageningen & Res Ctr, Nematol Lab, NL-6700 ES Wageningen, Netherlands. [Calabrese, Justin M.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. RP Meyer, KM (reprint author), Univ Gottingen, Fac Forest Sci & Forest Ecol, Busgenweg 4, D-37077 Gottingen, Germany. EM kmeyer5@uni-goettingen.de RI Hidding, Bert/C-3622-2008; Schob, Christian/B-6083-2008; Schadler, Martin/H-3176-2011; Duquesne, Sabine/H-5575-2011; Calabrese, Justin/B-9131-2012; Meyer, Katrin/E-6839-2013; van de Voorde, Tess/G-1812-2011; Calabrese, Pascale/M-6350-2014 OI Schob, Christian/0000-0003-4472-2286; Schadler, Martin/0000-0001-9700-0311; Meyer, Katrin/0000-0002-9990-4047; van de Voorde, Tess/0000-0002-2802-5619; FU EU [NEST 43268]; German Academic Exchange Service (DAAD); State of Lower Saxony (Ministry of Science and Culture) FX We thank Hauke Reuter and three anonymous reviewers for valuable comments on previous versions of this manuscript. We are grateful to the organizers of the Annual Meeting of the Society of Ecology of Germany, Austria and Switzerland GfO and of the XI Conference of the European Ecological Federation EURECO in Leipzig, 2008, for hosting the session on whose results this paper is based. JMC was funded by the EU project PATRES (NEST 43268). KS was supported by the German Academic Exchange Service (DAAD). KMM was partly funded by the State of Lower Saxony (Ministry of Science and Culture; Cluster of Excellence "Functional Biodiversity Research"). This is publication 4856 Netherlands Institute of Ecology (NIOO-KNAW). NR 57 TC 6 Z9 6 U1 1 U2 22 PU ELSEVIER GMBH, URBAN & FISCHER VERLAG PI JENA PA OFFICE JENA, P O BOX 100537, 07705 JENA, GERMANY SN 1439-1791 J9 BASIC APPL ECOL JI Basic Appl. Ecol. PY 2010 VL 11 IS 7 BP 563 EP 571 DI 10.1016/j.baae.2010.08.001 PG 9 WC Ecology SC Environmental Sciences & Ecology GA 714GK UT WOS:000286795300002 ER PT B AU Mettke-Hofmann, C AF Mettke-Hofmann, Claudia BE Zhang, W Liu, H TI LEARNING AND COGNITION IN RESIDENT AND MIGRANT BIRDS SO BEHAVIORAL AND CHEMICAL ECOLOGY SE Environmental Research Advances LA English DT Article; Book Chapter ID REALIZED HERITABILITY; EXPLORATORY-BEHAVIOR; AVIAN PERSONALITIES; POPULATION DECLINES; HIPPOCAMPAL VOLUME; MIGRATORY STOPOVER; FORAGING BEHAVIOR; SUMMER TANAGERS; PARUS-MAJOR; GREAT TITS AB Nearly all bird species experience some kind of environmental variability predictable or unpredictable and have evolved a variety of mechanisms to cope with it. In pronounced seasonal environments, these are on the one hand, migratory behaviour to avoid periods of food scarcity and on the other hand, residency by relying on or switching to resources that are still available. Migrants have evolved an entire suit of adaptations for their migratory way of life such as morphological (e.g., pointed wings), physiological (e.g., premigratory fattening), hormonal (e.g., lower melatonin production), and behavioural ones (e.g., migratory restlessness). However, little attention has been paid to adaptations in cognitive abilities. Migrants and residents differ strongly in the way they use environments. Migrants encounter a variety of unfamiliar habitats while on migration where they spent only short periods of time. Nonetheless, they have to get familiar with these sites to find food, shelter, and avoid predation. Residents, in contrast, live in the same area throughout the year but must cope with seasonal changes, e.g., in food abundance and distribution. Because of these differences, it is expected that migrants and residents have evolved specific learning and memory abilities that help them to optimize knowledge about their environment. I will first review the evidence for such adaptations in the context when changes in the familiar environment of an individual occur which may be particularly important for a resident to keep updated about newly emerging resources. Then I will focus on cognitive adaptations when individuals are confronted with a novel environment, which is an important aspect for migrants. The chapter will close with a discussion about the consequences of different cognitive abilities on population development in the face of increasingly faster changing environments. C1 [Mettke-Hofmann, Claudia] Liverpool John Moores Univ, Sch Nat Sci & Psychol, Liverpool L3 3AF, Merseyside, England. [Mettke-Hofmann, Claudia] Smithsonian Inst, Natl Zool Pk, Smithsonian Migratory Bird Ctr, Washington, DC 20008 USA. RP Mettke-Hofmann, C (reprint author), Liverpool John Moores Univ, Sch Nat Sci & Psychol, James Parsons Bldg,Byrom St, Liverpool L3 3AF, Merseyside, England. EM C.C.Mettke-Hofmann@ljmu.ac.uk NR 69 TC 1 Z9 1 U1 1 U2 5 PU NOVA SCIENCE PUBLISHERS, INC PI HAUPPAUGE PA 400 OSER AVE, STE 1600, HAUPPAUGE, NY 11788-3635 USA BN 978-1-60741-099-7 J9 ENVIRON RES ADV PY 2010 BP 155 EP 172 PG 18 WC Chemistry, Applied; Ecology; Environmental Sciences SC Chemistry; Environmental Sciences & Ecology GA BPE69 UT WOS:000278709400006 ER PT J AU Harris, TR Chapman, CA Monfort, SL AF Harris, Tara R. Chapman, Colin A. Monfort, Steven L. TI Small folivorous primate groups exhibit behavioral and physiological effects of food scarcity SO BEHAVIORAL ECOLOGY LA English DT Article DE black and white colobus monkeys; feeding competition; folivores; food availability; group size; primates ID KIBALE-NATIONAL-PARK; URINARY C-PEPTIDE; GORILLA-BERINGEI-BERINGEI; WHITE COLOBUS MONKEYS; CROWNED HAWK-EAGLES; GROUP-SIZE; RED COLOBUS; SCRAMBLE COMPETITION; SOCIAL-ORGANIZATION; ECOLOGICAL CONSTRAINTS AB The influence of diet and food distribution on the socioecology of group-living species has long been debated, particularly for primates. It has typically been assumed that folivorous primates experience relatively little feeding competition due to the abundant, widespread nature of their food, freeing them to form large groups in response to predation, to disperse with relative ease, and to have egalitarian female social relationships. Recent studies, however, have come to different conclusions about the extent to which folivorous primates are limited by food and experience food competition and how these factors affect folivore socioecology. To better understand the selective pressures that diet places on folivores, we investigated how 2 small highly folivorous groups of colobus monkeys (Colobus guereza) in Kibale National Park, Uganda, responded behaviorally and physiologically to a steep reduction in availability of their most important foods. The monkeys decreased their reliance on their 2 most frequently eaten food species and increased their daily path length, number of feeding patches visited/day, size of individual feeding areas, percentage of time spent feeding, and dietary diversity. They also showed evidence of physiological costs, in that lactating females' urinary C-peptide levels (i.e., insulin production) declined as top foods became scarce, and parasite loads slightly, but significantly, increased in 2 of 3 adult females examined. These results suggest that highly folivorous primates, even in very small groups, may experience behavioral and physiological effects of food limitation, within-group scramble competition for food, and possibly substantial selective pressures during periods of food scarcity. C1 [Harris, Tara R.] Max Planck Inst Evolutionary Anthropol, Dept Primatol, D-04103 Leipzig, Germany. [Harris, Tara R.; Monfort, Steven L.] Smithsonian Natl Zoo, Conservat & Res Ctr, Front Royal, VA 22630 USA. [Chapman, Colin A.] McGill Univ, Dept Anthropol, Montreal, PQ H3A 2T7, Canada. [Chapman, Colin A.] McGill Univ, McGill Sch Environm, Montreal, PQ H3A 2T7, Canada. [Chapman, Colin A.] Wildlife Conservat Soc, Bronx, NY 10460 USA. RP Harris, TR (reprint author), Minnesota Zoo, Conservat Dept, 13000 Zoo Blvd, Apple Valley, MN 55124 USA. EM taraharris1@juno.com FU Max Planck Institute for Evolutionary Anthropology; Alexander von Humboldt Foundation; Smithsonian Institution; Natural Sciences and Engineering Research Council; Canada Research Chair Program FX Max Planck Institute for Evolutionary Anthropology; Alexander von Humboldt Foundation; Smithsonian Institution's Conservation and Research Center; Natural Sciences and Engineering Research Council and Canada Research Chair Program. NR 73 TC 33 Z9 33 U1 3 U2 51 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1045-2249 J9 BEHAV ECOL JI Behav. Ecol. PD JAN-FEB PY 2010 VL 21 IS 1 BP 46 EP 56 DI 10.1093/beheco/arp150 PG 11 WC Behavioral Sciences; Biology; Ecology; Zoology SC Behavioral Sciences; Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Zoology GA 534VH UT WOS:000272925000008 ER PT J AU Goutte, S Kime, NM Argo, TF Ryan, MJ AF Goutte, S. Kime, N. M. Argo, T. F. Ryan, M. J. TI Calling strategies of male tungara frogs in response to dynamic playback SO BEHAVIOUR LA English DT Article DE tungara frog; animal communication; evoked vocal response; dynamic playback; interactive playback; acoustic behaviour; frog calls ID PHYSALAEMUS-PUSTULOSUS; NEOTROPICAL FROG; GREAT TITS; FEMALE; COMMUNICATION; CHORUS; ADVERTISEMENT AB Tungara frogs produce calls of varying complexity that consist of a whine followed by 0-7 chucks. In previous studies using static playbacks, males increase chuck number in response to calls with 1 versus 0 chucks but not in response to 2 or 3 versus 1 chuck. Here we use dynamic playback in which an automated interaction program counts the number of chucks present in a call and responds according to a specified calling strategy which determines the number of chucks in the response call. Males added progressively more chucks in response to the models' strategies of de-escalate, match or escalate; there was a significant difference in the focal males' responses to the de-escalate versus the escalate strategies. Similarly, males changed their calling strategy in response to the de-escalate strategy of the model. There was no evidence of change in calling patterns, as estimated by entropy, among treatments and between experimental and field data. Males produced significantly more chucks in these experiments than in the field, but in both contexts the mean chuck number is low and never approaches the maximum observed in nature. These data suggest that males are cost-sensitive when it comes to adding chucks and that they are more influenced by vocal competitors that de-escalate rather than escalate number of chucks. These are patterns of calling not previously revealed in studies using static playbacks, and this study is another demonstration of the usefulness of dynamic playback in studies of animal communication. C1 [Ryan, M. J.] Univ Texas Austin, Sect Integrat Biol, Austin, TX 78712 USA. [Ryan, M. J.] Smithsonian Trop Res Inst, Balboa, Panama. [Goutte, S.] Ecole Normale Super, F-75231 Paris, France. [Kime, N. M.] Edgewood Coll, Dept Nat Sci, Madison, WI USA. [Argo, T. F.] Univ Texas Austin, Dept Mech Engn, Austin, TX 78712 USA. [Argo, T. F.] Univ Texas Austin, Appl Res Labs, Austin, TX 78712 USA. RP Ryan, MJ (reprint author), Univ Texas Austin, Sect Integrat Biol, 1 Univ Stn C09300, Austin, TX 78712 USA. EM mryan@mail.utexas.edu RI goutte, sandra/M-2633-2014 FU National Science Foundation [IBN 9816564]; Ecole Normale Superieure de Paris FX This research was funded by a National Science Foundation grant to MJR (NSF IBN 9816564). SG was funded by Ecole Normale Superieure de Paris. We are especially grateful to the Smithsonian Tropical Research Institute for their continued logistical support of this research program. We thank Karin Akre, Ximena Bernal and Rachel Page for comments on the manuscript and permission to cite unpublished studies, and Jon Sakata for discussions and for suggesting the entropy analysis. NR 30 TC 11 Z9 11 U1 0 U2 7 PU BRILL ACADEMIC PUBLISHERS PI LEIDEN PA PLANTIJNSTRAAT 2, P O BOX 9000, 2300 PA LEIDEN, NETHERLANDS SN 0005-7959 J9 BEHAVIOUR JI Behaviour PY 2010 VL 147 IS 1 BP 65 EP 83 DI 10.1163/000579509X12483520922205 PG 19 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA 562TX UT WOS:000275078900005 ER PT B AU Parenti, LR Ebach, MC AF Parenti, Lynne R. Ebach, Malte C. BE Williams, DM Knapp, S TI WALLACEA DECONSTRUCTED SO BEYOND CLADISTICS: THE BRANCHING OF A PARADIGM SE Species and Systematics LA English DT Article; Book Chapter ID AREA NOMENCLATURE ICAN; HISTORICAL BIOGEOGRAPHY; INTERNATIONAL CODE; WEST PACIFIC; NEW-GUINEA; HYPOTHESES; EVOLUTION; ASIA; LINE C1 [Parenti, Lynne R.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. [Ebach, Malte C.] Univ New S Wales, Sydney, NSW 2052, Australia. RP Parenti, LR (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. EM parentil@si.edu; mcebach@gmail.com OI Ebach, Malte/0000-0002-9594-9010 NR 49 TC 5 Z9 5 U1 0 U2 2 PU UNIV CALIFORNIA PRESS PI OAKLAND PA 155 GRAND AVE, SUITE 400, OAKLAND, CA 94612-3758 USA BN 978-0-520-94799-3; 978-0-520-26772-5 J9 SPEC SYST PY 2010 VL 3 BP 303 EP 318 PG 16 WC Biodiversity Conservation SC Biodiversity & Conservation GA BXF16 UT WOS:000295933100017 ER PT B AU Gazeas, K Liakos, A Niarchos, P AF Gazeas, K. Liakos, A. Niarchos, P. BE Prsa, A Zejda, M TI DD Mon and XY UMa: CCD Photometry and Modeling of Two Close Binary Systems with Solar-Type Components SO BINARIES - KEY TO COMPREHENSION OF THE UNIVERSE SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT International Conference on Binaries - Key to the Comprehension of the Universe CY JUN 08-12, 2009 CL Masaryk Univ, Dept Theoret Phys & Astrophys, Brno, CZECH REPUBLIC HO Masaryk Univ, Dept Theoret Phys & Astrophys ID RADIAL-VELOCITY; CURVES; LIGHT AB We present our ground-based CCD observations of the close binary systems DD Mon and XY UMa in B, V, R and I bands. The light curves are analyzed using the Wilson-Devinney code (W-D) for the derivation of the geometric and photometric elements of the systems. We compare the methods of photometric and spectroscopic mass ratio determination in these binaries, as a function of all typical difficulties, which arise during the analysis of such systems (light curve asymmetries, third light etc). Finally, a new spot model is suggested for the eclipsing system XY UMa, which belongs to the RS CVn type of active binaries. C1 [Gazeas, K.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Gazeas, K.; Liakos, A.; Niarchos, P.] Univ Athens, Natl & Kapodistrian Univ Athens, Dept Astrophys, GR-15784 Athens, Greece. RP Gazeas, K (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Liakos, Alexios/K-4452-2013 OI Liakos, Alexios/0000-0002-0490-1469 NR 8 TC 2 Z9 2 U1 0 U2 1 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-750-6 J9 ASTR SOC P PY 2010 VL 435 BP 351 EP + PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BUO04 UT WOS:000289880000087 ER PT B AU Galan, C Mikolajewski, M Tomov, T Swierczynski, E Wiecek, M Brozek, T Maciejewski, G Wychudzki, P Hajduk, M Rozanski, PT Ragan, E Budzisz, B Dobierski, P Frackowiak, S Kurpinska-Winiarska, M Winiarski, M Zola, S Ogloza, W Kuzmicz, A Drozdz, M Kuligowska, E Krzesinski, J Szymanski, T Siwak, M Kundera, T Staels, B Hopkins, J Pye, J Elder, L Myers, G Dimitrov, D Popov, V Semkov, E Peneva, S Kolev, D Iliev, I Barzova, I Stateva, I Tomov, N Dvorak, S Miller, I Brat, L Niarchos, P Liakos, A Gazeas, K Pigulski, A Kopacki, G Narwid, A Majewska, A Steslicki, M Niemczura, E Ogmen, Y Oksanen, A Kucakova, H Lister, TA Heras, TA Dapergolas, A Bellas-Velidis, I Kocian, R Majcher, A AF Galan, C. Mikolajewski, M. Tomov, T. Swierczynski, E. Wiecek, M. Brozek, T. Maciejewski, G. Wychudzki, P. Hajduk, M. Rozanski, P. T. Ragan, E. Budzisz, B. Dobierski, P. Frackowiak, S. Kurpinska-Winiarska, M. Winiarski, M. Zola, S. Ogloza, W. Kuzmicz, A. Drozdz, M. Kuligowska, E. Krzesinski, J. Szymanski, T. Siwak, M. Kundera, T. Staels, B. Hopkins, J. Pye, J. Elder, L. Myers, G. Dimitrov, D. Popov, V. Semkov, E. Peneva, S. Kolev, D. Iliev, I. Barzova, I. Stateva, I. Tomov, N. Dvorak, S. Miller, I. Brat, L. Niarchos, P. Liakos, A. Gazeas, K. Pigulski, A. Kopacki, G. Narwid, A. Majewska, A. Steslicki, M. Niemczura, E. Ogmen, Y. Oksanen, A. Kucakova, H. Lister, T. A. Heras, T. A. Dapergolas, A. Bellas-Velidis, I. Kocian, R. Majcher, A. BE Prsa, A Zejda, M TI Multi-Ring Structure of the Eclipsing Disk in EE Cep - Possible Planets? SO BINARIES - KEY TO COMPREHENSION OF THE UNIVERSE SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT International Conference on Binaries - Key to the Comprehension of the Universe CY JUN 08-12, 2009 CL Masaryk Univ, Dept Theoret Phys & Astrophys, Brno, CZECH REPUBLIC HO Masaryk Univ, Dept Theoret Phys & Astrophys AB The photometric and spectroscopic observational campaign organized for the 2008/9 eclipse of EE Cep revealed features, which indicate that the eclipsing disk in the EE Cep system has a multi-ring structure. We suggest that the gaps in the disk can be related to the possible planet formation. C1 [Galan, C.; Mikolajewski, M.; Tomov, T.; Swierczynski, E.; Wiecek, M.; Brozek, T.; Maciejewski, G.; Wychudzki, P.; Hajduk, M.; Rozanski, P. T.; Ragan, E.; Budzisz, B.; Dobierski, P.; Frackowiak, S.] Nicolaus Copernicus Univ, Ul Gagarina 11, PL-87100 Torun, Poland. [Winiarski, M.; Zola, S.; Kuzmicz, A.; Kuligowska, E.; Szymanski, T.; Kundera, T.] Jagiellonian Univ, Astron Observ, PL-30244 Krakow, Poland. [Winiarski, M.; Zola, S.; Ogloza, W.; Krzesinski, J.] Pedagog Univ, Mt Suhora Obs, PL-30084 Krakow, Poland. [Siwak, M.] Univ Toronto, DAA, Toronto M5S 3H4, ON, Canada. [Staels, B.] Sonoita Res Observ AAVSO, Sonoita, AZ 85637 USA. [Hopkins, J.] Hopkins Phoenix Obs, Phoenix, AZ 85033 USA. [Pye, J.; Elder, L.] Maui Commun Coll, Kahului, HI 96732 USA. [Myers, G.] GRAS Observ, Mayhill, Mexico. [Dimitrov, D.; Popov, V.; Semkov, E.; Peneva, S.] Bulgarian Acad Sci, Astron Inst, BG-1784 Sofia, Bulgaria. [Kolev, D.; Iliev, I.; Barzova, I.; Tomov, N.] Bulgarian Acad Sci, NAO Rozhen, Astron Inst, BG-4700 Smoljan, Bulgaria. [Dvorak, S.] Rolling Hills Observ Clermont, Clermont, FL 34711 USA. [Miller, I.] Furzehill House, Swansea SA2 7LE, England. [Miller, I.] Variable Star Sec British Astron Assoc, Burlington, MA 01803 USA. [Brat, L.] Variable Star & Explanet Sec Czech Astron Soc, Valasske Meziric, Czech Republic. [Brat, L.] Altan Observ, Snezkou, Czech Republic. [Niarchos, P.; Liakos, A.] Natl & Kapodistrain Univ Athens, Astron & Mech, Dept Astrophys, GR-15784 Athens, Greece. [Gazeas, K.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Pigulski, A.; Kopacki, G.; Narwid, A.; Majewska, A.; Steslicki, M.; Niemczura, E.] Univ Wroclaw, Astron Inst, PL-51622 Wroclaw, Poland. [Ogmen, Y.] Green Island Observ B34, Gecitkale, Turkey. [Oksanen, A.] Hankasalmi Observ, FI-40270 Palokka, Finland. [Kocian, R.] Tech Univ Ostrava, Observ & Planetarium Johann Palisa VSB, C-70833 Ostrava, Czech Republic. [Lister, T. A.] Las Cumbres Observ, Goleta, CA 93117 USA. [Heras, T. A.] Observ Astron Las Pegueras NAVAS DE ORO, Navas de Oro, Spain. [Dapergolas, A.; Bellas-Velidis, I.] Inst Astron & Astrophys, Athens GR-11810, Greece. [Majcher, A.] Soltan Inst Nucl Studies, Warsaw, Poland. RP Galan, C (reprint author), Nicolaus Copernicus Univ, Ul Gagarina 11, PL-87100 Torun, Poland. EM cgalan@astri.uni.torun.p; mamiko@astri.uni.torun.pl; tomtom@astri.uni.torun.pl; Ernest.Swierczynski@astri.uni.torun.pl; wiecek@astri.uni.torun.pl; Tomasz.Brozek@astri.uni.torun.pl; zola@astro1.as.up.krakow.pl; sfogloza@cyf-kr.edu.pl; sfdrozdz@cyf-kr.edu.pl; tomasz.szymanski@oa.uj.edu.pl; siwak@astro.utoronto.ca; liliev@libra.astro.bas.bg; alliakos@phys.uoa.gr; hana.kucakova@centrum.cz RI Liakos, Alexios/K-4452-2013; Hajduk, Marcin/C-9693-2014; Maciejewski, Gracjan/D-6241-2014; Galan, Cezary/N-5556-2015; Dimitrov, Dinko/J-7682-2013 OI Liakos, Alexios/0000-0002-0490-1469; NR 5 TC 5 Z9 5 U1 0 U2 1 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-750-6 J9 ASTR SOC P PY 2010 VL 435 BP 423 EP + PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BUO04 UT WOS:000289880000107 ER PT J AU Woodman, N Stephens, RB AF Woodman, Neal Stephens, Ryan B. TI At the foot of the shrew: manus morphology distinguishes closely-related Cryptotis goodwini and Cryptotis griseoventris (Mammalia: Soricidae) in Central America SO BIOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE anatomy; digit; Insectivora; manus; ray; skeleton; small-eared shrew; Soricinae; Soricomorpha AB Small-eared shrews (Mammalia, Soricidae) of the New World genus Cryptotis are distributed from eastern North America to the northern Andes of South America. One well-defined clade in this genus is the Central American Cryptotis mexicana group, whose members are set off from other species in the genus by their variably broader fore feet and more elongate and broadened fore claws. Two species in the C. mexicana group, Cryptotis goodwini Jackson and Cryptotis griseoventris Jackson, inhabit highlands in Guatemala and southern Mexico and are presumed to be sister species whose primary distinguishing feature is the larger body size of C. goodwini. To better characterize these species and confirm the identification of recently-collected specimens, we obtained digital X-ray images of the manus from large series of dried skins of both species. Measurements of the metacarpals and phalanges successfully separated most specimens of C. goodwini and C. griseoventris. These measurements also show that the fore feet of C. griseoventris from Chiapas, Mexico, are morphologically distinct from those of members of the species inhabiting Guatemala. Univariate, bivariate, and multivariate analyses indicate that fore foot characters are more conservative within species of the C. mexicana group than are cranio-mandibular characters. Patterns of evolution of fore foot characters that superficially appear to be linear gradations are actually more complex, illustrating individual evolutionary trajectories. No claim to original US government works. Journal compilation (C) 2010 The Linnean Society of London, Biological Journal of the Linnean Society, 2010, 99, 118-134. C1 [Woodman, Neal] Smithsonian Inst, Natl Museum Nat Hist, USGS Patuxent Wildlife Res Ctr, Washington, DC 20013 USA. [Stephens, Ryan B.] Univ Wisconsin, Dept Biol, Stevens Point, WI USA. RP Woodman, N (reprint author), Smithsonian Inst, Natl Museum Nat Hist, USGS Patuxent Wildlife Res Ctr, Washington, DC 20013 USA. EM woodmann@si.edu FU Bill and Jean Lane Internship Endowment of the Research Training; National Museum of Natural History, Washington FX We thank Walter Bulmer, Ralph Eckerlin, Jack Matson, and Nicte Ordonez for providing new specimens of Cryptotis from Guatemala. Franklin Herrera assisted with permits for field work in Guatemala. R. Terry Chesser, Sandy Feinstein, Robert D. Fisher, and two anonymous reviewers provided valuable input on previous versions of this manuscript. Ryan Stephens was supported by the Bill and Jean Lane Internship Endowment of the Research Training Program, National Museum of Natural History, Washington. Any use of trade, product, or firm names is for descriptive purposes only and does not imply endorsement by the US government. NR 14 TC 12 Z9 12 U1 0 U2 0 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0024-4066 J9 BIOL J LINN SOC JI Biol. J. Linnean Soc. PD JAN PY 2010 VL 99 IS 1 BP 118 EP 134 PG 17 WC Evolutionary Biology SC Evolutionary Biology GA 534JK UT WOS:000272892200010 ER PT J AU Comizzoli, P Pukazhenthi, BS Wildt, DE AF Comizzoli, Pierre Pukazhenthi, Budhan S. Wildt, David E. TI Benefits of Germinal Vesicle Transfer by Intracytoplasmic Injection Versus Membrane Fusion on Homoplasmy and Maturational Success of Reconstructed Cat Oocytes SO BIOLOGY OF REPRODUCTION LA English DT Meeting Abstract CT 43rd Annual Meeting of the Society-for-the-Study-of-Reproduction CY JUL 31-AUG 03, 2010 CL Milwaukee, WI SP Soc Study Reproduct C1 [Comizzoli, Pierre; Pukazhenthi, Budhan S.; Wildt, David E.] Smithsonian Conservat Biol Inst, Front Royal, VA USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU SOC STUDY REPRODUCTION PI MADISON PA 1603 MONROE ST, MADISON, WI 53711-2021 USA SN 0006-3363 J9 BIOL REPROD JI Biol. Reprod. PY 2010 SU S MA 6 BP 52 EP 52 PG 1 WC Reproductive Biology SC Reproductive Biology GA 682DY UT WOS:000284381300005 ER PT J AU Nagashima, J Wildt, DE Songsasen, N AF Nagashima, Jennifer Wildt, David E. Songsasen, Nucharin TI Follicle Size and Gonadotropin Concentrations Influence In Vitro Growth of Preantral Dog Follicles SO BIOLOGY OF REPRODUCTION LA English DT Meeting Abstract CT 43rd Annual Meeting of the Society-for-the-Study-of-Reproduction CY JUL 31-AUG 03, 2010 CL Milwaukee, WI SP Soc Study Reproduct C1 [Nagashima, Jennifer; Wildt, David E.; Songsasen, Nucharin] Smithsonian Conservat Biol Inst, Ctr Species Survival, Front Royal, VA USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SOC STUDY REPRODUCTION PI MADISON PA 1603 MONROE ST, MADISON, WI 53711-2021 USA SN 0006-3363 J9 BIOL REPROD JI Biol. Reprod. PY 2010 SU S MA 27 BP 57 EP 57 PG 1 WC Reproductive Biology SC Reproductive Biology GA 682DY UT WOS:000284381300025 ER PT J AU Hobbs, RJ Howard, J Fleischer, RC Wildt, DE Comizzoli, P AF Hobbs, Rebecca J. Howard, JoGayle Fleischer, Robert C. Wildt, David E. Comizzoli, Pierre TI Seasonal Changes in FSH-Induced FSHR mRNA Splice Variant Expression During In Vitro Maturation of Cat Oocytes SO BIOLOGY OF REPRODUCTION LA English DT Meeting Abstract CT 43rd Annual Meeting of the Society-for-the-Study-of-Reproduction CY JUL 31-AUG 03, 2010 CL Milwaukee, WI SP Soc Study Reproduct C1 Smithsonian Conservat Biol Inst, Washington, DC USA. Smithsonian Conservat Biol Inst, Front Royal, VA USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SOC STUDY REPRODUCTION PI MADISON PA 1603 MONROE ST, MADISON, WI 53711-2021 USA SN 0006-3363 J9 BIOL REPROD JI Biol. Reprod. PY 2010 SU S MA 382 BP 133 EP 134 PG 2 WC Reproductive Biology SC Reproductive Biology GA 682DY UT WOS:000284381300356 ER PT J AU Terrell, KA Wildt, DE Anthony, NM Bavister, BD Leibo, SP Penfold, LM Marker, LL Crosier, AE AF Terrell, Kimberly A. Wildt, David E. Anthony, Nicola M. Bavister, Barry D. Leibo, Stanley P. Penfold, Linda M. Marker, Laurie L. Crosier, Adrienne E. TI Oxidative Metabolism Is Required for Sperm Motility and Viability in Felids, but May be Impaired in Cheetah (Acinonyx jubatus) Ejaculates. SO BIOLOGY OF REPRODUCTION LA English DT Meeting Abstract CT 43rd Annual Meeting of the Society-for-the-Study-of-Reproduction CY JUL 31-AUG 03, 2010 CL Milwaukee, WI SP Soc Study Reproduct C1 Smithsonian Conservat Biol Inst, Front Royal, VA USA. Univ New Orleans, New Orleans, LA 70148 USA. Univ Puerto Rico, San Juan, PR 00936 USA. White Oak Conservat Ctr, Yulee, FL USA. Cheetah Conservat Fund, Otjiwarongo, Namibia. NR 0 TC 0 Z9 0 U1 0 U2 3 PU SOC STUDY REPRODUCTION PI MADISON PA 1603 MONROE ST, MADISON, WI 53711-2021 USA SN 0006-3363 J9 BIOL REPROD JI Biol. Reprod. PY 2010 SU S MA 489 BP 156 EP 156 PG 1 WC Reproductive Biology SC Reproductive Biology GA 682DY UT WOS:000284381300454 ER PT J AU Pukazhenthi, BS Lapiana, F Padilla, L Santiestevan, J da Silva, MC Alvarenga, M Wildt, D AF Pukazhenthi, Budhan S. Lapiana, Francesca Padilla, Luis Santiestevan, Jenny da Silva, Marco Coutinho Alvarenga, Marco Wildt, David TI Improved Sperm Cryopreservation in the Critically Endangered Przewalski's Horse (Equus ferus przewalskii) Using Different Cryoprotectants SO BIOLOGY OF REPRODUCTION LA English DT Meeting Abstract CT 43rd Annual Meeting of the Society-for-the-Study-of-Reproduction CY JUL 31-AUG 03, 2010 CL Milwaukee, WI SP Soc Study Reproduct C1 Smithsonian Conservat Biol Inst, Front Royal, VA USA. Smithsonian Conservat Biol Inst, Washington, DC USA. Ohio State Univ, Columbus, OH 43210 USA. Sao Paulo State Univ, Sao Paulo, Brazil. NR 0 TC 0 Z9 0 U1 1 U2 7 PU SOC STUDY REPRODUCTION PI MADISON PA 1603 MONROE ST, MADISON, WI 53711-2021 USA SN 0006-3363 J9 BIOL REPROD JI Biol. Reprod. PY 2010 SU S MA 675 BP 193 EP 193 PG 1 WC Reproductive Biology SC Reproductive Biology GA 682DY UT WOS:000284381300612 ER PT J AU Pereira, AIA Curvelo, CRD Smith, DR Pereira, JMM Zanuncio, TV Zanuncio, JC AF Azevedo Pereira, Alexandre Igor da Silva Curvelo, Carmen Rosa Smith, David R. Milagres Pereira, Jose Milton Zanuncio, Teresinha Vinha Zanuncio, Jose Cola TI NATURAL MORTALITY FACTORS OF THE NEOTROPICAL Symphyta Haplostegus nigricrus (Hymenoptera: Pergidae) SO BIOSCIENCE JOURNAL LA Portuguese DT Article DE Guava; Sawfly; Herbivory; Pentatomidae; Biological Control ID BIOLOGICAL-CONTROL; TENTHREDINIDAE; SAWFLIES; TEMPERATURE; POPULATIONS; DEFOLIATION; PHYLOGENY; PREDATOR; GROWTH AB The main natural mortality factors of Haplostegus nigricrus Conde (Hymenoptera: Symphyta: Pergidae) present in a secondary forested area in the municipality of Vicosa, Minas Gerais, Brazil, are described. Adults were sampled monthly for one year by sweeping vegetation, and their numbers correlated with temperature and rainfall. Natural enemies were recorded from larvae and adults under both laboratory and field conditions and include predators, parasitoids, viruses, and fungi. Natural enemies were not observed in the egg and adult phases and the pupae viability was even less under laboratory conditions. Haplostegus nigricrus is bivotine, and its life cycle strongly coincides with both. The low occurrence of natural enemies, the high egg viability, and the strong correlation to regional abiotic factors suggest that this species has high adaptability to habitats composed of native Myrtaceae of economic importance in Brazil. C1 [Azevedo Pereira, Alexandre Igor; Milagres Pereira, Jose Milton; Zanuncio, Teresinha Vinha; Zanuncio, Jose Cola] Univ Fed Vicosa, Dept Biol Anim, Vicosa, MG, Brazil. [da Silva Curvelo, Carmen Rosa] Univ Fed Vicosa, Dept Fitotecnia, Vicosa, MG, Brazil. [Smith, David R.] ARS, Systemat Entomol Lab, PSI, Natl Museum Nat Hist,Smithsonian Inst, Washington, DC USA. RP Pereira, AIA (reprint author), Univ Fed Vicosa, Dept Biol Anim, Vicosa, MG, Brazil. EM aiapereira@yahoo.com.br NR 25 TC 1 Z9 2 U1 0 U2 0 PU UNIV FEDERAL UBERLANDIA PI UBERLANDIA PA AV PARA, 1720 CAMPUS UMUARAMA, UBERLANDIA, 38400-902, BRAZIL SN 1516-3725 J9 BIOSCI J JI Biosci. J. PD JAN-FEB PY 2010 VL 26 IS 1 BP 115 EP 120 PG 6 WC Agriculture, Multidisciplinary; Agronomy; Biology SC Agriculture; Life Sciences & Biomedicine - Other Topics GA 573VP UT WOS:000275943700015 ER PT J AU Koh, LP Ghazoul, J Butler, RA Laurance, WF Sodhi, NS Mateo-Vega, J Bradshaw, CJA AF Koh, Lian Pin Ghazoul, Jaboury Butler, Rhett A. Laurance, William F. Sodhi, Navjot S. Mateo-Vega, Javier Bradshaw, Corey J. A. TI Wash and Spin Cycle Threats to Tropical Biodiversity SO BIOTROPICA LA English DT Article ID WHALING ISSUE; CONSERVATION; OIL; DEFORESTATION; FORESTS; LANDS C1 [Koh, Lian Pin; Ghazoul, Jaboury] ETH, Inst Terr Ecosyst, CH-8092 Zurich, Switzerland. [Butler, Rhett A.] Mongabay Com, Menlo Pk, CA 94026 USA. [Laurance, William F.; Mateo-Vega, Javier] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Laurance, William F.] James Cook Univ, Sch Marine & Trop Biol, Cairns, Qld 4870, Australia. [Sodhi, Navjot S.] Natl Univ Singapore, Dept Biol Sci, Singapore 117543, Singapore. [Sodhi, Navjot S.] Harvard Univ, Dept Organism & Evolutionary Biol, Cambridge, MA 02138 USA. [Mateo-Vega, Javier] Yale Univ, Sch Forestry & Environm Studies, Environm Leadership & Training Initiat, New Haven, CT 06511 USA. [Bradshaw, Corey J. A.] Univ Adelaide, Inst Environm, Adelaide, SA 5005, Australia. [Bradshaw, Corey J. A.] Univ Adelaide, Sch Earth & Environm Sci, Adelaide, SA 5005, Australia. [Bradshaw, Corey J. A.] S Australian Res & Dev Inst, Henley Beach, SA 5022, Australia. RP Koh, LP (reprint author), ETH, Inst Terr Ecosyst, CHN G 74-2,Univ Str 16, CH-8092 Zurich, Switzerland. EM lian.koh@env.ethz.ch RI Koh, Lian Pin/A-5794-2010; Laurance, William/B-2709-2012; Bradshaw, Corey/A-1311-2008 OI Koh, Lian Pin/0000-0001-8152-3871; Bradshaw, Corey/0000-0002-5328-7741 FU ETH Fellowship; Swiss National Science Foundation FX The idea for this commentary was originally inspired by a tendentious response to an article posted on C. J. A. B.'s blog site (http://conservationbytes.com/2008/11/10/unexpected-benefits-of-falling- palm-oil-prices/); authors contributed to developing and writing the paper, and in debating the final text. We thank D. Wilcove for helpful discussions and R. Clements for permission to use his photograph. We also thank J. D. Neidel for transcribing the taped proceedings of the recent biofuels conference in Singapore. L. P. K. is supported by an ETH Fellowship and the Swiss National Science Foundation. NR 44 TC 17 Z9 17 U1 1 U2 6 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0006-3606 J9 BIOTROPICA JI Biotropica PD JAN PY 2010 VL 42 IS 1 BP 67 EP 71 DI 10.1111/j.1744-7429.2009.00588.x PG 5 WC Ecology SC Environmental Sciences & Ecology GA 539ZZ UT WOS:000273301100010 ER PT J AU Munroe, TA Krabbenhoft, TJ AF Munroe, Thomas A. Krabbenhoft, Trevor J. TI TWO UNUSUALLY LARGE PRE-TRANSITIONAL TONGUEFISH LARVAE (PLEURONECTIFORMES: CYNOGLOSSIDAE: SYMPHURUS) FROM OCEANIC WATERS NEAR THE GALAPAGOS ISLANDS SO BULLETIN OF MARINE SCIENCE LA English DT Article ID LIFE-HISTORY STAGES; SOLE MICROSTOMUS-PACIFICUS; GULF-OF-CALIFORNIA; DOVER SOLE; GLYPTOCEPHALUS-ZACHIRUS; REX SOLE; FLATFISHES; ATLANTIC; FLOUNDER; DURATION AB Two, exceptionally large (51.0 and 36.6 mm SL), pre-transitional larval tonguefishes, collected in the water column and near surface waters overlying deep oceanic waters off the Galdpagos Islands, are described and compared with larval stages and adults of eastern Pacific species of Symphurus. The larger specimen, Symphurus varius Garman, 1899, features a 1-3-3 pattern of interdigitation of proximal dorsal fin pterygiophores and neural spines (ID pattern), 12 caudal fin rays, 95 dorsal fin rays, 78 anal fin rays, 51 vertebrae, and 5 hypurals. This first known larval S. varius is also the largest known unmetamorphosed larva of the Cynoglossidae. The smaller larva is Symphurus melanurus Clark, 1936 based on its 1-5-3 ID pattern, meristic features, long protruding gut, and pigmentation. It represents the first known larva of S. melanurus and first occurrence of S. melanurus from the Galdpagos Islands region. Whether large pre-transitional larvae are typical for S. melanurus and S. varius, or merely represent individuals having undergone delayed metamorphosis, will be confirmed when additional specimens become available. Symphurus varius is known only from the Galapagos Islands and other oceanic islands in the eastern tropical Pacific, thus capture of a larval S. varius near these offshore islands is not unexpected. Large size and oceanic occurrence of the pre-transitional stage S. melanurus, an inshore species, strongly suggest an expatriated individual from coastal seas having undergone delayed metamorphosis. C1 [Munroe, Thomas A.] Smithsonian Inst, Natl Systemat Lab, NMFS NEFSC, NHB, Washington, DC 20013 USA. [Krabbenhoft, Trevor J.] Univ New Mexico, Museum SW Biol, Dept Biol, Albuquerque, NM 87131 USA. RP Munroe, TA (reprint author), Smithsonian Inst, Natl Systemat Lab, NMFS NEFSC, NHB, POB 37012,WC 57,MRC 153, Washington, DC 20013 USA. EM munroet@si.edu NR 54 TC 2 Z9 2 U1 1 U2 4 PU ROSENSTIEL SCH MAR ATMOS SCI PI MIAMI PA 4600 RICKENBACKER CAUSEWAY, MIAMI, FL 33149 USA SN 0007-4977 EI 1553-6955 J9 B MAR SCI JI Bull. Mar. Sci. PD JAN PY 2010 VL 86 IS 1 BP 15 EP 33 PG 19 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA 546IE UT WOS:000273803700002 ER PT J AU Aplin, KP Helgen, KM AF Aplin, K. P. Helgen, K. M. TI QUATERNARY MURID RODENTS OF TIMOR PART I: NEW MATERIAL OF CORYPHOMYS BUEHLERI SCHAUB, 1937, AND DESCRIPTION OF A SECOND SPECIES OF THE GENUS SO BULLETIN OF THE AMERICAN MUSEUM OF NATURAL HISTORY LA English DT Article ID COMPARATIVE FUNCTIONAL-MORPHOLOGY; BILL SIZE POLYMORPHISM; NEW-GUINEA; CHARACTER DISPLACEMENT; MUROID RODENTS; EAST-TIMOR; NUCLEAR GENES; JAW MUSCLES; EVOLUTIONARY SIGNIFICANCE; CLETHRIONOMYS-RUFOCANUS AB Large collections of fragmentary animal bones excavated from archaeological contexts in East Timor between 1968 and 2002 provide new material referable to the recently extinct, gigantic murine genus Coryphomys. We document the upper and lower dentition and palatal anatomy of C. buehleri Schaub, 1937, and identify and name a second species of Coryphomys, based on differences in molar size and morphology and skeletal robusticity. Alternative interpretations of the observed morphological and metric variability (sexual dimorphism, resource-based polymorphism, sample heterochroneity) are each carefully assessed and rejected, and we conclude that the genus comprised two species of approximately similar body size. Preserved cranial elements of both species of Coryphomys feature a high degree of anatomical specialization, including an unusual elaboration of the maxillary sinus complex. Though the specialized anatomy of Coryphomys invites consideration of its phylogenetic relationships, this exercise is hindered by a demonstrable high level of homoplasy (i.e., multiple, independent evolutionary losses and gains) in many of the key craniodental features traditionally surveyed within Murinae, while other features are insufficiently well surveyed for broad-scale analysis. Nevertheless, our comparisons highlight two potentially related lineages among the geographically proximate Murinae the Philippine Phloeomyini and the Australo-Papuan Hydromyini. The remains of Coryphomys are relatively scarce in all the archaeological samples, but distributional evidence suggests that both species of Coryphomys were found primarily in upland habitats. Late Pleistocene samples document their former presence at lower elevations, possibly reflecting-cooler climatic conditions at that time. C1 [Aplin, K. P.] CSIRO, Australian Natl Wildlife Collect, Div Sustainable Ecosyst, Canberra, ACT, Australia. [Aplin, K. P.; Helgen, K. M.] Amer Museum Nat Hist, Div Vertebrate Zool Mammal, New York, NY 10024 USA. [Helgen, K. M.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. RP Aplin, KP (reprint author), CSIRO, Australian Natl Wildlife Collect, Div Sustainable Ecosyst, Canberra, ACT, Australia. EM ken.aplin@csiro.au; HELGENK@si.edu NR 286 TC 13 Z9 13 U1 0 U2 1 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 0003-0090 EI 1937-3546 J9 B AM MUS NAT HIST JI Bull. Amer. Mus. Nat. Hist. PY 2010 IS 341 BP 1 EP 80 PG 80 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 631JP UT WOS:000280343100001 ER PT J AU Venzke, E Sennert, SK Wunderman, R AF Venzke, Edward Sennert, Sally Kuhn Wunderman, Richard TI Reports from the Smithsonian's Global Volcanism Network, July 2009 SO BULLETIN OF VOLCANOLOGY LA English DT Article AB Information included in this summary is based on more detailed reports published in the Bulletin of the Global Volcanism Network, vol. 34, no. 7, July 2009 (on the Internet at http://www.volcano.si.edu/). Edited by scientists at the Smithsonian, this bulletin includes reports provided by a worldwide network of correspondents. The reports contain the names and contact information for all sources. Please note that these reports are preliminary and subject to change as events are studied in more detail. The Global Volcanism Program welcomes further reports of current volcanism, seismic unrest, monitoring data, and field observations. C1 [Venzke, Edward; Sennert, Sally Kuhn; Wunderman, Richard] Smithsonian Inst, Natl Museum Nat Hist, Global Volcanism Program, Washington, DC 20013 USA. RP Venzke, E (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Global Volcanism Program, MRC 119,POB 37012, Washington, DC 20013 USA. EM gvp@si.edu NR 0 TC 1 Z9 1 U1 2 U2 3 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0258-8900 J9 B VOLCANOL JI Bull. Volcanol. PD JAN PY 2010 VL 72 IS 1 BP 129 EP 130 DI 10.1007/s00445-009-0326-2 PG 2 WC Geosciences, Multidisciplinary SC Geology GA 530YT UT WOS:000272629600010 ER PT J AU Morineaux, M Nishi, E Ormos, A Mouchel, O AF Morineaux, Marie Nishi, Eijiroh Ormos, Andrea Mouchel, Olivier TI A new species of Phyllochaetopterus (Annelida: Chaetopteridae) from deep-sea hydrothermal Ashadze-1 vent field, Mid-Atlantic Ridge: taxonomical description and partial COI DNA sequence SO CAHIERS DE BIOLOGIE MARINE LA English DT Article DE Polychaeta; Hydrothermal vent; Mid-Atlantic Ridge; Taxonomy; New species; COI ID POLYCHAETA; REDESCRIPTION AB Phyllochaetopterus polus, a new species of the polychaete family Chaetopteridae is described. Specimens were collected at the Ashadze-1 vent field (Mid-Atlantic Ridge), from 4100-4200 m depth. P polus is the first chaetopterid reported from the Atlantic hydrothermal vents. Three chaetopterid species have been recorded from deep-sea hydrothermal vents belonging to two genera, Spiochaetopterus and Phyllochaetopterus. P polus sp. nov. is a medium-sized chaetopterid, characterized by 9 chaetigers in region A and 2 in region B; region C is usually incomplete in the specimens examined, but has at least 40-70 chaetigers. This polychaete has one pair of modified chaetae in chaetiger 4 with a pear-shaped obliquely truncated head, triangular uncini and a branched annulated tube. The species resembles P lauensis Nishi & Rouse, 2007 in most characters but differs by the colour of the ventral shield and tube structure. Blast results of a 655 bp fragment of the mitochondrial DNA COI gene of this new species revealed Phyllochaetopterids as the closest available sequences in Genbank. A phylogenetic tree has been further built using all other COI chaetopterid polychaete sequences found in Genbank to infer phylogenetic position of the new species. It adds to the previous observations of close proximity of communities associated to whale falls and hydrothermal vents communities as the phylogenetically closest species is an undescribed Phyllochaetopterus found around whale fall in Monterey Bay (California). C1 [Morineaux, Marie; Mouchel, Olivier] IFREMER, Ctr Brest, Dept Etud Ecosyst Profonds, F-29280 Plouzane, France. [Nishi, Eijiroh] Yokohama Natl Univ, Manazuru Marine Lab, Kanagawa 2590202, Japan. [Ormos, Andrea] Smithsonian Inst, Natl Museum Nat Hist, Labs Analyt Biol, Washington, DC 20013 USA. RP Morineaux, M (reprint author), IFREMER, Ctr Brest, Dept Etud Ecosyst Profonds, BP70, F-29280 Plouzane, France. EM marie.morineaux@ifremer.fr FU Ifremer; KAKENHI [20008766]; [ANR06 BDV005] FX We thank Y. Fouquet, chief scientist on the SERPENTINE cruise for providing samples, D. Desbruyeres, P. Briand and S. Hourdez for providing samples, P. Crassous for SEM images, Sophie Arnaud for her gracious help in molecular analysis and E. Kupriyanova for her suggestions, help and translation of Russian. We are grateful to T. Laperousaz for providing P. lauensis paratype from the South Australian Museum, to A. Driskell from the Smithsonian Institution and P. Martinez-Arbizu from the CeDAmar for the barcoding workshop. We are also very grateful to the ROV "Victor" team and the POURQUOI PAS ? crew for their support at sea, to two anonymous reviewers for their comments and suggestions upgrading the manuscript. The SERPENTINE cruise has been supported by Ifremer and this research by the ANR06 BDV005 'Deep-Oases' grant and partly funded by KAKENHI 20008766. NR 25 TC 4 Z9 5 U1 0 U2 6 PU CAHIERS DE BIOLOGIE MARINE PI ROSCOFF PA STATION BIOLOGIQUE PLACE GEORGES TEISSIER, 29680 ROSCOFF, FRANCE SN 0007-9723 EI 2262-3094 J9 CAH BIOL MAR JI Cah. Biol. Mar. PY 2010 VL 51 IS 3 BP 239 EP 248 PG 10 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 646GP UT WOS:000281527100003 ER PT J AU Karlstrom, PJ AF Karlstrom, Paul J. TI THE MODERN MOVES WEST: CALIFORNIA ARTISTS AND DEMOCRATIC CULTURE IN THE TWENTIETH CENTURY SO CALIFORNIA HISTORY LA English DT Book Review C1 [Karlstrom, Paul J.] Smithsonian Inst, Archives Amer Art, Washington, DC 20560 USA. RP Karlstrom, PJ (reprint author), Smithsonian Inst, Archives Amer Art, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU CALIFORNIA HISTORICAL SOC PI SAN FRANCISCO PA 678 MISSION ST, SAN FRANCISCO, CA 94105-4014 USA SN 0162-2897 J9 CALIF HIST JI Calif. Hist. PY 2010 VL 88 IS 1 BP 58 EP 58 PG 1 WC History SC History GA V32JW UT WOS:000208948500005 ER PT S AU Frebel, A Simon, JD Kirby, E Geha, M Willman, B AF Frebel, Anna Simon, Joshua D. Kirby, Evan Geha, Marla Willman, Beth BE Cunha, K Spite, M Barbuy, B TI Extremely metal-poor stars in dwarf galaxies SO CHEMICAL ABUNDANCES IN THE UNIVERSE: CONNECTING FIRST STARS TO PLANETS SE IAU Symposium Proceedings Series LA English DT Proceedings Paper CT 265th Symposium of the International-Astronomical-Union CY AUG 10-14, 2009 CL Rio de Janeiro, BRAZIL SP Int Astron Union, Minist Ciencia & Tecnol, CNPQ, FAPESP, FAPERJ, CAPES DE stars: abundances; stars: Population II; Galaxy: formation; Galaxy: halo; galaxies: dwarf; (galaxies:) Local Group; galaxies: stellar content; (cosmology:) early universe ID SPHEROIDAL GALAXY; GALACTIC HALO; 1ST STARS; KINEMATICS; HISTORIES; MILKY AB We present Keck/HIRES spectra of six metal-poor stars in two of the ultra-faint dwarf galaxies orbiting the Milky Way, Ursa Major 11 and Coma Berenices, and a Magellan/MIKE spectrum of a star in the classical dwarf spheroidal galaxy (dSph) Sculptor. Our data include the first high-resolution spectroscopic observations of extremely metal-poor stars ([Fe/H] < -3.0) not belonging to the Milky Way (MW) stellar halo field population. We obtain abundance measurements and upper limits for up to 26 elements between carbon and europium. The stars span a range of -3.8 < [Fe/H] < -2.3, with the ultra-faints having large spreads in Fe. A comparison with MW halo stars of similar metallicity reveals substantial agreement between the abundance patterns of the ultra-faint dwarf galaxies and Sculptor and the MW halo for the light, a and iron-peak elements (C to Zn). This agreement contrasts with the results of earlier studies of more metal-rich stars (-2.5 less than or similar to [Fe/H] less than or similar to -1.0) in more luminous dwarfs, which found significant abundance discrepancies with respect to the MW halo data. The abundances of neutron-capture elements (Sr to Eu) in all three galaxies are extremely low, consistent with the most metal-poor halo stars, but not with the typical halo abundance pattern at [Fe/H] less than or similar to -3.0. Our results are broadly consistent with a. galaxy formation model which predicts that massive dwarf galaxies are the source of the metal-rich component ([Fe/H] > -2.5) of the MW inner halo, but we propose that dwarf galaxies similar to the dSphs are the primary contributors to the metal-poor end of the metallicity distribution of the MW outer halo. C1 [Frebel, Anna] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Frebel, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM afrebel@cfa.harvard.edu; jsimon@ociw.edu; enk@astro.caltech.edu; marla.geha@yale.edu; bwillman@haverford.edu NR 17 TC 0 Z9 0 U1 0 U2 0 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND SN 1743-9213 BN 978-0-521-76495-7 J9 IAU SYMP P SERIES JI IAU Symposium Proc. Series PY 2010 VL 5 IS 265 BP 237 EP 240 DI 10.1017/S1743921310000633 PG 4 WC Astronomy & Astrophysics; Chemistry, Physical SC Astronomy & Astrophysics; Chemistry GA BQB13 UT WOS:000280548900056 ER PT J AU del Rio, M AF del Rio, Mercedes TI THE TREASURES OF THE MALLKU OF POCONA AND TOTORA IN THE SIXTEENTH CENTURY SO CHUNGARA-REVISTA DE ANTROPOLOGIA CHILENA LA Spanish DT Article DE Andean ethnohistory; coca; curacas; border; Pocona and Totora; pre-Colombian and colonial iconography AB Tins article presents an etnohistorical analysis of a coca production zone on the eastern frontiers of the Tawantinsuyu during the 16(th) century. The Inkas had organized a multiethnic archipelago in the valleys of Pocona and Totora (Charcas) in order to defend the frontier and cultivate coca for the State; this continued during the early Colonial Period. The paper shows that colonial ethnic leaders in these frontier valleys hoarded prestigious symbols of authority from the time oldie Inka which reinforced their colonial position. In particular these treasures commemorated their ancestors, who had been captains of the Inkas and had organized the labor force in the cocales, as well as during seasonal agricultural ceremonies and military festivals. C1 Smithsonian Inst, Dept Anthropol, Natl Museum Nat Hist, Washington, DC 20560 USA. RP del Rio, M (reprint author), Smithsonian Inst, Dept Anthropol, Natl Museum Nat Hist, Washington, DC 20560 USA. EM mercedes3310@verizon.net NR 45 TC 3 Z9 3 U1 0 U2 0 PU UNIV TARAPACA PI ARICA PA CASILLA 6-D, ARICA, 1775, CHILE SN 0716-1182 J9 CHUNGARA JI Chungara PD JAN-JUN PY 2010 VL 42 IS 1 BP 199 EP 220 PG 22 WC Anthropology SC Anthropology GA 608ET UT WOS:000278566300030 ER PT S AU Elvis, M AF Elvis, Martin BE Peterson, BM Somerville, RS StorchiBergmann, T TI The Quasar Continuum SO CO-EVOLUTION OF CENTRAL BLACK HOLES AND GALAXIES SE IAU Symposium Proceedings Series LA English DT Proceedings Paper CT 267th Symposium of the International Astronomical Union CY AUG 10-14, 2009 CL Rio de Janeiro, BRAZIL DE accreion disks; galaxies: active; galaxies: jets; galaxies: nuclei; galaxies: quasars: general; infrared: galaxies; radio continuum: galaxies; ultraviolet: galaxies; X-ray: galaxies ID ACTIVE GALACTIC NUCLEI; X-RAY-EMISSION; SUPERMASSIVE BLACK-HOLES; RADIO-QUIET QUASARS; SPECTRAL ENERGY-DISTRIBUTIONS; ADVECTION-DOMINATED ACCRETION; HIGH-REDSHIFT QUASARS; SEYFERT-GALAXIES; HOST GALAXIES; OBSERVATIONAL CONSTRAINTS AB The powerful compact continuum emission from quasars is understood only in outline. New surveys allow investigation of the quasar continuum over a wide range of parameters (z, L, L/L-Edd) and wavelengths (radio to X-ray). I review the spectral energy distributions of quasars and how new scaling relations with physical parameters promise to take us to a deeper understanding of the quasar continuum. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Elvis, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM elvis@cfa.harvard.edu NR 86 TC 1 Z9 1 U1 0 U2 0 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND SN 1743-9213 BN 978-0-521-76502-2 J9 IAU SYMP P SERIES JI IAU Symposium Proc. Series PY 2010 VL 267 BP 55 EP 64 DI 10.1017/S1743921310005570 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BVJ71 UT WOS:000291672300008 ER PT S AU Kelly, BC Vestergaard, M Fan, XH Hernquist, L Hopkins, P Siemiginowska, A AF Kelly, Brandon C. Vestergaard, Marianne Fan, Xiaohui Hernquist, Lars Hopkins, Philip Siemiginowska, Aneta BE Peterson, BM Somerville, RS StorchiBergmann, T TI The Distribution and Evolution of Black Hole Mass in Broad Line Quasars SO CO-EVOLUTION OF CENTRAL BLACK HOLES AND GALAXIES SE IAU Symposium Proceedings Series LA English DT Proceedings Paper CT 267th Symposium of the International Astronomical Union CY AUG 10-14, 2009 CL Rio de Janeiro, BRAZIL DE galaxies: active; galaxies: mass function; quasars: general C1 [Kelly, Brandon C.; Hernquist, Lars; Siemiginowska, Aneta] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. 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 NR 1 TC 0 Z9 0 U1 1 U2 1 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND SN 1743-9213 BN 978-0-521-76502-2 J9 IAU SYMP P SERIES JI IAU Symposium Proc. Series PY 2010 VL 267 BP 263 EP 263 DI 10.1017/S174392131000640X PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BVJ71 UT WOS:000291672300091 ER EF